[ { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/548hq-52334", "eprint_id": 98371, "eprint_status": "archive", "datestamp": "2023-08-22 02:26:35", "lastmod": "2023-10-18 17:18:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kreidberg-L", "name": { "family": "Kreidberg", "given": "Laura" }, "orcid": "0000-0003-0514-1147" }, { "id": "Koll-D-D-B", "name": { "family": "Koll", "given": "Daniel D. B." } }, { "id": "Morley-C-V", "name": { "family": "Morley", "given": "Caroline" }, "orcid": "0000-0002-4404-0456" }, { "id": "Hu-Renyu", "name": { "family": "Hu", "given": "Renyu" }, "orcid": "0000-0003-2215-8485" }, { "id": "Schaefer-L", "name": { "family": "Schaefer", "given": "Laura" } }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Stevenson-K-B", "name": { "family": "Stevenson", "given": "Kevin B." }, "orcid": "0000-0002-7352-7941" }, { "id": "Dittmann-J-A", "name": { "family": "Dittmann", "given": "Jason" } }, { "id": "Vanderburg-A", "name": { "family": "Vanderburg", "given": "Andrew" }, "orcid": "0000-0001-7246-5438" }, { "id": "Berardo-D", "name": { "family": "Berardo", "given": "David" } }, { "id": "Guo-Xueying", "name": { "family": "Guo", "given": "Xueying" } }, { "id": "Stassun-K-G", "name": { "family": "Stassun", "given": "Keivan" }, "orcid": "0000-0002-3481-9052" }, { "id": "Crossfield-I-J-M", "name": { "family": "Crossfield", "given": "Ian" }, "orcid": "0000-0002-1835-1891" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Loeb-A", "name": { "family": "Loeb", "given": "Abraham" }, "orcid": "0000-0003-4330-287X" }, { "id": "Ricker-G-R", "name": { "family": "Ricker", "given": "George" } }, { "id": "Seager-S", "name": { "family": "Seager", "given": "Sara" }, "orcid": "0000-0002-6892-6948" }, { "id": "Vanderspek-R", "name": { "family": "Vanderspek", "given": "Roland" } } ] }, "title": "Absence of a thick atmosphere on the terrestrial exoplanet LHS\u00a03844b", "ispublished": "pub", "full_text_status": "public", "keywords": "Exoplanets; Stars", "note": "\u00a9 2019 Nature Publishing Group. \n\nReceived 22 March 2019; Accepted 22 July 2019; Published 19 August 2019. \n\nData availability: The raw data used in this study are available at the Spitzer Heritage Archive, https://sha.ipac.caltech.edu/applications/Spitzer/SHA. \n\nCode availability: We processed and fitted the data with the open-source pipeline POET, which is available at https://github.com/kevin218/POET. We used the code version corresponding to commit ID adbe62e7b733df9541231e8d1e5d32b7e2cdad76. \n\nL.K. is a Junior Fellow of the Harvard Society of Fellows. J.D. is a 51 Pegasi b Postdoctoral Fellow. A.V. is a NASA Sagan Fellow. D.D.B.K. was supported by a James S. McDonnell Foundation postdoctoral fellowship. R.H. is supported in part by NASA Grant number 80NM0018F0612. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. A.V.'s work was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory, funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. D.C. acknowledges support from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. \n\nAuthor Contributions: L.K. conceived the project, planned the observations and carried out the primary data reduction. D.D.B.K., C.M. and R.H. ran theoretical models for the planet's atmosphere and surface. L.S. provided atmospheric evolution models. D.D., K.B.S., J.D., A.V., D.B. and X.G. contributed to the data analysis. K.S. modelled the stellar spectrum. I.C., D.C., D.W.L., A.L., G.R., S.S. and R.V. provided useful comments on the manuscript and assisted with the observing proposal. \n\nThe authors declare no competing interests.\n\n
Accepted Version - 1908.06834.pdf
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", "abstract": "Most known terrestrial planets orbit small stars with radii less than 60 per cent of that of the Sun. Theoretical models predict that these planets are more vulnerable to atmospheric loss than their counterparts orbiting Sun-like stars. To determine whether a thick atmosphere has survived on a small planet, one approach is to search for signatures of atmospheric heat redistribution in its thermal phase curve. Previous phase curve observations of the super-Earth 55 Cancri e (1.9 Earth radii) showed that its peak brightness is offset from the substellar point (latitude and longitude of 0 degrees)\u2014possibly indicative of atmospheric circulation. Here we report a phase curve measurement for the smaller, cooler exoplanet LHS 3844b, a 1.3-Earth-radii world in an 11-hour orbit around the small nearby star LHS 3844. The observed phase variation is symmetric and has a large amplitude, implying a dayside brightness temperature of 1,040 \u00b1 40 kelvin and a nightside temperature consistent with zero kelvin (at one standard deviation). Thick atmospheres with surface pressures above 10 bar are ruled out by the data (at three standard deviations), and less-massive atmospheres are susceptible to erosion by stellar wind. The data are well fitted by a bare-rock model with a low Bond albedo (lower than 0.2 at two standard deviations). These results support theoretical predictions that hot terrestrial planets orbiting small stars may not retain substantial atmospheres.", "date": "2019-09-05", "date_type": "published", "publication": "Nature", "volume": "573", "number": "7772", "publisher": "Nature Publishing Group", "pagerange": "87-90", "id_number": "CaltechAUTHORS:20190830-105526886", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190830-105526886", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Harvard University" }, { "agency": "Heising-Simons Foundation", "grant_number": "51 Pegasi b Fellowship" }, { "agency": "NASA Sagan Fellowship" }, { "agency": "James S. McDonnell Foundation" }, { "agency": "NASA", "grant_number": "80NM0018F0612" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "John Templeton Foundation" } ] }, "doi": "10.1038/s41586-019-1497-4", "primary_object": { "basename": "41586_2019_1497_Fig9_ESM.jpg", "url": "https://authors.library.caltech.edu/records/548hq-52334/files/41586_2019_1497_Fig9_ESM.jpg" }, "related_objects": [ { "basename": "1908.06834.pdf", "url": "https://authors.library.caltech.edu/records/548hq-52334/files/1908.06834.pdf" }, { "basename": "41586_2019_1497_Fig10_ESM.jpg", "url": "https://authors.library.caltech.edu/records/548hq-52334/files/41586_2019_1497_Fig10_ESM.jpg" }, { "basename": "41586_2019_1497_Fig5_ESM.jpg", "url": "https://authors.library.caltech.edu/records/548hq-52334/files/41586_2019_1497_Fig5_ESM.jpg" }, { "basename": "41586_2019_1497_Fig6_ESM.jpg", "url": "https://authors.library.caltech.edu/records/548hq-52334/files/41586_2019_1497_Fig6_ESM.jpg" }, { "basename": "41586_2019_1497_Fig7_ESM.jpg", "url": "https://authors.library.caltech.edu/records/548hq-52334/files/41586_2019_1497_Fig7_ESM.jpg" }, { "basename": "41586_2019_1497_Fig8_ESM.jpg", "url": "https://authors.library.caltech.edu/records/548hq-52334/files/41586_2019_1497_Fig8_ESM.jpg" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Kreidberg, Laura; Koll, Daniel D. B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6h75w-73983", "eprint_id": 94592, "eprint_status": "archive", "datestamp": "2023-08-19 15:01:31", "lastmod": "2024-01-14 21:42:14", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "L\u00f3pez-Morales-M", "name": { "family": "L\u00f3pez-Morales", "given": "Mercedes" }, "orcid": "0000-0003-3204-8183" }, { "id": "Currie-T", "name": { "family": "Currie", "given": "Thayne" }, "orcid": "0000-0002-7405-3119" }, { "id": "Teske-J-K", "name": { "family": "Teske", "given": "Johanna K." } }, { "id": "Gaidos-E-J", "name": { "family": "Gaidos", "given": "Eric" }, "orcid": "0000-0002-5258-6846" }, { "id": "Kempton-E-M-R", "name": { "family": "Kempton", "given": "Eliza M.-R." }, "orcid": "0000-0002-1337-9051" }, { "id": "Males-J-R", "name": { "family": "Males", "given": "Jared R." } }, { "id": "Lewis-N-K", "name": { "family": "Lewis", "given": "Nikole K." }, "orcid": "0000-0002-8507-1304" }, { "id": "Rackham-B-V", "name": { "family": "Rackham", "given": "Benjamin V." } }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "id": "Bikby-J", "name": { "family": "Birkby", "given": "Jayne" } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Close-L-M", "name": { "family": "Close", "given": "Laird" }, "orcid": "0000-0002-2167-8246" }, { "id": "Crane-J-D", "name": { "family": "Crane", "given": "Jeff" } }, { "id": "Dressing-C-D", "name": { "family": "Dressing", "given": "Courtney" }, "orcid": "0000-0001-8189-0233" }, { "id": "Froning-C-S", "name": { "family": "Froning", "given": "Cynthia" }, "orcid": "0000-0001-8499-2892" }, { "id": "Hasegawa-Yasuhiro", "name": { "family": "Hasegawa", "given": "Yasuhiro" }, "orcid": "0000-0002-9017-3663" }, { "id": "Konopacky-Q-M", "name": { "family": "Konopacky", "given": "Quinn" }, "orcid": "0000-0002-9936-6285" }, { "id": "Kopparapu-R-K", "name": { "family": "Kopparapu", "given": "Ravi K." } }, { "id": "Mawet-D", "name": { "family": "Mawet", "given": "Dimitri" }, "orcid": "0000-0002-8895-4735" }, { "id": "Mennesson-B", "name": { "family": "Mennesson", "given": "Bertrand" }, "orcid": "0000-0003-4205-4800" }, { "id": "Ramirez-R", "name": { "family": "Ramirez", "given": "Ramses" } }, { "id": "Stelter-D", "name": { "family": "Stelter", "given": "Deno" } }, { "id": "Szentgyorgyi-A-H", "name": { "family": "Szentgyorgyi", "given": "Andrew" }, "orcid": "0000-0002-0255-2525" }, { "id": "Wang-Ji", "name": { "family": "Wang", "given": "Ji" }, "orcid": "0000-0002-4361-8885" } ] }, "title": "Detecting Earth-like Biosignatures on Rocky Exoplanets around Nearby Stars with Ground-based Extremely Large Telescopes", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted - 1903.09523.pdf
", "abstract": "As we begin to discover rocky planets in the habitable zone of nearby stars with missions like TESS and CHEOPS, we will need quick advancements on instrumentation and observational techniques that will enable us to answer key science questions, such as What are the atmospheric characteristics of habitable zone rocky planets? How common are Earth-like biosignatures in rocky\nplanets?} How similar or dissimilar are those planets to Earth? Over the next decade we expect to have discovered several Earth-analog candidates, but we will not have the tools to study the atmospheres of all of them in detail. Ground-based ELTs can identify biosignatures in the spectra of these candidate exo-Earths and understand how the planets' atmospheres compare to the Earth at different epochs. Transit spectroscopy, high-resolution spectroscopy, and reflected-light direct imaging on ELTs can identify multiple biosignatures for habitable zone, rocky planets around M stars at optical to near-infrared wavelengths. Thermal infrared direct imaging can detect habitable zone, rocky planets around AFGK stars, identifying ozone and motivating reflected-light\nfollow-up observations with NASA missions like HabEx/LUVOIR. Therefore, we recommend that the Astro2020 Decadal Survey Committee support: (1) the search for Earth-like biosignatures on rocky planets around nearby stars as a key science case; (2) the construction over the next decade of ground-based Extremely Large Telecopes (ELTs), which will provide the large aperture and\nspatial resolution necessary to start revealing the atmospheres of\nEarth-analogues around nearby stars; (3) the development of instrumentation that optimizes the detection of biosignatures; and (4) the generation of accurate line lists for potential biosignature gases, which are needed as model templates to detect those molecules.", "date": "2019-04-09", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20190409-125055281", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190409-125055281", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.48550/arXiv.1903.09523", "primary_object": { "basename": "1903.09523.pdf", "url": "https://authors.library.caltech.edu/records/6h75w-73983/files/1903.09523.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "L\u00f3pez-Morales, Mercedes; Currie, Thayne; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/w46ah-11w88", "eprint_id": 76837, "eprint_status": "archive", "datestamp": "2023-08-19 02:39:29", "lastmod": "2023-10-25 16:54:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dittmann-J-A", "name": { "family": "Dittmann", "given": "Jason A." } }, { "id": "Irwin-J-M", "name": { "family": "Irwin", "given": "Jonathan M." } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Bonfils-X", "name": { "family": "Bonfils", "given": "Xavier" }, "orcid": "0000-0001-9003-8894" }, { "id": "Astudillo-Defru-N", "name": { "family": "Astudillo-Defru", "given": "Nicola" } }, { "id": "Haywood-R-D", "name": { "family": "Haywood", "given": "Rapha\u00eblle D." }, "orcid": "0000-0001-9140-3574" }, { "id": "Berta-Thompson-Z-K", "name": { "family": "Berta-Thompson", "given": "Zachory K." }, "orcid": "0000-0002-3321-4924" }, { "id": "Newton-E-R", "name": { "family": "Newton", "given": "Elisabeth R." }, "orcid": "0000-0003-4150-841X" }, { "id": "Rodriguez-J-E", "name": { "family": "Rodriguez", "given": "Joseph E." }, "orcid": "0000-0001-8812-0565" }, { "id": "Winters-J-G", "name": { "family": "Winters", "given": "Jennifer G." }, "orcid": "0000-0001-6031-9513" }, { "id": "Tan-Thiam-Guan", "name": { "family": "Tan", "given": "Thiam-Guan" } }, { "id": "Almenara-J-M", "name": { "family": "Almenara", "given": "Jose-Manuel" } }, { "id": "Bouchy-F", "name": { "family": "Bouchy", "given": "Fran\u00e7ois" } }, { "id": "Delfosse-X", "name": { "family": "Delfosse", "given": "Xavier" } }, { "id": "Forveille-T", "name": { "family": "Forveille", "given": "Thierry" } }, { "id": "Lovis-C", "name": { "family": "Lovis", "given": "Christophe" } }, { "id": "Murgas-F", "name": { "family": "Murgas", "given": "Felipe" } }, { "id": "Pepe-F", "name": { "family": "Pepe", "given": "Francesco" } }, { "id": "Santos-N-C", "name": { "family": "Santos", "given": "Nuno C." } }, { "id": "Udry-S", "name": { "family": "Udry", "given": "Stephane" } }, { "id": "W\u00fcnsche-A", "name": { "family": "W\u00fcnsche", "given": "Ana\u00ebl" } }, { "id": "Esquerdo-G-A", "name": { "family": "Esquerdo", "given": "Gilbert A." }, "orcid": "0000-0002-9789-5474" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Dressing-C-D", "name": { "family": "Dressing", "given": "Courtney D." }, "orcid": "0000-0001-8189-0233" } ] }, "title": "A temperate rocky super-Earth transiting a nearby cool star", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 Macmillan Publishers Limited, part of Springer Nature. \n\nReceived 22 December 2016; Accepted 09 March 2017; Published online 19 April 2017. \n\nWe thank the staff at the Cerro Tololo Inter-American Observatory for assistance in the construction and operation of MEarth-South. The MEarth team acknowledges funding from the David and Lucille Packard Fellowship for Science and Engineering (awarded to D.C.). This material is based on work supported by the National Science Foundation under grants AST-0807690, AST-1109468, AST-1004488 (Alan T. Waterman Award) and AST-1616624. This publication was made possible through the support of a grant from the John Templeton Foundation and NASA XRP Program #NNX15AC90G. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. HARPS observations were made with European Southern Observatory (ESO) telescopes under observing programs 191.C-0873 and 198.C-0838. This work was performed in part under contract with the Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. E.R.N. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1602597. N.C.S. acknowledges support from Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT) through national funds and by FEDER through COMPETE2020 by grants UID/FIS/04434/2013&POCI-01-0145-FEDER-007672 and PTDC/FIS-AST/1526/2014&POCI-01-0145-FEDER-016886. N.C.S. was also supported by FCT through Investigador FCT contract reference IF/00169/2012/CP0150/CT0002. X.B., X.D. and T.F. acknowledge the support of the INSU/PNP (Programme national de plan\u00e9tologie) and INSU/PNPS (Programme national de physique stellaire). X.B., J.-M.A. and A.W. acknowledge funding from the European Research Council under ERC Grant Agreement no. 337591-ExTrA. We thank A. Vanderburg for backseat MCMCing. This publication makes use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the National Science Foundation. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the JPL/California Institute of Technology, funded by NASA. This research has made extensive use of the NASA Astrophysics Data System (ADS), and the SIMBAD database, operated at CDS, Strasbourg, France. \n\nCode availability: The EMCEE code is available as a Python install and is publicly available on GitHub (https://github.com/dfm/emcee). JKTEBOP and the modifications performed to it are also publicly available on GitHub (https://github.com/mdwarfgeek/eb). These codes were used to produce the light curve and radial-velocity models used in the analysis of our data. \n\nThe code used to determine the planetary orbit and mass, with Gaussian process regression to account for the magnetic activity variations of the host star, is not yet publically available, but we are currently working to make it so. \n\nData availability: All data used in this work are provided as Supplementary Data, and are available on the MEarth project webpage (https://www.cfa.harvard.edu/MEarth/Welcome.html) and via the online repository FigShare (https://figshare.com/s/9e2b29d4f7a8043ca071 for MEarth and PEST photometry; https://figshare.com/s/49625e95aabf9e1f2ae6 for HARPS radial-velocity data). \n\nThe authors declare no competing financial interests. \n\nNature thanks A. Hatzes and the other anonymous reviewer(s) for their contribution to the peer review of this work.\n\nSubmitted - 1704.05556.pdf
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", "abstract": "M dwarf stars, which have masses less than 60 per cent that of the Sun, make up 75 per cent of the population of the stars in the Galaxy. The atmospheres of orbiting Earth-sized planets are observationally accessible via transmission spectroscopy when the planets pass in front of these stars. Statistical results suggest that the nearest transiting Earth-sized planet in the liquid-water, habitable zone of an M dwarf star is probably around 10.5 parsecs away. A temperate planet has been discovered orbiting Proxima Centauri, the closest M dwarf, but it probably does not transit and its true mass is unknown. Seven Earth-sized planets transit the very low-mass star TRAPPIST-1, which is 12 parsecs away, but their masses and, particularly, their densities are poorly constrained. Here we report observations of LHS 1140b, a planet with a radius of 1.4 Earth radii transiting a small, cool star (LHS 1140) 12 parsecs away. We measure the mass of the planet to be 6.6 times that of Earth, consistent with a rocky bulk composition. LHS 1140b receives an insolation of 0.46 times that of Earth, placing it within the liquid-water, habitable zone. With 90 per cent confidence, we place an upper limit on the orbital eccentricity of 0.29. The circular orbit is unlikely to be the result of tides and therefore was probably present at formation. Given its large surface gravity and cool insolation, the planet may have retained its atmosphere despite the greater luminosity (compared to the present-day) of its host star in its youth. Because LHS 1140 is nearby, telescopes currently under construction might be able to search for specific atmospheric gases in the future.", "date": "2017-04-19", "date_type": "published", "publication": "Nature", "volume": "544", "number": "7650", "publisher": "Nature Publishing Group", "pagerange": "333-336", "id_number": "CaltechAUTHORS:20170424-083045536", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170424-083045536", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "David and Lucille Packard Foundation" }, { "agency": "NSF", "grant_number": "AST-0807690" }, { "agency": "NSF", "grant_number": "AST-1109468" }, { "agency": "NSF", "grant_number": "AST-1004488" }, { "agency": "NSF", "grant_number": "AST-1616624" }, { "agency": "John Templeton Foundation" }, { "agency": "NASA", "grant_number": "NNX15AC90G" }, { "agency": "NASA Sagan Fellowship" }, { "agency": "NSF", "grant_number": "AST-1602597" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "UID/FIS/04434/2013" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "POCI-01-0145-FEDER-007672" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "PTDC/FIS-AST/1526/2014" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "POCI-01-0145-FEDER-016886" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "IF/00169/2012/CP0150/CT0002" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "European Research Council (ERC)", "grant_number": "337591-ExTrA" } ] }, "doi": "10.1038/nature22055", "primary_object": { "basename": "nature22055-sf4.jpg", "url": "https://authors.library.caltech.edu/records/w46ah-11w88/files/nature22055-sf4.jpg" }, "related_objects": [ { "basename": "nature22055-sf5.jpg", "url": "https://authors.library.caltech.edu/records/w46ah-11w88/files/nature22055-sf5.jpg" }, { "basename": "nature22055-sf8.jpg", "url": "https://authors.library.caltech.edu/records/w46ah-11w88/files/nature22055-sf8.jpg" }, { "basename": "1704.05556.pdf", "url": "https://authors.library.caltech.edu/records/w46ah-11w88/files/1704.05556.pdf" }, { "basename": "nature22055-s1.txt", "url": "https://authors.library.caltech.edu/records/w46ah-11w88/files/nature22055-s1.txt" }, { "basename": "nature22055-sf3.jpg", "url": "https://authors.library.caltech.edu/records/w46ah-11w88/files/nature22055-sf3.jpg" }, { "basename": "nature22055-sf6.jpg", "url": "https://authors.library.caltech.edu/records/w46ah-11w88/files/nature22055-sf6.jpg" }, { "basename": "nature22055-sf7.jpg", "url": "https://authors.library.caltech.edu/records/w46ah-11w88/files/nature22055-sf7.jpg" }, { "basename": "nature22055-s2.txt", "url": "https://authors.library.caltech.edu/records/w46ah-11w88/files/nature22055-s2.txt" }, { "basename": "nature22055-sf1.jpg", "url": "https://authors.library.caltech.edu/records/w46ah-11w88/files/nature22055-sf1.jpg" }, { "basename": "nature22055-sf2.jpg", "url": "https://authors.library.caltech.edu/records/w46ah-11w88/files/nature22055-sf2.jpg" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Dittmann, Jason A.; Irwin, Jonathan M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/v8enh-tsw42", "eprint_id": 74442, "eprint_status": "archive", "datestamp": "2023-08-22 19:43:41", "lastmod": "2024-02-02 21:10:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dressing-C-D", "name": { "family": "Dressing", "given": "Courtney D." }, "orcid": "0000-0001-8189-0233" }, { "id": "Newton-E-R", "name": { "family": "Newton", "given": "Elisabeth R." }, "orcid": "0000-0003-4150-841X" }, { "id": "Schlieder-J-E", "name": { "family": "Schlieder", "given": "Joshua E." }, "orcid": "0000-0001-5347-7062" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Vanderburg-A", "name": { "family": "Vanderburg", "given": "Andrew" }, "orcid": "0000-0001-7246-5438" }, { "id": "Sinukoff-E", "name": { "family": "Sinukoff", "given": "Evan" }, "orcid": "0000-0002-5658-0601" } ] }, "title": "Characterizing K2 Candidate Planetary Systems Orbiting Low-mass Stars. I. Classifying Low-mass Host Stars Observed during Campaigns 1\u20137", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems; planets and satellites: fundamental parameters; stars: fundamental parameters; stars: late-type; stars: low-mass; techniques: spectroscopic", "note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 September 5; revised 2016 November 17; accepted 2016 November 18; published 2017 February 17. \n\nMany of our targets were provided by the K2 California Consortium (K2C2). We thank K2C2 for sharing their candidate lists and vetting products. In particular, we thank K2C2 members Ian Crossfield and Arturo Martinez for their willingness to coordinate follow-up observations of low-mass stars. We are grateful to Michael Cushing for sharing a beta version of the Spextool pipeline designed for TripleSpec data. We thank Philip Muirhead and Juliette Becker for providing advice regarding TripleSpec data acquisition and reduction. We also acknowledge helpful conversations with Chas Beichman and Eric Gaidos. We thank Andrew Howard for donating SpeX time and Kimberly Aller, Will Best, and Michael Liu for obtaining some of the SpeX observations described in this paper. Finally, we thank the anonymous referee for providing feedback that improved the quality of this paper. \n\nThis work was performed under contract with the Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed here are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This paper includes data collected by the K2 mission, which is funded by the NASA Science Mission directorate. Our follow-up observations were obtained at the IRTF, which is operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration and at Palomar Observatory. We thank the staff at both observatories and the Caltech Remote Observing Facilities staff for supporting us during our many observing runs. We are grateful to the IRTF and Caltech TACs for awarding us telescope time. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. \n\nThe authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nFacilities: IRTF (SpeX), Palomar (TripleSpec).\n\nPublished - Dressing_2017_ApJ_836_167.pdf
Submitted - 1701.00586.pdf
", "abstract": "We present near-infrared spectra for 144 candidate planetary systems identified during Campaigns 1\u20137 of the NASA K2 Mission. The goal of the survey was to characterize planets orbiting low-mass stars, but our Infrared Telescope Facility/SpeX and Palomar/TripleSpec spectroscopic observations revealed that 49% of our targets were actually giant stars or hotter dwarfs reddened by interstellar extinction. For the 72 stars with spectra consistent with classification as cool dwarfs (spectral types K3\u2013M4), we refined their stellar properties by applying empirical relations based on stars with interferometric radius measurements. Although our revised temperatures are generally consistent with those reported in the Ecliptic Plane Input Catalog (EPIC), our revised stellar radii are typically 0.13 R_\u2299 (39%) larger than the EPIC values, which were based on model isochrones that have been shown to underestimate the radii of cool dwarfs. Our improved stellar characterizations will enable more efficient prioritization of K2 targets for follow-up studies.", "date": "2017-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "836", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 167", "id_number": "CaltechAUTHORS:20170221-161918414", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170221-161918414", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Sagan Fellowship" }, { "agency": "John Templeton Foundation" }, { "agency": "NASA", "grant_number": "NNH14CK55B" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/836/2/167", "primary_object": { "basename": "1701.00586.pdf", "url": "https://authors.library.caltech.edu/records/v8enh-tsw42/files/1701.00586.pdf" }, "related_objects": [ { "basename": "Dressing_2017_ApJ_836_167.pdf", "url": "https://authors.library.caltech.edu/records/v8enh-tsw42/files/Dressing_2017_ApJ_836_167.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Dressing, Courtney D.; Newton, Elisabeth R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/evdee-m8281", "eprint_id": 78367, "eprint_status": "archive", "datestamp": "2023-08-19 00:20:58", "lastmod": "2023-10-26 00:02:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Otor-O-J", "name": { "family": "Otor", "given": "Oderah Justin" } }, { "id": "Montet-B-T", "name": { "family": "Montet", "given": "Benjamin T." }, "orcid": "0000-0001-7516-8308" }, { "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John Asher" }, "orcid": "0000-0001-9808-7172" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Collier-Cameron-A", "name": { "family": "Collier-Cameron", "given": "Andrew" }, "orcid": "0000-0002-8863-7828" }, { "id": "Howard-A-W", "name": { "family": "Howard", "given": "Andrew W." }, "orcid": "0000-0001-8638-0320" }, { "id": "Isaacson-H-T", "name": { "family": "Isaacson", "given": "Howard" }, "orcid": "0000-0002-0531-1073" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "L\u00f3pez-Morales-M", "name": { "family": "L\u00f3pez-Morales", "given": "Mercedes" }, "orcid": "0000-0003-3204-8183" }, { "id": "Lovis-C", "name": { "family": "Lovis", "given": "Christophe" } }, { "id": "Mayor-M", "name": { "family": "Mayor", "given": "Michel" } }, { "id": "Micela-G", "name": { "family": "Micela", "given": "Giusi" }, "orcid": "0000-0002-9900-4751" }, { "id": "Molinari-E", "name": { "family": "Molinari", "given": "Emilio" } }, { "id": "Pepe-F", "name": { "family": "Pepe", "given": "Francesco" } }, { "id": "Piotto-G", "name": { "family": "Piotto", "given": "Giampaolo" } }, { "id": "Phillips-D-F", "name": { "family": "Phillips", "given": "David F." } }, { "id": "Queloz-D", "name": { "family": "Queloz", "given": "Didier" }, "orcid": "0000-0002-3012-0316" }, { "id": "Rice-K", "name": { "family": "Rice", "given": "Ken" } }, { "id": "Sasselov-D-D", "name": { "family": "Sasselov", "given": "Dimitar" }, "orcid": "0000-0001-7014-1771" }, { "id": "S\u00e9gransan-D", "name": { "family": "S\u00e9gransan", "given": "Damien" } }, { "id": "Sozzetti-A", "name": { "family": "Sozzetti", "given": "Alessandro" } }, { "id": "Udry-S", "name": { "family": "Udry", "given": "St\u00e9phane" } }, { "id": "Watson-C-A", "name": { "family": "Watson", "given": "Chris" } } ] }, "title": "The Orbit and Mass of the Third Planet in the Kepler-56 System", "ispublished": "pub", "full_text_status": "public", "keywords": "planets and satellites: fundamental parameters \u2013 planets and satellites: individual (Kepler-56) \u2013 techniques: radial velocities", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 August 10; revised 2016 September 17; accepted 2016 September 21; published 2016 November 15. \n\nWe thank Eric Agol, Daniel Fabrycky, and Daniel Huber for comments and conversations which improved the quality of this manuscript. \n\nO.J.O. thanks the members and friends of the Banneker Institute, who made the summer in which this project began a fruitful time. He also thanks Neta Bahcall for allowing him to continue this research as his senior thesis. He gratefully acknowledges support from the Banneker Institute and Princeton's astrophysics department, Class of 1984, and Office of the Dean of Undergraduate Students in facilitating travel to AAS 227 to present this research. He would be remiss to forget the other members of the Party of Three and their associates. \n\nB.T.M. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE1144469. \n\nJ.A.J. is supported by generous grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. \n\nC.A.W. acknowledges support from STFC grant ST/L000709/1. \n\nThis publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This material is based upon work supported by the National Aeronautics and Space Administration under grant No. NNX15AC90G issued through the Exoplanets Research Program. \n\nThe research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under Grant Agreement No. 313014 (ETAEARTH). \n\nSome of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nThe HARPS-N project was funded by the Prodex program of the Swiss Space Office (SSO), the Harvard University Origin of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queens University Belfast, and University of Edinburgh. \n\nFacilities: Keck:I (HIRES) - , TNG (HARPS-N). -\n\nPublished - Otor_2016_AJ_152_165.pdf
Submitted - 1608.03627.pdf
", "abstract": "While the vast majority of multiple-planet systems have orbital angular momentum axes that align with the spin axis of their host star, Kepler-56 is an exception: its two transiting planets are coplanar yet misaligned by at least 40\u00b0 with respect to the rotation axis of their host star. Additional follow-up observations of Kepler-56 suggest the presence of a massive, non-transiting companion that may help explain this misalignment. We model the transit data along with Keck/HIRES and HARPS-N radial velocity data to update the masses of the two transiting planets and infer the physical properties of the third, non-transiting planet. We employ a Markov Chain Monte Carlo sampler to calculate the best-fitting orbital parameters and their uncertainties for each planet. We find the outer planet has a period of 1002 \u00b1 5 days and minimum mass of 5.61 \u00b1 0.38 M_(Jup). We also place a 95% upper limit of 0.80 m s^(\u22121) yr^(\u22121) on long-term trends caused by additional, more distant companions.", "date": "2016-12", "date_type": "published", "publication": "Astronomical Journal", "volume": "152", "number": "6", "publisher": "American Astronomical Society", "pagerange": "Art. No. 165", "id_number": "CaltechAUTHORS:20170620-092104954", "issn": "1538-3881", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170620-092104954", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000709/1" }, { "agency": "John Templeton Foundation" }, { "agency": "NASA", "grant_number": "NNX15AC90G" }, { "agency": "European Research Council (ERC)", "grant_number": "313014 (ETAEARTH)" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.3847/0004-6256/152/6/165", "primary_object": { "basename": "1608.03627.pdf", "url": "https://authors.library.caltech.edu/records/evdee-m8281/files/1608.03627.pdf" }, "related_objects": [ { "basename": "Otor_2016_AJ_152_165.pdf", "url": "https://authors.library.caltech.edu/records/evdee-m8281/files/Otor_2016_AJ_152_165.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Otor, Oderah Justin; Montet, Benjamin T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/42ay2-fyp07", "eprint_id": 62622, "eprint_status": "archive", "datestamp": "2023-08-22 16:48:19", "lastmod": "2023-10-25 17:17:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Montet-B-T", "name": { "family": "Montet", "given": "Benjamin T." }, "orcid": "0000-0001-7516-8308" }, { "id": "Bowler-B-P", "name": { "family": "Bowler", "given": "Brendan P." }, "orcid": "0000-0003-2649-2288" }, { "id": "Shkolnik-E-L", "name": { "family": "Shkolnik", "given": "Evgenya L." }, "orcid": "0000-0002-7260-5821" }, { "id": "Deck-K-M", "name": { "family": "Deck", "given": "Katherine M." } }, { "id": "Wang-Ji", "name": { "family": "Wang", "given": "Ji" }, "orcid": "0000-0002-4361-8885" }, { "id": "Horch-E-P", "name": { "family": "Horch", "given": "Elliott P." }, "orcid": "0000-0003-2159-1463" }, { "id": "Liu-Michael-C", "name": { "family": "Liu", "given": "Michael C." }, "orcid": "0000-0003-2232-7664" }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." } }, { "id": "Kraus-A-L", "name": { "family": "Kraus", "given": "Adam L." }, "orcid": "0000-0001-9811-568X" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" } ] }, "title": "Dynamical Masses of Young M Dwarfs: Masses and Orbital Parameters of GJ 3305 AB, the Wide Binary Companion to the Imaged Exoplanet Host 51 Eri", "ispublished": "pub", "full_text_status": "public", "keywords": "astrometry; binaries: close; stars: fundamental parameters; stars: individual (GJ 3305 AB)", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 August 25; accepted 2015 October 8; published 2015 October 26. \n\nB.T.M. is supported by the National Science Foundation\nGraduate Research Fellowship under grant No. DGE-1144469.\nThis research has made use of the Keck Observatory Archive\n(KOA), which is operated by the W. M. Keck Observatory and\nthe NASA Exoplanet Science Institute (NExScI), under\ncontract with the National Aeronautics and Space\nAdministration. These results made use of Lowell Observatory's Discovery Channel Telescope. Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications.\nThis publication was made possible through the support of a\ngrant from the John Templeton Foundation. The opinions\nexpressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton\nFoundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\nFacilities: DCT: DSSI, Keck:I (HIRES), Keck:II (NIRC2).\n\nPublished - Montet_2015pL11.pdf
Submitted - 1508.05945v2.pdf
", "abstract": "We combine new high resolution imaging and spectroscopy from Keck/NIRC2, Discovery Channel Telescope/DSSI, and Keck/HIRES with published astrometry and radial velocities to measure individual masses and orbital elements of the GJ 3305 AB system, a young (~20 Myr) M+M binary (unresolved spectral type M0) member of the \u03b2 Pictoris moving group comoving with the imaged exoplanet host 51 Eri. We measure a total system mass of 1.11 \u00b1 0.04 M_\u2299, a period of 29.03 \u00b1 0.50 year, a semimajor axis of 9.78 \u00b1 0.14 AU, and an eccentricity of 0.19 \u00b1 0.02. The primary component has a dynamical mass of 0.67 \u00b1 0.05 M_\u2299 and the secondary has a mass of 0.44 \u00b1 0.05 M_\u2299. The recently updated BHAC15 models are consistent with the masses of both stars to within 1.5\u03c3. Given the observed masses the models predict an age of the GJ 3305 AB system of 37 \u00b1 9 Myr. Based on the observed system architecture and our dynamical mass measurement, it is unlikely that the orbit of 51 Eri b has been significantly altered by the Kozai\u2013Lidov mechanism.", "date": "2015-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "813", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L11", "id_number": "CaltechAUTHORS:20151204-140128306", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151204-140128306", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "NASA" }, { "agency": "John Templeton Foundation" } ] }, "doi": "10.1088/2041-8205/813/1/L11", "primary_object": { "basename": "1508.05945v2.pdf", "url": "https://authors.library.caltech.edu/records/42ay2-fyp07/files/1508.05945v2.pdf" }, "related_objects": [ { "basename": "Montet_2015pL11.pdf", "url": "https://authors.library.caltech.edu/records/42ay2-fyp07/files/Montet_2015pL11.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Montet, Benjamin T.; Bowler, Brendan P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/pckw0-8mn41", "eprint_id": 61552, "eprint_status": "archive", "datestamp": "2023-08-20 08:44:39", "lastmod": "2023-10-23 15:12:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vanderburg-A", "name": { "family": "Vanderburg", "given": "Andrew" }, "orcid": "0000-0001-7246-5438" }, { "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John Asher" }, "orcid": "0000-0001-9808-7172" }, { "id": "Rappaport-S", "name": { "family": "Rappaport", "given": "Saul" }, "orcid": "0000-0003-3182-5569" }, { "id": "Bieryla-A", "name": { "family": "Bieryla", "given": "Allyson" }, "orcid": "0000-0001-6637-5401" }, { "id": "Irwin-J-M", "name": { "family": "Irwin", "given": "Jonathan" } }, { "id": "Lewis-J-A", "name": { "family": "Lewis", "given": "John Arban" } }, { "id": "Kipping-D", "name": { "family": "Kipping", "given": "David" } }, { "id": "Brown-W-R", "name": { "family": "Brown", "given": "Warren R." } }, { "id": "Dufour-P", "name": { "family": "Dufour", "given": "Patrick" } }, { "id": "Ciardi-D-R", "name": { "family": "Ciardi", "given": "David R." }, "orcid": "0000-0002-5741-3047" }, { "id": "Angus-R", "name": { "family": "Angus", "given": "Ruth" } }, { "id": "Schaefer-L", "name": { "family": "Schaefer", "given": "Laura" } }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "Charles" }, "orcid": "0000-0002-5627-5471" }, { "id": "Eastman-J-D", "name": { "family": "Eastman", "given": "Jason" }, "orcid": "0000-0003-3773-5142" }, { "id": "McCrady-N", "name": { "family": "McCrady", "given": "Nate" } }, { "id": "Wittenmyer-R-A", "name": { "family": "Wittenmyer", "given": "Robert A." }, "orcid": "0000-0001-9957-9304" }, { "id": "Wright-J-T", "name": { "family": "Wright", "given": "Jason T." }, "orcid": "0000-0001-6160-5888" } ] }, "title": "A disintegrating minor planet transiting a white dwarf", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2015 Macmillan Publishers Limited. \n\nReceived 11 June 2015. Accepted 26 August 2015. Published online 21 October 2015. \n\nWe thank B. Croll, D. Veras, M. Holman, R. Loomis, J. Becker, K. Deck, H. Schlichting, H. Lin, A. Loeb, and D. Osip for discussions and assistance. We thank C. Allinson, S. Dillet, D. Frostig, A. Johnson, D. Hellstrom, S. Johnson, B. Peak, and T. Reneau for conducting MINERVA observations. We thank M. Wyatt for suggesting how to present Supplementary Fig. 8. A.V. is supported by a National Science Foundation Graduate Research Fellowship (grant DGE 1144152). J.A.J. is supported by grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. The Center for Exoplanets and Habitable Worlds is supported by Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. The MEarth Team acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering (to D.C.), the National Science Foundation under grants AST-0807690, AST-1109468, and AST-1004488 (Alan T. Waterman Award), and a grant from the John Templeton Foundation. The opinions expressed here are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This research has made use of NASA's Astrophysics Data System, the SIMBAD database and VizieR catalog access tool operated at the Centre de Donn\u00e9es astronomiques de Strasbourg, France. Some of the data presented here were obtained from the Mikulski Archive for Space Telescopes (MAST). This paper includes data from the Kepler/K2 mission, the Wide-field Infrared Survey Explorer, the MMT Observatory, the Sloan Digital Sky Survey (SDSS-III), the National Geographic Society\u2014Palomar Observatory Sky Atlas (POSS-I) and the W.M. Keck Observatory. MINERVA is made possible by contributions from its collaborating institutions and Mt Cuba Astronomical Foundation, the David and Lucile Packard Foundation, the National Aeronautics and Space Administration, and the Australian Research Council. We acknowledge the cultural significance of the summit of Maunakea within the indigenous Hawai'ian community. We are grateful for the opportunity to conduct observations from this mountain. \n\nContributions: A.V. processed and searched the K2 data, identified this system, analysed the K2 data for WD 1145+017 (with help from S.R., D.K., and J.T.W.), processed the MINERVA data, measured radial velocities (with help from W.R.B. and D.W.L.), and was the primary author of the manuscript. S.R. performed the dynamical calculations and dust simulations. W.R.B. obtained and reduced the MMT spectra. P.D. analysed the MMT spectra and SDSS photometry to measure spectroscopic properties. J.A.L. analysed archival photometric measurements and modelled the excess infrared emission. A.B. and D.W.L. obtained and processed the FLWO data. J.I. and D.C. obtained and processed the MEarth data. D.R.C. and C.B. obtained and processed the Keck data. R.A. calculated the systematics insensitive periodogram. L.S. calculated vapour pressures for some minerals with MAGMA. J.A.J., J.E., N.M., R.A.W., and J.T.W. made it possible to use MINERVA. J.A.J. provided scientific leadership. \n\nThe authors declare no competing financial interests. \n\nThe raw K2 data are available at http://archive.stsci.edu/k2/data_search/search.php under the identification number 201563164. The processed K2 data are available at https://archive.stsci.edu/missions/hlsp/k2sff/html/c01/ep201563164.html. We have opted not to make the code used in this work available.\n\nSubmitted - 1510.06387.pdf
Supplemental Material - nature15527-s1.pdf
Supplemental Material - nature15527-s2.txt
Supplemental Material - nature15527-s3.txt
Supplemental Material - nature15527-s4.txt
", "abstract": "Most stars become white dwarfs after they have exhausted their nuclear fuel (the Sun will be one such). Between one-quarter and one-half of white dwarfs have elements heavier than helium in their atmospheres, even though these elements ought to sink rapidly into the stellar interiors (unless they are occasionally replenished). The abundance ratios of heavy elements in the atmospheres of white dwarfs are similar to the ratios in rocky bodies in the Solar System. This fact, together with the existence of warm, dusty debris disks surrounding about four per cent of white dwarfs, suggests that rocky debris from the planetary systems of white-dwarf progenitors occasionally pollutes the atmospheres of the stars. The total accreted mass of this debris is sometimes comparable to the mass of large asteroids in the Solar System. However, rocky, disintegrating bodies around a white dwarf have not yet been observed. Here we report observations of a white dwarf\u2014WD 1145+017\u2014being transited by at least one, and probably several, disintegrating planetesimals, with periods ranging from 4.5 hours to 4.9 hours. The strongest transit signals occur every 4.5 hours and exhibit varying depths (blocking up to 40 per cent of the star's brightness) and asymmetric profiles, indicative of a small object with a cometary tail of dusty effluent material. The star has a dusty debris disk, and the star's spectrum shows prominent lines from heavy elements such as magnesium, aluminium, silicon, calcium, iron, and nickel. This system provides further evidence that the pollution of white dwarfs by heavy elements might originate from disrupted rocky bodies such as asteroids and minor planets.", "date": "2015-10-22", "date_type": "published", "publication": "Nature", "volume": "526", "number": "7574", "publisher": "Nature Publishing Group", "pagerange": "546-549", "id_number": "CaltechAUTHORS:20151027-101452236", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151027-101452236", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE 1144152" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Pennsylvania State University" }, { "agency": "Pennsylvania Space Grant Consortium" }, { "agency": "NSF", "grant_number": "AST-0807690" }, { "agency": "NSF", "grant_number": "AST-1109468" }, { "agency": "NSF", "grant_number": "AST-1004488" }, { "agency": "John Templeton Foundation" }, { "agency": "Mt. Cuba Astronomical Foundation" }, { "agency": "NASA" }, { "agency": "Australian Research Council" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1038/nature15527", "primary_object": { "basename": "1510.06387.pdf", "url": "https://authors.library.caltech.edu/records/pckw0-8mn41/files/1510.06387.pdf" }, "related_objects": [ { "basename": "nature15527-s1.pdf", "url": "https://authors.library.caltech.edu/records/pckw0-8mn41/files/nature15527-s1.pdf" }, { "basename": "nature15527-s2.txt", "url": "https://authors.library.caltech.edu/records/pckw0-8mn41/files/nature15527-s2.txt" }, { "basename": "nature15527-s3.txt", "url": "https://authors.library.caltech.edu/records/pckw0-8mn41/files/nature15527-s3.txt" }, { "basename": "nature15527-s4.txt", "url": "https://authors.library.caltech.edu/records/pckw0-8mn41/files/nature15527-s4.txt" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Vanderburg, Andrew; Johnson, John Asher; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9k0dt-nta61", "eprint_id": 62666, "eprint_status": "archive", "datestamp": "2023-08-20 08:37:15", "lastmod": "2023-10-25 17:18:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "West-A-A", "name": { "family": "West", "given": "Andrew A." } }, { "id": "Weisenburger-K-L", "name": { "family": "Weisenburger", "given": "Kolby L." } }, { "id": "Irwin-J", "name": { "family": "Irwin", "given": "Jonathan" } }, { "id": "Berta-Thompson-Z-K", "name": { "family": "Berta-Thompson", "given": "Zachory K." }, "orcid": "0000-0002-3321-4924" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Dittmann-J-A", "name": { "family": "Dittmann", "given": "Jason" } }, { "id": "Pineda-J-S", "name": { "family": "Pineda", "given": "J. Sebastian" }, "orcid": "0000-0002-4489-0135" } ] }, "title": "An Activity\u2013Rotation Relationship and Kinematic Analysis of Nearby Mid-to-Late-Type M Dwarfs", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: activity \u2013 stars: chromospheres \u2013 stars: kinematics and dynamics \u2013 stars: late-type \u2013 stars: lowmass \u2013 stars: rotation", "note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 February 12; accepted 2015 August 22; published 2015 October 2. \n\nThe authors acknowledge Elisabeth Newton, Dylan Morgan,\nand the other members of the Boston Area Drinking And\nSociety for Stars of Elfin Stature for useful conversations in the\npreparation of this manuscript. A.A.W. acknowledges the\nsupport of NSF grants AST-1109273 and AST-1255568 and\nthe Research Corporation for Science Advancement\u02bcs Cottrell\nScholarship. K.L.W. acknowledges the support of the Boston\nUniversity UROP program and the Clare Boothe Luce\nscholarship. Z.K.B.T. gratefully acknowledges support from\nthe Torres Fellowship for Exoplanetary Research. The MEarth\nTeam gratefully acknowledges funding from the David and\nLucille Packard Fellowship for Science and Engineering\n(awarded to D.C.). This material is based upon work supported\nby the National Science Foundation under grants AST-\n0807690, AST-1109468, and AST-1004488 (Alan T. Waterman\nAward). This publication was made possible through the\nsupport of a grant from the John Templeton Foundation. The\nopinions expressed in this publication are those of the authors\nand do not necessarily reflect the views of the John Templeton\nFoundation. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship (to\nJSP) under grant No. DGE-1144469.\n\nPublished - West_2015p3.pdf
Submitted - 1509.01590v1.pdf
", "abstract": "Using spectroscopic observations and photometric light curves of 238 nearby M dwarfs from the MEarth exoplanet transit survey, we examine the relationships between magnetic activity (quantified by H\u03b1 emission), rotation period, and stellar age. Previous attempts to investigate the relationship between magnetic activity and rotation in these stars were hampered by the limited number of M dwarfs with measured rotation periods (and the fact that v sin i measurements probe only rapid rotation). However, the photometric data from MEarth allows us to probe a wide range of rotation periods for hundreds of M dwarf stars (from shorter than one to longer than 100 days). Over all M spectral types that we probe, we find that the presence of magnetic activity is tied to rotation, including for late-type, fully convective M dwarfs. We also find evidence that the fraction of late-type M dwarfs that are active may be higher at longer rotation periods compared to their early-type counterparts, with several active, late-type, slowly rotating stars present in our sample. Additionally, we find that all M dwarfs with rotation periods shorter than 26 days (early-type; M1\u2013M4) and 86 days (late-type; M5\u2013M8) are magnetically active. This potential mismatch suggests that the physical mechanisms that connect stellar rotation to chromospheric heating may be different in fully convective stars. A kinematic analysis suggests that the magnetically active, rapidly rotating stars are consistent with a kinematically young population, while slow-rotators are less active or inactive and appear to belong to an older, dynamically heated stellar population.", "date": "2015-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "812", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 3", "id_number": "CaltechAUTHORS:20151207-154149426", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151207-154149426", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1109273" }, { "agency": "NSF", "grant_number": "AST-1255568" }, { "agency": "Research Corporation" }, { "agency": "Boston University" }, { "agency": "Clare Boothe Luce Postdoctoral Fellowship" }, { "agency": "Torres Fellowship for Exoplanetary Research" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "NSF", "grant_number": "AST-0807690" }, { "agency": "NSF", "grant_number": "AST-1109468" }, { "agency": "NSF", "grant_number": "AST-1004488" }, { "agency": "John Templeton Foundation" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" } ] }, "doi": "10.1088/0004-637X/812/1/3", "primary_object": { "basename": "1509.01590v1.pdf", "url": "https://authors.library.caltech.edu/records/9k0dt-nta61/files/1509.01590v1.pdf" }, "related_objects": [ { "basename": "West_2015p3.pdf", "url": "https://authors.library.caltech.edu/records/9k0dt-nta61/files/West_2015p3.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "West, Andrew A.; Weisenburger, Kolby L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ph38c-p4662", "eprint_id": 58058, "eprint_status": "archive", "datestamp": "2023-08-22 15:31:13", "lastmod": "2024-02-02 21:07:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "D\u00e9sert-J-M", "name": { "family": "D\u00e9sert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" }, { "id": "Fressin-F", "name": { "family": "Fressin", "given": "Fran\u00e7ois" } }, { "id": "Ballard-S", "name": { "family": "Ballard", "given": "Sarah" }, "orcid": "0000-0002-3247-5081" }, { "id": "Bryson-S-T", "name": { "family": "Bryson", "given": "Stephen T." } }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Batalha-N-M", "name": { "family": "Batalha", "given": "Natalie M." } }, { "id": "Borucki-W-J", "name": { "family": "Borucki", "given": "William J." } }, { "id": "Brown-T-M", "name": { "family": "Brown", "given": "Timothy M." }, "orcid": "0000-0002-1793-9968" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Ford-E-B", "name": { "family": "Ford", "given": "Eric B." }, "orcid": "0000-0001-6545-639X" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Gilliland-R-L", "name": { "family": "Gilliland", "given": "Ronald L." }, "orcid": "0000-0002-1554-5578" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Seager-S", "name": { "family": "Seager", "given": "Sara" }, "orcid": "0000-0002-6892-6948" } ] }, "title": "Low False Positive Rate of Kepler Candidates Estimated From A Combination Of Spitzer And Follow-Up Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing; eclipses; planetary systems; planets and satellites: detection; techniques: polarimetric", "note": "\u00a9 2015. The American Astronomical Society.\n\nReceived 26 June 2014, accepted for publication 7 February 2015; Published 30 April 2015.\n\nWe thank the anonymous reviewer for the careful reading of our manuscript and the valuable comments. This work is based on observations made with Kepler, which was competitively selected as the 10th Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. The authors would like to thank the many people who generously gave so much of their time to make this mission a success. This work is also based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. D.C. acknowledges support for this work from grants NNX09AB53G and NNX12AC77G, and G.T. acknowledges support from grants NNX12AC75G and NNX14AB83G, each from the NASA Kepler Mission Participating Scientist Program. D.C. acknowledges the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. We would like to thank the Spitzer staff at IPAC and in particular Nancy Silbermann for scheduling the Spitzer observations of this program. J.-M.D. and S.B. acknowledge the Sagan Exoplanet Fellowship program supported by the National Aeronautics and Space Administration and administered by the NASA Exoplanet Science Institute (NExScI). We thank Samaya Nissanke for careful reading of the manuscript.\n\nPublished - 0004-637X_804_1_59.pdf
Submitted - 1503.03173v1.pdf
", "abstract": "NASA's Kepler mission has provided several thousand transiting planet candidates during the 4 yr of its nominal mission, yet only a small subset of these candidates have been confirmed as true planets. Therefore, the most fundamental question about these candidates is the fraction of bona fide planets. Estimating the rate of false positives of the overall Kepler sample is necessary to derive the planet occurrence rate. We present the results from two large observational campaigns that were conducted with the Spitzer Space Telescope during the the Kepler mission. These observations are dedicated to estimating the false positive rate (FPR) among the Kepler candidates. We select a sub-sample of 51 candidates, spanning wide ranges in stellar, orbital, and planetary parameter space, and we observe their transits with Spitzer at 4.5 \u03bcm. We use these observations to measures the candidate's transit depths and infrared magnitudes. An authentic planet produces an achromatic transit depth (neglecting the modest effect of limb darkening). Conversely a bandpass-dependent depth alerts us to the potential presence of a blending star that could be the source of the observed eclipse: a false positive scenario. For most of the candidates (85%), the transit depths measured with Kepler are consistent with the transit depths measured with Spitzer as expected for planetary objects, while we find that the most discrepant measurements are due to the presence of unresolved stars that dilute the photometry. The Spitzer constraints on their own yield FPRs between 5% and depending on the Kepler Objects of Interest. By considering the population of the Kepler field stars, and by combining follow-up observations (imaging) when available, we find that the overall FPR of our sample is low. The measured upper limit on the FPR of our sample is 8.8% at a confidence level of 3\u03c3. This observational result, which uses the achromatic property of planetary transit signals that is not investigated by the Kepler observations, provides an independent indication that Kepler's FPR is low.", "date": "2015-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "804", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 59", "id_number": "CaltechAUTHORS:20150605-135723176", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150605-135723176", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/804/1/59", "primary_object": { "basename": "0004-637X_804_1_59.pdf", "url": "https://authors.library.caltech.edu/records/ph38c-p4662/files/0004-637X_804_1_59.pdf" }, "related_objects": [ { "basename": "1503.03173v1.pdf", "url": "https://authors.library.caltech.edu/records/ph38c-p4662/files/1503.03173v1.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "D\u00e9sert, Jean-Michel; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/gmgrg-61h92", "eprint_id": 48644, "eprint_status": "archive", "datestamp": "2023-08-22 13:13:41", "lastmod": "2024-02-02 21:04:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zellem-R-T", "name": { "family": "Zellem", "given": "Robert T." }, "orcid": "0000-0001-7547-0398" }, { "id": "Lewis-N-K", "name": { "family": "Lewis", "given": "Nikole K." }, "orcid": "0000-0002-8507-1304" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Griffith-C-A", "name": { "family": "Griffith", "given": "Caitlin A." } }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Laughlin-G-P", "name": { "family": "Laughlin", "given": "Gregory" }, "orcid": "0000-0002-3253-2621" }, { "id": "Langton-J", "name": { "family": "Langton", "given": "Jonathan" } } ] }, "title": "The 4.5 \u03bcm Full-orbit Phase Curve of the Hot Jupiter HD 209458b", "ispublished": "pub", "full_text_status": "public", "keywords": "atmospheric effects; methods: numerical; planets and satellites: general; planets and satellites: individual (HD 209458b); techniques: photometric", "note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2014 March 20; accepted 2014 June 2; published 2014 July 2.\n\nR.Z. and C.A.G. are supported by the NASA Planetary Atmospheres Program.\nN.K.L. performed this work in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute.\nA.P.S. is supported by the NASA Origins program.\nR.Z. would like to thank Travis Barman, Ian J. M. Crossfield, Julien de Wit, Davin Flateau, Joe Giacalone, Tiffany Kataria, Michael R. Line, Julianne I. Moses, Kyle A. Pearson, Emily Rauscher, Tamara M. Rogers, David K. Sing, and Mark R. Swain for their helpful discussions.\n\nWe would like to thank the two referees for their helpful comments and suggestions.\n\nPublished - 0004-637X_790_1_53.pdf
Submitted - 1405.5923v1.pdf
", "abstract": "The hot Jupiter HD 209458b is particularly amenable to detailed study as it is among the brightest transiting exoplanet systems currently known (V-mag = 7.65; K-mag = 6.308) and has a large planet-to-star contrast ratio. HD 209458b is predicted to be in synchronous rotation about its host star with a hot spot that is shifted eastward of the substellar point by superrotating equatorial winds. Here we present the first full-orbit observations of HD 209458b, in which its 4.5\u2009\u03bcm emission was recorded with Spitzer/IRAC. Our study revises the previous 4.5\u2009\u03bcm measurement of HD 209458b's secondary eclipse emission downward by ~35% to 0.1391%^(+0.0072%)_(-0.0069%), changing our interpretation of the properties of its dayside atmosphere. We find that the hot spot on the planet's dayside is shifted eastward of the substellar point by 40\u00b0.9 \u00b1 6\u00b0.0, in agreement with circulation models predicting equatorial superrotation. HD 209458b's dayside (T_(bright) = 1499 \u00b1 15 K) and nightside (T_(bright) = 972 \u00b1 44 K) emission indicate a day-to-night brightness temperature contrast smaller than that observed for more highly irradiated exoplanets, suggesting that the day-to-night temperature contrast may be partially a function of the incident stellar radiation. The observed phase curve shape deviates modestly from global circulation model predictions potentially due to disequilibrium chemistry or deficiencies in the current hot CH4 line lists used in these models. Observations of the phase curve at additional wavelengths are needed in order to determine the possible presence and spatial extent of a dayside temperature inversion, as well as to improve our overall understanding of this planet's atmospheric circulation.", "date": "2014-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "790", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 53", "id_number": "CaltechAUTHORS:20140818-092028974", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140818-092028974", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Sagan Fellowship" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/790/1/53", "primary_object": { "basename": "0004-637X_790_1_53.pdf", "url": "https://authors.library.caltech.edu/records/gmgrg-61h92/files/0004-637X_790_1_53.pdf" }, "related_objects": [ { "basename": "1405.5923v1.pdf", "url": "https://authors.library.caltech.edu/records/gmgrg-61h92/files/1405.5923v1.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Zellem, Robert T.; Lewis, Nikole K.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/kps0x-26333", "eprint_id": 46328, "eprint_status": "archive", "datestamp": "2023-08-22 12:30:53", "lastmod": "2023-10-26 19:40:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ranjan-S", "name": { "family": "Ranjan", "given": "Sukrit" } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "D\u00e9sert-J-M", "name": { "family": "D\u00e9sert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Madhusudhan-N", "name": { "family": "Madhusudhan", "given": "Nikku" }, "orcid": "0000-0002-4869-000X" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Wilkins-A-N", "name": { "family": "Wilkins", "given": "Ashlee" } }, { "id": "Mandell-A-M", "name": { "family": "Mandell", "given": "Avi M." }, "orcid": "0000-0002-8119-3355" } ] }, "title": "Atmospheric Characterization of Five Hot Jupiters with the Wide Field Camera 3 on the Hubble Space Telescope", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; planetary systems; techniques: photometric; techniques: spectroscopic", "note": "\u00a9 2014 American Astronomical Society. Received 2013 June 17; accepted 2014 March 4; published 2014 April 4. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI). These observations are associated with program HST-GO-12181. Support for this program was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities \nfor Research in Astronomy, Inc., under NASA contract\nNAS 5-26555. This material is based upon work supported by\nthe National Science Foundation Graduate Research Fellowship\nunder grant No. DGE-1144152. This work was also performed\nin part under contract with the California Institute of Technology\n(Caltech) funded by NASA through the Sagan Fellowship\nProgram grant awarded to J.-M.D. N.M. acknowledges support\nfrom Yale University through the YCAA postdoctoral prize fellowship.\nThis research has made use of the Exoplanet Orbit\nDatabase and the Exoplanet Data Explorer at exoplanets.org;\nthe SIMBAD database, operated at CDS, Strasbourg, France;\nNASA's Astrophysics Data System Bibliographic Services; and\nSAOImage DS9, developed by Smithsonian Astrophysical Observatory.\nThe authors are grateful to Z. Berta-Thompson and\nJ. Carter for many fruitful discussions, to the STScI HST help\nteam for their assistance, and to an anonymous referee whose\ncomments strengthened the paper.\nFacility: HST (WFC3)\n\nPublished - 0004-637X_785_2_148.pdf
Submitted - 1403.1266v1.pdf
", "abstract": "We probe the structure and composition of the atmospheres of five hot Jupiter exoplanets using the Hubble Space Telescope Wide Field Camera 3 (WFC3) instrument. We use the G141 grism (1.1-1.7 \u03bcm) to study TrES-2b, TrES-4b, and CoRoT-1b in transit; TrES-3b in secondary eclipse; and WASP-4b in both. This wavelength region includes a predicted absorption feature from water at 1.4 \u03bcm, which we expect to be nondegenerate with the other molecules that are likely to be abundant for hydrocarbon-poor (e.g., solar composition) hot Jupiter atmospheres. We divide our wavelength regions into 10 bins. For each bin we produce a spectrophotometric light curve spanning the time of transit or eclipse. We correct these light curves for instrumental systematics without reference to an instrument model. For our transmission spectra, our mean 1\u03c3 precision per bin corresponds to variations of 2.1, 2.8, and 3.0 atmospheric scale heights for TrES-2b, TrES-4b, and CoRoT-1b, respectively. We find featureless spectra for these three planets. We are unable to extract a robust transmission spectrum for WASP-4b. For our dayside emission spectra, our mean 1\u03c3 precision per bin corresponds to a planet-to-star flux ratio of 1.5 \u00d7 10^(\u20134) and 2.1 \u00d7 10^(\u20134) for WASP-4b and TrES-3b, respectively. We combine these estimates with previous broadband measurements and conclude that for both planets isothermal atmospheres are disfavored. We find no signs of features due to water. We confirm that WFC3 is suitable for studies of transiting exoplanets, but in staring mode multivisit campaigns are necessary to place strong constraints on water abundance.", "date": "2014-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "785", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 148", "id_number": "CaltechAUTHORS:20140618-102016119", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140618-102016119", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Space Telescope Science Institute" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144152" }, { "agency": "NASA/Caltech" }, { "agency": "NASA Sagan Fellowship" }, { "agency": "Yale University" } ] }, "doi": "10.1088/0004-637X/785/2/148", "primary_object": { "basename": "1403.1266v1.pdf", "url": "https://authors.library.caltech.edu/records/kps0x-26333/files/1403.1266v1.pdf" }, "related_objects": [ { "basename": "0004-637X_785_2_148.pdf", "url": "https://authors.library.caltech.edu/records/kps0x-26333/files/0004-637X_785_2_148.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ranjan, Sukrit; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/z7nkw-pjv37", "eprint_id": 39492, "eprint_status": "archive", "datestamp": "2023-08-22 10:19:29", "lastmod": "2024-02-02 21:11:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Wilkins-A-N", "name": { "family": "Wilkins", "given": "Ashlee" } }, { "id": "McCullough-P-R", "name": { "family": "McCullough", "given": "Peter" }, "orcid": "0000-0001-9165-9799" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Dobbs-Dixon-I", "name": { "family": "Dobbs-Dixon", "given": "Ian" }, "orcid": "0000-0002-4989-6501" }, { "id": "Madhusudhan-N", "name": { "family": "Madhusudhan", "given": "Nikku" }, "orcid": "0000-0002-4869-000X" }, { "id": "Crouzet-N", "name": { "family": "Crouzet", "given": "Nicolas" } }, { "id": "D\u00e9sert-J-M", "name": { "family": "D\u00e9sert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Gilliland-R-L", "name": { "family": "Gilliland", "given": "Ronald L." }, "orcid": "0000-0002-1554-5578" }, { "id": "Haynes-K", "name": { "family": "Haynes", "given": "Korey" } }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Line-M-R", "name": { "family": "Line", "given": "Michael" }, "orcid": "0000-0002-2338-476X" }, { "id": "Magic-Z", "name": { "family": "Magic", "given": "Zazralt" } }, { "id": "Mandell-A-M", "name": { "family": "Mandell", "given": "Avi M." }, "orcid": "0000-0002-8119-3355" }, { "id": "Ranjan-S", "name": { "family": "Ranjan", "given": "Sukrit" } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Clampin-M-C", "name": { "family": "Clampin", "given": "Mark" } }, { "id": "Seager-S", "name": { "family": "Seager", "given": "Sara" }, "orcid": "0000-0002-6892-6948" }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } } ] }, "title": "Infrared Transmission Spectroscopy of the Exoplanets HD209458b and XO-1b Using the Wide Field Camera-3 on the Hubble Space Telescope", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems; planets and satellites: atmospheres; techniques: photometric; techniques: spectroscopic", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 February 5, accepted for publication 2013 July 10; Published 2013 August 20. \n\nWe are grateful for the excellent support of the staff at STScI for the scheduling and execution of our demanding observations, especially our contact person Shelly Meyett. We also thank an anonymous referee for insightful comments that improved this paper.\n\nPublished - Deming_2013p95.pdf
Submitted - 1302.1141v2.pdf
", "abstract": "Exoplanetary transmission spectroscopy in the near-infrared using the Hubble Space Telescope (HST) NICMOS is currently ambiguous because different observational groups claim different results from the same data, depending on their analysis methodologies. Spatial scanning with HST/WFC3 provides an opportunity to resolve this ambiguity. We here report WFC3 spectroscopy of the giant planets HD 209458b and XO-1b in transit, using spatial scanning mode for maximum photon-collecting efficiency. We introduce an analysis technique that derives the exoplanetary transmission spectrum without the necessity of explicitly decorrelating instrumental effects, and achieves nearly photon-limited precision even at the high flux levels collected in spatial scan mode. Our errors are within 6% (XO-1) and 26% (HD 209458b) of the photon-limit at a resolving power of \u03bb/\u03b4\u03bb ~ 70, and are better than 0.01% per spectral channel. Both planets exhibit water absorption of approximately 200 ppm at the water peak near 1.38 \u03bcm. Our result for XO-1b contradicts the much larger absorption derived from NICMOS spectroscopy. The weak water absorption we measure for HD 209458b is reminiscent of the weakness of sodium absorption in the first transmission spectroscopy of an exoplanet atmosphere by Charbonneau et al. Model atmospheres having uniformly distributed extra opacity of 0.012 cm2 g\u22121 account approximately for both our water measurement and the sodium absorption. Our results for HD 209458b support the picture advocated by Pont et al. in which weak molecular absorptions are superposed on a transmission spectrum that is dominated by continuous opacity due to haze and/or dust. However, the extra opacity needed for HD 209458b is grayer than for HD 189733b, with a weaker Rayleigh component.", "date": "2013-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "774", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 95", "id_number": "CaltechAUTHORS:20130722-101038892", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130722-101038892", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/774/2/95", "primary_object": { "basename": "1302.1141v2.pdf", "url": "https://authors.library.caltech.edu/records/z7nkw-pjv37/files/1302.1141v2.pdf" }, "related_objects": [ { "basename": "Deming_2013p95.pdf", "url": "https://authors.library.caltech.edu/records/z7nkw-pjv37/files/Deming_2013p95.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Deming, Drake; Wilkins, Ashlee; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/rvv36-4qp92", "eprint_id": 41453, "eprint_status": "archive", "datestamp": "2023-08-22 10:06:54", "lastmod": "2023-10-24 23:45:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ballard-S", "name": { "family": "Ballard", "given": "Sarah" }, "orcid": "0000-0002-3247-5081" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Fressin-F", "name": { "family": "Fressin", "given": "Francois" } }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" }, { "id": "Irwin-J-M", "name": { "family": "Irwin", "given": "Jonathan" } }, { "id": "D\u00e9sert-J-M", "name": { "family": "D\u00e9sert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Newton-E-R", "name": { "family": "Newton", "given": "Elisabeth" }, "orcid": "0000-0003-4150-841X" }, { "id": "Mann-A-W", "name": { "family": "Mann", "given": "Andrew W." }, "orcid": "0000-0003-3654-1602" }, { "id": "Ciardi-D-R", "name": { "family": "Ciardi", "given": "David R." }, "orcid": "0000-0002-5741-3047" }, { "id": "Crepp-J-R", "name": { "family": "Crepp", "given": "Justin R." }, "orcid": "0000-0003-0800-0593" }, { "id": "Henze-C-E", "name": { "family": "Henze", "given": "Christopher E." } }, { "id": "Bryson-S-T", "name": { "family": "Bryson", "given": "Stephen T." } }, { "id": "Howell-S-B", "name": { "family": "Howell", "given": "Steven B." }, "orcid": "0000-0002-2532-2853" }, { "id": "Horch-E-P", "name": { "family": "Horch", "given": "Elliott P." }, "orcid": "0000-0003-2159-1463" }, { "id": "Everett-M-E", "name": { "family": "Everett", "given": "Mark E." }, "orcid": "0000-0002-0885-7215" }, { "id": "Shporer-A", "name": { "family": "Shporer", "given": "Avi" }, "orcid": "0000-0002-1836-3120" } ] }, "title": "Exoplanet Characterization by Proxy: A Transiting 2.15 R_\u2295 Planet near the Habitable Zone of the Late K Dwarf Kepler-61", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; planetary systems; stars: individual (Kepler-61, KOI 1361, KIC 6960913)", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2012 September 5; accepted 2013 April 22; published 2013 July 30. \n\nWe thank Perry Berlind and Mike Calkins at the Fred Lawrence Whipple Observatory for gathering the FAST spectra of Kepler-61 and GJ 380. We thank Courtney Dressing for applying the methodology of Dressing & Charbonneau (2013) to deduce the physical properties of Kepler-61 and sharing these values with us. We thank Philip Muirhead, Katherine Hamren, Everett Schlawin, B\u00e1rbara Rojas-Ayala, Kevin Covey, and James Lloyd for gathering, reducing, and sharing the TripleSpec K-band spectrum of Kepler-61. We thank the Spitzer team at the Infrared Processing and Analysis Center in Pasadena, California, and in particular Nancy Silbermann for scheduling the Spitzer observations of this program. This work was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. It was conducted with observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This work is also based on observations made with Kepler, which was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. The authors would like to thank the many people who generously gave so much their time to make this Mission a success. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.\n\nPublished - 0004-637X_773_2_98.pdf
Submitted - 1304.6726v1.pdf
", "abstract": "We present the validation and characterization of Kepler-61b: a 2.15 R_\u2295 planet orbiting near the inner edge of the habitable zone of a low-mass star. Our characterization of the host star Kepler-61 is based upon a comparison with a set of spectroscopically similar stars with directly measured radii and temperatures. We apply a stellar prior drawn from the weighted mean of these properties, in tandem with the Kepler photometry, to infer a planetary radius for Kepler-61b of 2.15 \u00b1 0.13 R_\u2295 and an equilibrium temperature of 273 \u00b1 13 K (given its period of 59.87756 \u00b1 0.00020 days and assuming a planetary albedo of 0.3). The technique of leveraging the physical properties of nearby \"proxy\" stars allows for an independent check on stellar characterization via the traditional measurements with stellar spectra and evolutionary models. In this case, such a check had implications for the putative habitability of Kepler-61b: the planet is 10% warmer and larger than inferred from K-band spectral characterization. From the Kepler photometry, we estimate a stellar rotation period of 36 days, which implies a stellar age of >1 Gyr. We summarize the evidence for the planetary nature of the Kepler-61 transit signal, which we conclude is 30,000 times more likely to be due to a planet than a blend scenario. Finally, we discuss possible compositions for Kepler-61b with a comparison to theoretical models as well as to known exoplanets with similar radii and dynamically measured masses.", "date": "2013-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "773", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 98", "id_number": "CaltechAUTHORS:20130920-141844033", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130920-141844033", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA Sagan Fellowship" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/773/2/98", "primary_object": { "basename": "0004-637X_773_2_98.pdf", "url": "https://authors.library.caltech.edu/records/rvv36-4qp92/files/0004-637X_773_2_98.pdf" }, "related_objects": [ { "basename": "1304.6726v1.pdf", "url": "https://authors.library.caltech.edu/records/rvv36-4qp92/files/1304.6726v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Ballard, Sarah; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7ya07-ttn47", "eprint_id": 39485, "eprint_status": "archive", "datestamp": "2023-08-22 10:06:40", "lastmod": "2024-02-02 21:11:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Baskin-N-J", "name": { "family": "Baskin", "given": "Nathaniel J." } }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Lewis-N-K", "name": { "family": "Lewis", "given": "Nikole K." }, "orcid": "0000-0002-8507-1304" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "D\u00e9sert-J-M", "name": { "family": "Desert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Langton-J", "name": { "family": "Langton", "given": "Jonathan" } }, { "id": "Laughlin-G-P", "name": { "family": "Laughlin", "given": "Gregory" }, "orcid": "0000-0002-3253-2621" }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } } ] }, "title": "Secondary Eclipse Photometry of the Exoplanet WASP-5b with Warm Spitzer", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; planetary systems; techniques: photometric", "note": "\u00a9 2013 American Astronomical Society. Received 2013 March 14, accepted for publication 2013 July 3. Published 2013 August 1.\n\nPublished - 0004-637X_773_2_124.pdf
Submitted - 1303.3886v2.pdf
", "abstract": "We present secondary eclipse photometry of the extrasolar planet WASP-5b taken in the 3.6 and 4.5 \u03bcm bands with the Spitzer Space Telescope's Infrared Array Camera as part of the extended warm mission. By estimating the depth of the secondary eclipse in these two bands we can place constraints on the planet's atmospheric pressure-temperature profile and chemistry. We measure secondary eclipse depths of 0.197% \u00b1 0.028% and 0.237% \u00b1 0.024% in the 3.6 \u03bcm and 4.5 \u03bcm bands, respectively. For the case of a solar-composition atmosphere and chemistry in local thermal equilibrium, our observations are best matched by models showing a hot dayside and, depending on our choice of model, a weak thermal inversion or no inversion at all. We measure a mean offset from the predicted center of eclipse of 3.7 \u00b1 1.8 minutes, corresponding to ecos \u03c9 = 0.0025 \u00b1 0.0012 and consistent with a circular orbit. We conclude that the planet's orbit is unlikely to have been perturbed by interactions with another body in the system as claimed by Fukui et al.", "date": "2013-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "773", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 124", "id_number": "CaltechAUTHORS:20130722-092340344", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130722-092340344", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/773/2/124", "primary_object": { "basename": "0004-637X_773_2_124.pdf", "url": "https://authors.library.caltech.edu/records/7ya07-ttn47/files/0004-637X_773_2_124.pdf" }, "related_objects": [ { "basename": "1303.3886v2.pdf", "url": "https://authors.library.caltech.edu/records/7ya07-ttn47/files/1303.3886v2.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Baskin, Nathaniel J.; Knutson, Heather A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/5wa56-gfc22", "eprint_id": 39562, "eprint_status": "archive", "datestamp": "2023-08-22 09:39:19", "lastmod": "2024-02-02 21:10:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Todorov-K-O", "name": { "family": "Todorov", "given": "Kamen O." }, "orcid": "0000-0002-9276-8118" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Lewis-N-K", "name": { "family": "Lewis", "given": "Nikole K." }, "orcid": "0000-0002-8507-1304" }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "D\u00e9sert-J-M", "name": { "family": "Desert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Sada-P-V", "name": { "family": "Sada", "given": "Pedro V." } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Laughlin-G-P", "name": { "family": "Laughlin", "given": "Gregory" }, "orcid": "0000-0002-3253-2621" }, { "id": "Langton-J", "name": { "family": "Langton", "given": "Jonathan" } }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } } ] }, "title": "Warm Spitzer Photometry of Three Hot Jupiters: HAT-P-3b, HAT-P-4b and HAT-P-12b", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; planetary systems; techniques: photometric", "note": "\u00a9 2013 American Astronomical Society. Received 2013 March 11; accepted 2013 April 30; published 2013 May 30. We thank Jonathan Fraine for helpful discussions on \"prayer bead\" uncertainty estimation. This work is based on observations\nmade with the Spitzer Space Telescope, which is operated\nby the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. We thank\nthe anonymous referee for a careful review of this paper.\n\nPublished - 0004-637X_770_2_102.pdf
Submitted - 1305.0833v1.pdf
", "abstract": "We present Warm Spitzer/IRAC secondary eclipse time series photometry of three short-period transiting exoplanets, HAT-P-3b, HAT-P-4b and HAT-P-12b, in both the available 3.6 and 4.5 \u03bcm bands. HAT-P-3b and HAT-P-4b are Jupiter-mass objects orbiting an early K and an early G dwarf star, respectively. For HAT-P-3b we find eclipse depths of 0.112^(+0.015)_(-0.030) (3.6 \u03bcm) and 0.094^(+0.016)_(-0.009)(4.5 \u03bcm). The HAT-P-4b values are 0.142^(+0.014)_(-0.016)(3.6 \u03bcm) and 0.122^(+0.012)_(-0.014)(4.5 \u03bcm). The two planets' photometry is consistent with inefficient heat redistribution from their day to night sides (and low albedos), but it is inconclusive about possible temperature inversions in their atmospheres. HAT-P-12b is a Saturn-mass planet and is one of the coolest planets ever observed during secondary eclipse, along with the hot Neptune GJ 436b and the hot Saturn WASP-29b. We are able to place 3\u03c3 upper limits on the secondary eclipse depth of HAT-P-12b in both wavelengths: <0.042% (3.6 \u03bcm) and <0.085% (4.5 \u03bcm). We discuss these results in the context of the Spitzer secondary eclipse measurements of GJ 436b and WASP-29b. It is possible that we do not detect the eclipses of HAT-P-12b due to high eccentricity, but find that weak planetary emission in these wavelengths is a more likely explanation. We place 3\u03c3 upper limits on the |e cos \u03c9| quantity (where e is eccentricity and \u03c9 is the argument of periapsis) for HAT-P-3b (<0.0081) and HAT-P-4b (<0.0042), based on the secondary eclipse timings.", "date": "2013-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "770", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 102", "id_number": "CaltechAUTHORS:20130724-141445119", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130724-141445119", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Pennsylvania State University" }, { "agency": "Eberly College of Science" }, { "agency": "Pennsylvania Space Grant Consortium" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/770/2/102", "primary_object": { "basename": "0004-637X_770_2_102.pdf", "url": "https://authors.library.caltech.edu/records/5wa56-gfc22/files/0004-637X_770_2_102.pdf" }, "related_objects": [ { "basename": "1305.0833v1.pdf", "url": "https://authors.library.caltech.edu/records/5wa56-gfc22/files/1305.0833v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Todorov, Kamen O.; Deming, Drake; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qsa9y-0ah53", "eprint_id": 38255, "eprint_status": "archive", "datestamp": "2023-08-22 09:04:20", "lastmod": "2024-02-02 21:07:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lewis-N-K", "name": { "family": "Lewis", "given": "Nikole K." }, "orcid": "0000-0002-8507-1304" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Laughlin-G-P", "name": { "family": "Laughlin", "given": "Gregory" }, "orcid": "0000-0002-3253-2621" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Crepp-J-R", "name": { "family": "Crepp", "given": "Justin R." }, "orcid": "0000-0003-0800-0593" }, { "id": "Mighell-K-J", "name": { "family": "Mighell", "given": "Kenneth J." } }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Bakos-G-\u00c1", "name": { "family": "Bakos", "given": "G\u00e1sp\u00e1r \u00c1." }, "orcid": "0000-0001-7204-6727" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "D\u00e9sert-J-M", "name": { "family": "D\u00e9sert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Fischer-D-A", "name": { "family": "Fischer", "given": "Debra A." }, "orcid": "0000-0003-2221-0861" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Hartman-J-D", "name": { "family": "Hartman", "given": "Joel D." }, "orcid": "0000-0001-8732-6166" }, { "id": "Hinkley-S", "name": { "family": "Hinkley", "given": "Sasha" }, "orcid": "0000-0001-8074-2562" }, { "id": "Howard-A-W", "name": { "family": "Howard", "given": "Andrew W." }, "orcid": "0000-0001-8638-0320" }, { "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John Asher" }, "orcid": "0000-0001-9808-7172" }, { "id": "Kao-Melodie-M", "name": { "family": "Kao", "given": "Melodie" }, "orcid": "0000-0001-5125-1414" }, { "id": "Langton-J", "name": { "family": "Langton", "given": "Jonathan" } }, { "id": "Marcy-G-W", "name": { "family": "Marcy", "given": "Geoffrey W." }, "orcid": "0000-0002-2909-0113" } ] }, "title": "Orbital Phase Variations of the Eccentric Giant Planet HAT-P-2b", "ispublished": "pub", "full_text_status": "public", "keywords": "atmospheric effects; methods: numerical; planets and satellites: general; planets and satellites: individual (HAT-P-2b); techniques: photometric", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2012 October 18; accepted 2013 February 19; published 2013 March 13. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by JPL/Caltech. N.K.L. was further supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program (NNX08AX02H), Origins Program (NNX08AF27G), and in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. N.K.L. wishes to thank B. K. Jackson and J. A. Carter for many useful discussions during the preparation of this manuscript and the anonymous referee for their helpful suggestions.\n\nPublished - 0004-637X_766_2_95.pdf
Accepted Version - 1302.5084.pdf
", "abstract": "We present the first secondary eclipse and phase curve observations for the highly eccentric hot Jupiter HAT-P-2b in the 3.6, 4.5, 5.8, and 8.0 \u03bcm bands of the Spitzer Space Telescope. The 3.6 and 4.5 \u03bcm data sets span an entire orbital period of HAT-P-2b (P = 5.6334729 d), making them the longest continuous phase curve observations obtained to date and the first full-orbit observations of a planet with an eccentricity exceeding 0.2. We present an improved non-parametric method for removing the intrapixel sensitivity variations in Spitzer data at 3.6 and 4.5 \u03bcm that robustly maps position-dependent flux variations. We find that the peak in planetary flux occurs at 4.39 \u00b1 0.28, 5.84 \u00b1 0.39, and 4.68 \u00b1 0.37 hr after periapse passage with corresponding maxima in the planet/star flux ratio of 0.1138% \u00b1 0.0089%, 0.1162% \u00b1 0.0080%, and 0.1888% \u00b1 0.0072% in the 3.6, 4.5, and 8.0 \u03bcm bands, respectively. Our measured secondary eclipse depths of 0.0996% \u00b1 0.0072%, 0.1031% \u00b1 0.0061%, 0.071%^(+0.029%)_(-0.013%), and 0.1392% \u00b1 0.0095% in the 3.6, 4.5, 5.8, and 8.0 \u03bcm bands, respectively, indicate that the planet cools significantly from its peak temperature before we measure the dayside flux during secondary eclipse. We compare our measured secondary eclipse depths to the predictions from a one-dimensional radiative transfer model, which suggests the possible presence of a transient day side inversion in HAT-P-2b's atmosphere near periapse. We also derive improved estimates for the system parameters, including its mass, radius, and orbital ephemeris. Our simultaneous fit to the transit, secondary eclipse, and radial velocity data allows us to determine the eccentricity (e = 0.50910 \u00b1 0.00048) and argument of periapse (\u03c9 = 188\u00b0.09 \u00b1 0\u00b0.39) of HAT-P-2b's orbit with a greater precision than has been achieved for any other eccentric extrasolar planet. We also find evidence for a long-term linear trend in the radial velocity data. This trend suggests the presence of another substellar companion in the HAT-P-2 system, which could have caused HAT-P-2b to migrate inward to its present-day orbit via the Kozai mechanism.", "date": "2013-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "766", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 95", "id_number": "CaltechAUTHORS:20130503-092758220", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130503-092758220", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "NNX08AX02H" }, { "agency": "NASA", "grant_number": "NNX08AF27G" }, { "agency": "Caltech" }, { "agency": "NASA Sagan Fellowship" }, { "agency": "NASA Exoplanet Science Institute" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/766/2/95", "primary_object": { "basename": "0004-637X_766_2_95.pdf", "url": "https://authors.library.caltech.edu/records/qsa9y-0ah53/files/0004-637X_766_2_95.pdf" }, "related_objects": [ { "basename": "1302.5084.pdf", "url": "https://authors.library.caltech.edu/records/qsa9y-0ah53/files/1302.5084.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Lewis, Nikole K.; Knutson, Heather A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6gwc9-f1j62", "eprint_id": 35389, "eprint_status": "archive", "datestamp": "2023-08-22 06:28:01", "lastmod": "2023-10-20 16:10:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Xiao-Hing-Yu", "name": { "family": "Xiao", "given": "Hong Yu" } }, { "id": "Covey-K-R", "name": { "family": "Covey", "given": "Kevin R." }, "orcid": "0000-0001-6914-7797" }, { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "Luisa" }, "orcid": "0000-0001-6381-515X" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "Georgi" } }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis" }, "orcid": "0000-0002-4858-6106" }, { "id": "Slesnick-C-L", "name": { "family": "Slesnick", "given": "Catherine" } }, { "id": "Lloyd-J-P", "name": { "family": "Lloyd", "given": "James P." } } ] }, "title": "A Census of Rotation and Variability in L1495: A Uniform Analysis of Trans-atlantic Exoplanet Survey Light Curves for Pre-main-sequence Stars in Taurus", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: pre-main sequence; stars: rotation", "note": "\u00a9 2012 American Astronomical Society. Received 2012 January 6; accepted 2012 July 10; published 2012 August 28. The authors thank Lynne Hillenbrand for helping motivate the TrES team to monitor L1495; Michael Meyer and Eric Mamajek for useful discussions that inspired this analysis of the data; Eric Feigelson, Adam Miller, and Joseph Richards for informative discussions of period detection techniques that\nwould be robust against the presence of red noise; and Jerome Bouvier for noting that v sin i measurements may support LkCa 21's sub-day period. We also thank the anonymous referee for thoughtful comments which spurred several improvements to the analysis and interpretation presented here. K.R.C. acknowledges support for this work from the Hubble Fellowship Program, provided by NASA through Hubble Fellowship grant HST-HF-51253.01-A awarded by the STScI, which is operated by the AURA, Inc., for NASA, under contract NAS 5-26555. This material is based on work that was supported by NASA under grants NNG05GJ29G issued through the Origins of Solar Systems Program.\nThis research has made use of NASA's Astrophysics Data\nSystem Bibliographic Services, the SIMBAD database, operated\nat CDS, Strasbourg, France, the NASA/IPAC Extragalactic\nDatabase, operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology, under contract with the National Aeronautics and Space Administration, and the VizieR database of astronomical catalogs (Ochsenbein et al. 2000). IRAF (Image Reduction and Analysis Facility) is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.\nThe Two Micron All Sky Survey was a joint project of\nthe University of Massachusetts and the Infrared Processing\nand Analysis Center (California Institute of Technology). The University of Massachusetts was responsible for the overall management of the project, the observing facilities, and the data acquisition. The Infrared Processing and Analysis Center was responsible for data processing, data distribution, and data archiving.\n\nPublished - 0067-0049_202_1_7.pdf
", "abstract": "We analyze light curves obtained by the Trans-atlantic Exoplanet Survey (TrES) for a field centered on the L1495 dark cloud in Taurus. The Spitzer Taurus Legacy Survey catalog identifies 179 bona fide Taurus members within the TrES field; 48 of the known Taurus members are detected by TrES, as well as 26 candidate members identified by the Spitzer Legacy team. We quantify the variability of each star in our sample using the ratio of the standard deviation of the original light curve (\u03c3_(orig.)) to the standard deviation of a light curve that has been smoothed by 9 or 1001 epochs (\u03c3_9 and \u03c3_(1001), respectively). Known Taurus members typically demonstrate (\u03c3_(orig.)/\u03c3_9) < 2.0, and (\u03c3_(orig.)/\u03c3_(1001)) < 5, while field stars reveal (\u03c3_(orig.)/\u03c3_9) ~ 3.0 and (\u03c3_(orig.)/\u03c3_(1001)) ~ 10, as expected for light curves dominated by unstructured white noise. Of the 74 Taurus members/candidates with TrES light curves, we detect significant variability in 49 sources. Adapting a quantitative metric originally developed to assess the reliability of transit detections, we measure the amount of red and white noise in each light curve and identify 18 known or candidate Taurus members with highly significant period measurements. These appear to be the first periods measured for four of these sources (HD 282276, CX Tau, FP Tau, TrES J042423+265008), and in two other cases, the first non-aliased periods (LkCa 21 and DK Tau AB). For the remainder, the TrES measurements typically agree very well (\u03b4P < 1%) with previously reported values. Including periods measured at lower confidence for 15 additional sources, we report periods for 11 objects where no previous periods were found, including 8 confirmed Taurus members. We also identify 10 of the 26 candidate Taurus members that demonstrate variability levels consistent with being bona fide T Tauri stars. A Kolomgorov-Smirnov (K-S) test confirms that these new periods confirm the distinction between the rotation period distributions of stars with and without circumstellar disks, with only a 10% probability of the two populations sharing the same parent period distribution. K-S tests do suggest, however, that the updated Taurus period distribution now more closely resembles those measured in other young star-forming clusters (i.e., NGC 2264, NGC 6530, and the ONC). This improved agreement may reflect the exclusion of long rotation periods which are detected in Taurus at lower significance, and which may be beyond the limits of detectability in more distant star-forming regions.", "date": "2012-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "202", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 7", "id_number": "CaltechAUTHORS:20121109-120803100", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121109-120803100", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51235.01" }, { "agency": "Space Telescope Science Institute" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA", "grant_number": "NNG05GJ29G" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/202/1/7", "primary_object": { "basename": "0067-0049_202_1_7.pdf", "url": "https://authors.library.caltech.edu/records/6gwc9-f1j62/files/0067-0049_202_1_7.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Xiao, Hong Yu; Covey, Kevin R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/5f7q5-wdx80", "eprint_id": 32982, "eprint_status": "archive", "datestamp": "2023-08-22 06:12:41", "lastmod": "2024-02-02 21:04:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Lewis-N-K", "name": { "family": "Lewis", "given": "Nikole" }, "orcid": "0000-0002-8507-1304" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Aigrain-S", "name": { "family": "Aigrain", "given": "Suzanne" }, "orcid": "0000-0003-1453-0574" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "D\u00e9sert-J-M", "name": { "family": "D\u00e9sert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Henry-G-W", "name": { "family": "Henry", "given": "Gregory W." }, "orcid": "0000-0003-4155-8513" }, { "id": "Langton-J", "name": { "family": "Langton", "given": "Jonathan" } }, { "id": "Laughlin-G-P", "name": { "family": "Laughlin", "given": "Gregory" }, "orcid": "0000-0002-3253-2621" } ] }, "title": "3.6 and 4.5 \u03bcm Phase Curves and Evidence for Non-equilibrium Chemistry in the Atmosphere of Extrasolar Planet HD 189733b", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing; planetary systems; techniques: photometric", "note": "\u00a9 2012 The American Astronomical Society.\nReceived 2012 February 22; accepted 2012 May 5; published 2012 June 29.\nWe thank Josh Carter for his assistance in implementing a\nwavelet MCMC analysis for these data. This work is based on\nobservations made with the Spitzer Space Telescope, which is\noperated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. H.A.K. was supported in part by a fellowship from the Miller Institute for Basic Research in Science.\n\nPublished - Knutson2012p19058Astrophys_J.pdf
Submitted - 1206.6887v1.pdf
", "abstract": "We present new, full-orbit observations of the infrared phase variations of the canonical hot Jupiter HD 189733b obtained in the 3.6 and 4.5 \u03bcm bands using the Spitzer Space Telescope. When combined with previous phase curve observations at 8.0 and 24 \u03bcm, these data allow us to characterize the exoplanet's emission spectrum as a function of planetary longitude and to search for local variations in its vertical thermal profile and atmospheric composition. We utilize an improved method for removing the effects of intrapixel sensitivity variations and robustly extracting phase curve signals from these data, and we calculate our best-fit parameters and uncertainties using a wavelet-based Markov Chain Monte Carlo analysis that accounts for the presence of time-correlated noise in our data. We measure a phase curve amplitude of 0.1242% \u00b1 0.0061% in the 3.6 \u03bcm band and 0.0982% \u00b1 0.0089% in the 4.5 \u03bcm band, corresponding to brightness temperature contrasts of 503 \u00b1 21 K and 264 \u00b1 24 K, respectively. We find that the times of minimum and maximum flux occur several hours earlier than predicted for an atmosphere in radiative equilibrium, consistent with the eastward advection of gas by an equatorial super-rotating jet. The locations of the flux minima in our new data differ from our previous observations at 8 \u03bcm, and we present new evidence indicating that the flux minimum observed in the 8 \u03bcm is likely caused by an overshooting effect in the 8 \u03bcm array. We obtain improved estimates for HD 189733b's dayside planet-star flux ratio of 0.1466% \u00b1 0.0040% in the 3.6 \u03bcm band and 0.1787% \u00b1 0.0038% in the 4.5 \u03bcm band, corresponding to brightness temperatures of 1328 \u00b1 11 K and 1192 \u00b1 9 K, respectively; these are the most accurate secondary eclipse depths obtained to date for an extrasolar planet. We compare our new dayside and nightside spectra for HD 189733b to the predictions of one-dimensional radiative transfer models from Burrows et al. and conclude that fits to this planet's dayside spectrum provide a reasonably accurate estimate of the amount of energy transported to the night side. Our 3.6 and 4.5 \u03bcm phase curves are generally in good agreement with the predictions of general circulation models for this planet from Showman et al., although we require either excess drag or slower rotation rates in order to match the locations of the measured maxima and minima in the 4.5, 8.0, and 24 \u03bcm bands. We find that HD 189733b's 4.5 \u03bcm nightside flux is 3.3\u03c3 smaller than predicted by these models, which assume that the chemistry is in local thermal equilibrium. We conclude that this discrepancy is best explained by vertical mixing, which should lead to an excess of CO and correspondingly enhanced 4.5 \u03bcm absorption in this region. This result is consistent with our constraints on the planet's transmission spectrum, which also suggest excess absorption in the 4.5 \u03bcm band at the day-night terminator.", "date": "2012-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "754", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 22", "id_number": "CaltechAUTHORS:20120807-121059996", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120807-121059996", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Miller Institute for Basic Research in Science" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/754/1/22", "primary_object": { "basename": "1206.6887v1.pdf", "url": "https://authors.library.caltech.edu/records/5f7q5-wdx80/files/1206.6887v1.pdf" }, "related_objects": [ { "basename": "Knutson2012p19058Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/5f7q5-wdx80/files/Knutson2012p19058Astrophys_J.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Knutson, Heather A.; Lewis, Nikole; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/gh8wn-g4f92", "eprint_id": 31610, "eprint_status": "archive", "datestamp": "2023-08-22 04:56:30", "lastmod": "2024-02-02 21:02:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Todorov-K-O", "name": { "family": "Todorov", "given": "Kamen O." }, "orcid": "0000-0002-9276-8118" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Sada-P-V", "name": { "family": "Sada", "given": "Pedro V." } }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "D\u00e9sert-J-M", "name": { "family": "Desert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Laughlin-G-P", "name": { "family": "Laughlin", "given": "Gregory" }, "orcid": "0000-0002-3253-2621" }, { "id": "Langton-J", "name": { "family": "Langton", "given": "Jonathan" } }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } }, { "id": "Lewis-N-K", "name": { "family": "Lewis", "given": "Nikole K." }, "orcid": "0000-0002-8507-1304" } ] }, "title": "Warm Spitzer Observations of Three Hot Exoplanets: XO-4b, HAT-P-6b, and HAT-P-8b", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; planetary systems; techniques: photometric", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2011 July 7; accepted 2011 November 23; published 2012 January 27.\n\nThis work is based on observations made with the Spitzer\nSpace Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. We thank the anonymous referee for a careful review of this paper.\n\nPublished - Todorov2012p18199Astrophys_J.pdf
", "abstract": "We analyze Warm Spitzer/Infrared Array Camera observations of the secondary eclipses of three planets, XO-4b, HAT-P-6b, and HAT-P-8b. We measure secondary eclipse amplitudes at 3.6 \u03bcm and 4.5 \u03bcm for each target. XO-4b exhibits a stronger eclipse depth at 4.5 \u03bcm than at 3.6 \u03bcm, which is consistent with the presence of a temperature inversion. HAT-P-8b shows a stronger eclipse amplitude at 3.6 \u03bcm and is best described by models without a temperature inversion. The eclipse depths of HAT-P-6b can be fitted with models with a small or no temperature inversion. We consider our results in the context of a postulated relationship between stellar activity and temperature inversion and a relationship between irradiation level and planet dayside temperature, as discussed by Knutson et al. and Cowan & Agol, respectively. Our results are consistent with these hypotheses, but do not significantly strengthen them. To measure accurate secondary eclipse central phases, we require accurate ephemerides. We obtain primary transit observations and supplement them with publicly available observations to update the orbital ephemerides of the three planets. Based on the secondary eclipse timing, we set upper boundaries for e cos(\u03c9) for HAT-P-6b, HAT-P-8b, and XO-4b and find that the values are consistent with circular orbits.", "date": "2012-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "746", "number": "1", "publisher": "American Astronomical Society", "pagerange": "111", "id_number": "CaltechAUTHORS:20120523-103519192", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120523-103519192", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Pennsylvania State University" }, { "agency": "Eberly College of Science" }, { "agency": "Pennsylvania Space Grant Consortium" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/746/1/111", "primary_object": { "basename": "Todorov2012p18199Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/gh8wn-g4f92/files/Todorov2012p18199Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Todorov, Kamen O.; Deming, Drake; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1egw2-0h014", "eprint_id": 36671, "eprint_status": "archive", "datestamp": "2023-08-22 04:46:07", "lastmod": "2024-02-02 21:06:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fressin-F", "name": { "family": "Fressin", "given": "Francois" } }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" }, { "id": "Pont-F", "name": { "family": "Pont", "given": "Frederic" }, "orcid": "0000-0003-0076-5444" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Mazeh-T", "name": { "family": "Mazeh", "given": "Tsevi" } }, { "id": "Aigrain-S", "name": { "family": "Aigrain", "given": "Suzanne" }, "orcid": "0000-0003-1453-0574" }, { "id": "Fridlund-M", "name": { "family": "Fridlund", "given": "Malcolm" } }, { "id": "Henze-C-E", "name": { "family": "Henze", "given": "Christopher E." } }, { "id": "Guillot-T", "name": { "family": "Guillot", "given": "Tristan" }, "orcid": "0000-0002-7188-8428" }, { "id": "Rauer-H", "name": { "family": "Rauer", "given": "Heike" } } ] }, "title": "Spitzer Infrared Observations and Independent Validation of the Transiting Super-Earth CoRoT-7 b", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing; planetary systems; stars: individual: CoRoT-7; stars: statistics; techniques: photometric", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 July 18; accepted 2011 October 24; published 2011 December 29. \n\nWe are grateful to the anonymous referee for many very helpful comments and suggestions. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This research has made use of the facilities at the NASA Advanced Supercomputing Division (NASA Ames Research Center).\n\nPublished - 0004-637X_745_1_81.pdf
Accepted Version - 1110.5336.pdf
", "abstract": "The detection and characterization of the first transiting super-Earth, CoRoT-7 b, has required an unprecedented effort in terms of telescope time and analysis. Although the star does display a radial-velocity signal at the period of the planet, this has been difficult to disentangle from the intrinsic stellar variability and pinning down the velocity amplitude has been very challenging. As a result, the precise value of the mass of the planet\u2014and even the extent to which it can be considered to be confirmed\u2014has been debated in the recent literature, with six mass measurements published so far based on the same spectroscopic observations, ranging from about 2 to 8 Earth masses. Here we report on an independent validation of the planet discovery using one of the fundamental properties of a transit signal: its achromaticity. We observed four transits of CoRoT-7 b at 4.5 \u03bcm and 8.0 \u03bcm with the Infrared Array Camera (IRAC) on board the Spitzer Space Telescope in order to determine whether the depth of the transit signal in the near-infrared is consistent with that observed in the CoRoT bandpass, as expected for a planet. We detected the transit and found an average depth of 0.426 \u00b1 0.115 mmag at 4.5 \u03bcm, which is in good agreement with the depth of 0.350 \u00b1 0.011 mmag (ignoring limb darkening) found by CoRoT. The observations at 8.0 \u03bcm did not yield a significant detection. The 4.5 \u03bcm observations place important constraints on the kinds of astrophysical false positives that could mimic the signal. Combining this with additional constraints reported earlier, we performed an exhaustive exploration of possible blend scenarios for CoRoT-7 b using the BLENDER technique. We are able to rule out the vast majority of false positives, and the remaining ones are found to be much less likely than a true transiting planet. We thus validate CoRoT-7 b as a bona fide planet with a very high degree of confidence, independently of any radial-velocity information. Our Spitzer observations have additionally allowed us to significantly improve the ephemeris of the planet, so that future transits should be recoverable well into the next decade. In its warm phase Spitzer is expected to be an essential tool for the validation, along the lines of the present analysis, of transiting planet candidates with shallow signals from CoRoT as well as from the Kepler mission, including potentially rocky planets in the habitable zones of their parent stars.", "date": "2012-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "745", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 81", "id_number": "CaltechAUTHORS:20130129-154459823", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-154459823", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/745/1/81", "primary_object": { "basename": "1110.5336.pdf", "url": "https://authors.library.caltech.edu/records/1egw2-0h014/files/1110.5336.pdf" }, "related_objects": [ { "basename": "0004-637X_745_1_81.pdf", "url": "https://authors.library.caltech.edu/records/1egw2-0h014/files/0004-637X_745_1_81.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Fressin, Francois; Torres, Guillermo; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7yhy1-ean86", "eprint_id": 28583, "eprint_status": "archive", "datestamp": "2023-08-22 04:04:41", "lastmod": "2023-10-24 18:00:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blomme-J", "name": { "family": "Blomme", "given": "J." } }, { "id": "Sarro-L-M", "name": { "family": "Sarro", "given": "L. M." } }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "F. T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Debosscher-J", "name": { "family": "Debosscher", "given": "J." } }, { "id": "Brown-T", "name": { "family": "Brown", "given": "T." } }, { "id": "Lopez-M", "name": { "family": "Lopez", "given": "M." } }, { "id": "Dubath-P", "name": { "family": "Dubath", "given": "P." } }, { "id": "Rimoldini-L", "name": { "family": "Rimoldini", "given": "L." } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "D." }, "orcid": "0000-0002-9003-484X" }, { "id": "Dunham-E", "name": { "family": "Dunham", "given": "E." } }, { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "G." } }, { "id": "Ciardi-D-R", "name": { "family": "Ciardi", "given": "D. R." }, "orcid": "0000-0002-5741-3047" }, { "id": "De-Ridder-J", "name": { "family": "De Ridder", "given": "J." } }, { "id": "Aerts-C", "name": { "family": "Aerts", "given": "C." }, "orcid": "0000-0003-1822-7126" } ] }, "title": "Improved methodology for the automated classification of periodic variable stars", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis; methods: statistical; techniques: photometric", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. \n\nAccepted 2011 July 18. Received 2011 July 18; in original form 2010 October 2. Article first published online: 22 Sep. 2011. \n\nThe research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 227224 (PROSPERITY), the Research Council of K. U. Leuven (GOA/2008/04), from the Fund for Scientific Research of Flanders (G.0332.06), the Belgian Federal Science Policy Office (C90309: CoRoT Data Exploitation, C90291 Gaia-DPAC) and the Spanish Ministerio de Educaci\u03ccn y Ciencia through grant AYA2005-04286. Public access to the TrES data was provided to the through the NASA Star and Exoplanet Database (NStED, http://nsted.ipac.caltech.edu).\n\nPublished - Blomme2011p16563Mon_Not_R_Astron_Soc.pdf
Supplemental Material - MNR_19466_sm_Table6.zip
", "abstract": "We present a novel automated methodology to detect and classify periodic variable stars in a large data base of photometric time series. The methods are based on multivariate Bayesian statistics and use a multistage approach. We applied our method to the ground-based data of the Trans-Atlantic Exoplanet Survey (TrES) Lyr1 field, which is also observed by the Kepler satellite, covering ~26 000 stars. We found many eclipsing binaries as well as classical non-radial pulsators, such as slowly pulsating B stars, \u03b3 Doradus, \u03b2 Cephei and \u03b4 Scuti stars. Also a few classical radial pulsators were found.", "date": "2011-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "418", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "96-106", "id_number": "CaltechAUTHORS:20111223-085345434", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111223-085345434", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "227224 (PROSPERITY)" }, { "agency": "Research Council of K. U. Leuven", "grant_number": "GOA/2008/04" }, { "agency": "Fonds Wetenschappelijk Onderzoek - Vlaanderen (FWO)", "grant_number": "G.0332.06" }, { "agency": "Belgian Federal Science Policy Office (BELSPO)", "grant_number": "C90309" }, { "agency": "Belgian Federal Science Policy Office (BELSPO)", "grant_number": "C90291" }, { "agency": "Minsterio de Educaci\u00f3n y Ciencia (MEC)", "grant_number": "AYA2005-04286" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2011.19466.x", "primary_object": { "basename": "MNR_19466_sm_Table6.zip", "url": "https://authors.library.caltech.edu/records/7yhy1-ean86/files/MNR_19466_sm_Table6.zip" }, "related_objects": [ { "basename": "Blomme2011p16563Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/7yhy1-ean86/files/Blomme2011p16563Mon_Not_R_Astron_Soc.pdf" } ], "resource_type": "article", "pub_year": "2011", "author_list": "Blomme, J.; Sarro, L. M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/mrhw2-n7610", "eprint_id": 36677, "eprint_status": "archive", "datestamp": "2023-08-22 04:05:55", "lastmod": "2024-02-02 21:06:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "D\u00e9sert-J-M", "name": { "family": "D\u00e9sert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Madhusudhan-N", "name": { "family": "Madhusudhan", "given": "Nikku" }, "orcid": "0000-0002-4869-000X" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Fressin-F", "name": { "family": "Fressin", "given": "Fran\u00e7ois" } }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Borucki-W-J", "name": { "family": "Borucki", "given": "William J." } }, { "id": "Brown-T-M", "name": { "family": "Brown", "given": "Timothy M." }, "orcid": "0000-0002-1793-9968" }, { "id": "Caldwell-D-A", "name": { "family": "Caldwell", "given": "Douglas" }, "orcid": "0000-0003-1963-9616" }, { "id": "Ford-E-B", "name": { "family": "Ford", "given": "Eric B." }, "orcid": "0000-0001-6545-639X" }, { "id": "Gilliland-R-L", "name": { "family": "Gilliland", "given": "Ronald L." }, "orcid": "0000-0002-1554-5578" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Marcy-G-W", "name": { "family": "Marcy", "given": "Geoffrey W." }, "orcid": "0000-0002-2909-0113" }, { "id": "Seager-S", "name": { "family": "Seager", "given": "Sara" }, "orcid": "0000-0002-6892-6948" } ] }, "title": "The Atmospheres of the Hot-Jupiters Kepler-5b and Kepler-6b Observed during Occultations with Warm-Spitzer and Kepler", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; planetary systems; techniques: photometric", "note": "\u00a9 2011 American Astronomical Society. \n\nReceived 2011 February 3; accepted 2011 October 8; published 2011 November 1. \n\nWe would like to thank Jessie Christiansen, Brice-Olivier Demory, and Pavel Machaleck for discussions about Kepler photometry, light curves analysis, and interpretation. Thank you to the Spitzer staff at IPAC and in particular to Nancy Silbermann for scheduling the observations of this large program. We would like to thank Jacob Bean for a variety of useful discussions. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This work is also based on observations made with Kepler which was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. The authors would like to thank the many people who generously gave so much their time to make this Mission a success. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.\n\nPublished - 0067-0049_197_1_11.pdf
Submitted - 1102.0555.pdf
", "abstract": "This paper reports the detection and the measurements of occultations of the two transiting hot giant exoplanets Kepler-5b and Kepler-6b by their parent stars. The observations are obtained in the near-infrared with Warm-Spitzer Space Telescope and at optical wavelengths by combining more than a year of Kepler photometry. The investigation consists of constraining the eccentricities of these systems and of obtaining broadband emergent photometric data for individual planets. For both targets, the occultations are detected at the 3\u03c3 level at each wavelength with mid-occultation times consistent with circular orbits. The brightness temperatures of these planets are deduced from the infrared observations and reach T_(Spitzer) = 1930 \u00b1 100 K and T_(Spitzer) = 1660 \u00b1 120 K for Kepler-5b and Kepler-6b, respectively. We measure optical geometric albedos A_g in the Kepler bandpass and find A_g = 0.12 \u00b1 0.04 for Kepler-5b and A_g = 0.11 \u00b1 0.04 for Kepler-6b, leading to upper an limit for the Bond albedo of A_B \u2264 0.17 in both cases. The observations for both planets are best described by models for which most of the incident energy is redistributed on the dayside, with only less than 10% of the absorbed stellar flux redistributed to the nightside of these planets.", "date": "2011-11", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "197", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 11", "id_number": "CaltechAUTHORS:20130130-081112844", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130130-081112844", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "corp_creators": { "items": [ "Kepler Science Team" ] }, "doi": "10.1088/0067-0049/197/1/11", "primary_object": { "basename": "0067-0049_197_1_11.pdf", "url": "https://authors.library.caltech.edu/records/mrhw2-n7610/files/0067-0049_197_1_11.pdf" }, "related_objects": [ { "basename": "1102.0555.pdf", "url": "https://authors.library.caltech.edu/records/mrhw2-n7610/files/1102.0555.pdf" } ], "resource_type": "article", "pub_year": "2011", "author_list": "D\u00e9sert, Jean-Michel; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/xw0d8-n8x44", "eprint_id": 36669, "eprint_status": "archive", "datestamp": "2023-08-22 03:09:10", "lastmod": "2024-02-02 21:06:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Madhusudhan-N", "name": { "family": "Madhusudhan", "given": "Nikku" }, "orcid": "0000-0002-4869-000X" }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Christiansen-J-L", "name": { "family": "Christiansen", "given": "Jessie L." }, "orcid": "0000-0002-8035-4778" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "D\u00e9sert-J-M", "name": { "family": "D\u00e9sert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Henry-G-W", "name": { "family": "Henry", "given": "Gregory W." }, "orcid": "0000-0003-4155-8513" }, { "id": "Homeier-D", "name": { "family": "Homeier", "given": "Derek" } }, { "id": "Langton-J", "name": { "family": "Langton", "given": "Jonathan" } }, { "id": "Laughlin-G-P", "name": { "family": "Laughlin", "given": "Gregory" }, "orcid": "0000-0002-3253-2621" }, { "id": "Seager-S", "name": { "family": "Seager", "given": "Sara" }, "orcid": "0000-0002-6892-6948" } ] }, "title": "A Spitzer Transmission Spectrum for the Exoplanet GJ 436b, Evidence for Stellar Variability, and Constraints on Dayside Flux Variations", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing; planetary systems; stars: activity; techniques: photometric", "note": "\u00a9 2011 American Astronomical Society. \n\nReceived 2011 February 14; accepted 2011 April 13; published 2011 June 10. \n\nWe thank the anonymous referee for a very thoughtful report, as well as Jonathan Fortney, Megan Shabram, and Nikole Lewis for helpful discussions on the implications of our data for their published models of GJ 436b.We are also grateful to Eric Gaidos for his commentary on the nature of activity on M dwarfs, and Josh Winn for helpful discussions on spin-orbit alignment for GJ 436b. We also thank Howard Isaacson for supplying the SHK values for our activity study and acknowledge the Keck observers who obtained the HIRES spectra used for these measurements, including Andrew Howard, John Johnson, Debra Fischer, and Geoff Marcy. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. H.A.K. was supported by a fellowship from the Miller Institute for Basic Research in Science. E.A. was supported in part by the National Science Foundation under CAREER Grant No. 0645416.\n\nPublished - 0004-637X_735_1_27.pdf
Accepted Version - 1104.2901.pdf
", "abstract": "In this paper, we describe a uniform analysis of eight transits and eleven secondary eclipses of the extrasolar planet GJ 436b obtained in the 3.6, 4.5, and 8.0 \u03bcm bands using the IRAC instrument on the Spitzer Space Telescope between UT 2007 June 29 and UT 2009 February 4. We find that the best-fit transit depths for visits in the same bandpass can vary by as much as 8% of the total (4.7\u03c3 significance) from one epoch to the next. Although we cannot entirely rule out residual detector effects or a time-varying, high-altitude cloud layer in the planet's atmosphere as the cause of these variations, we consider the occultation of active regions on the star in a subset of the transit observations to be the most likely explanation. We find that for the deepest 3.6 \u03bcm transit the in-transit data have a higher standard deviation than the out-of-transit data, as would be expected if the planet occulted a star spot. We also compare all published transit observations for this object and find that transits observed in the infrared typically have smaller timing offsets than those observed in visible light. In this case, the three deepest Spitzer transits are all measured within a period of five days, consistent with a single epoch of increased stellar activity. We reconcile the presence of magnetically active regions with the lack of significant visible or infrared flux variations from the star by proposing that the star's spin axis is tilted with respect to our line of sight and that the planet's orbit is therefore likely to be misaligned. In contrast to the results reported by Beaulieu et al., we find no convincing evidence for methane absorption in the planet's transmission spectrum. If we exclude the transits that we believe to be most affected by stellar activity, we find that we prefer models with enhanced CO and reduced methane, consistent with GJ 436b's dayside composition from Stevenson et al. It is also possible that all transits are significantly affected by this activity, in which case it may not be feasible to characterize the planet's transmission spectrum using broadband photometry obtained over multiple epochs. These observations serve to illustrate the challenges associated with transmission spectroscopy of planets orbiting late-type stars; we expect that other systems, such as GJ 1214, may display comparably variable transit depths. We compare the limb-darkening coefficients predicted by PHOENIX and ATLAS stellar atmosphere models and discuss the effect that these coefficients have on the measured planet-star radius ratios given GJ 436b's near-grazing transit geometry. Our measured 8 \u03bcm secondary eclipse depths are consistent with a constant value, and we place a 1\u03c3 upper limit of 17% on changes in the planet's dayside flux in this band. These results are consistent with predictions from general circulation models for this planet, which find that the planet's dayside flux varies by a few percent or less in the 8 \u03bcm band. Averaging over the eleven visits gives us an improved estimate of 0.0452% \u00b1 0.0027% for the secondary eclipse depth; we also examine residuals from the eclipse ingress and egress and place an upper limit on deviations caused by a non-uniform surface brightness for GJ 436b. We combine timing information from our observations with previously published data to produce a refined orbital ephemeris and determine that the best-fit transit and eclipse times are consistent with a constant orbital period. We find that the secondary eclipse occurs at a phase of 0.58672 \u00b1 0.00017, corresponding to ecos (\u03c9) = 0.13754 \u00b1 0.00027, where e is the planet's orbital eccentricity and \u03c9 is the longitude of pericenter. We also present improved estimates for other system parameters, including the orbital inclination, a/R_\u2605, and the planet-star radius ratio.", "date": "2011-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "735", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 27", "id_number": "CaltechAUTHORS:20130129-151828269", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-151828269", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "NSF", "grant_number": "AST-0645416" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/735/1/27", "primary_object": { "basename": "1104.2901.pdf", "url": "https://authors.library.caltech.edu/records/xw0d8-n8x44/files/1104.2901.pdf" }, "related_objects": [ { "basename": "0004-637X_735_1_27.pdf", "url": "https://authors.library.caltech.edu/records/xw0d8-n8x44/files/0004-637X_735_1_27.pdf" } ], "resource_type": "article", "pub_year": "2011", "author_list": "Knutson, Heather A.; Madhusudhan, Nikku; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zaz72-sb625", "eprint_id": 36667, "eprint_status": "archive", "datestamp": "2023-08-22 01:52:04", "lastmod": "2024-02-02 21:06:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Beerer-I-M", "name": { "family": "Beerer", "given": "Ingrid M." } }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "D\u00e9sert-J-M", "name": { "family": "Desert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Langton-J", "name": { "family": "Langton", "given": "Jonathan" } }, { "id": "Laughlin-G-P", "name": { "family": "Laughlin", "given": "Gregory" }, "orcid": "0000-0002-3253-2621" }, { "id": "Lewis-N-K", "name": { "family": "Lewis", "given": "Nikole K." }, "orcid": "0000-0002-8507-1304" }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } } ] }, "title": "Secondary Eclipse Photometry of WASP-4b with Warm Spitzer", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; planetary systems; stars: individual (WASP-4b); techniques: photometric", "note": "\u00a9 2011 American Astronomical Society. \n\nReceived 2010 July 22; accepted 2010 November 8; published 2010 December 28. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Support for this work was provided by NASA. Heather A. Knutson is supported by a fellowship from the Miller Institute for Basic Research Science. Eric Agol acknowledges the support of NSF CAREER grant No. 0645416.\n\nPublished - 0004-637X_727_1_23.pdf
Accepted Version - 1011.4066.pdf
", "abstract": "We present photometry of the giant extrasolar planet WASP-4b at 3.6 and 4.5 \u03bcm taken with the Infrared Array Camera on board the Spitzer Space Telescope as part of Spitzer's extended warm mission. We find secondary eclipse depths of 0.319% \u00b1 0.031% and 0.343% \u00b1 0.027% for the 3.6 and 4.5 \u03bcm bands, respectively, and show model emission spectra and pressure-temperature profiles for the planetary atmosphere. These eclipse depths are well fit by model emission spectra with water and other molecules in absorption, similar to those used for TrES-3 and HD 189733b. Depending on our choice of model, these results indicate that this planet has either a weak dayside temperature inversion or no inversion at all. The absence of a strong thermal inversion on this highly irradiated planet is contrary to the idea that highly irradiated planets are expected to have inversions, perhaps due the presence of an unknown absorber in the upper atmosphere. This result might be explained by the modestly enhanced activity level of WASP-4b's G7V host star, which could increase the amount of UV flux received by the planet, therefore reducing the abundance of the unknown stratospheric absorber in the planetary atmosphere as suggested in Knutson et al. We also find no evidence for an offset in the timing of the secondary eclipse and place a 2\u03c3 upper limit on |ecos \u03c9| of 0.0024, which constrains the range of tidal heating models that could explain this planet's inflated radius.", "date": "2011-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "727", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 23", "id_number": "CaltechAUTHORS:20130129-145910562", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-145910562", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "NSF", "grant_number": "AST-0645416" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/727/1/23", "primary_object": { "basename": "0004-637X_727_1_23.pdf", "url": "https://authors.library.caltech.edu/records/zaz72-sb625/files/0004-637X_727_1_23.pdf" }, "related_objects": [ { "basename": "1011.4066.pdf", "url": "https://authors.library.caltech.edu/records/zaz72-sb625/files/1011.4066.pdf" } ], "resource_type": "article", "pub_year": "2011", "author_list": "Beerer, Ingrid M.; Knutson, Heather A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ksjer-da992", "eprint_id": 36666, "eprint_status": "archive", "datestamp": "2023-08-22 01:50:27", "lastmod": "2024-02-02 21:06:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather" }, "orcid": "0000-0002-5375-4725" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "D\u00e9sert-J-M", "name": { "family": "Desert", "given": "Jean-Michel" }, "orcid": "0000-0002-0875-8401" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Laughlin-G-P", "name": { "family": "Laughlin", "given": "Gregory" }, "orcid": "0000-0002-3253-2621" }, { "id": "Langton-J", "name": { "family": "Langton", "given": "Jonathan" } }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } }, { "id": "Lewis-N-K", "name": { "family": "Lewis", "given": "Nikole K." }, "orcid": "0000-0002-8507-1304" } ] }, "title": "Warm Spitzer Photometry of the Transiting Exoplanets CoRoT-1 and CoRoT-2 at Secondary Eclipse", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; planetary systems; techniques: photometric", "note": "\u00a9 2011 American Astronomical Society. Received 2010 May 4; accepted 2010 November 2; published 2010 December 20. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA. H.K. is supported by a fellowship from the Miller Institute for Basic Research in Science. E.A. acknowledges support under NSF CAREER grant no. 0645416. A.B. was supported by NASA grant NNX07AG80G and under JPL/Spitzer Agreements 1328092, 1348668, and 1312647. He is also pleased to note that part of this work was performed while in residence at the Kavli Institute for Theoretical Physics, funded by the NSF through grant no. PHY05-51164. We thank Dr. Rory Barnes for informative conversations regarding the tidal evolution of CoRoT-2, and an anonymous referee for a very thorough review that improved this paper significantly. \nFacilities: Spitzer\n\nPublished - 0004-637X_726_2_95.pdf
", "abstract": "We measure secondary eclipses of the hot giant exoplanets CoRoT-1 at 3.6 and 4.5 \u03bcm, and CoRoT-2 at 3.6 \u03bcm, both using Warm Spitzer. We find that the Warm Spitzer mission is working very well for exoplanet science. For consistency of our analysis we also re-analyze archival cryogenic Spitzer data for secondary eclipses of CoRoT-2 at 4.5 and 8 \u03bcm. We compare the total data for both planets, including optical eclipse measurements by the CoRoT mission, and ground-based eclipse measurements at 2 \u03bcm, to existing models. Both planets exhibit stronger eclipses at 4.5 than at 3.6 \u03bcm, which is often indicative of an atmospheric temperature inversion. The spectrum of CoRoT-1 is best reproduced by a 2460 K blackbody, due either to a high altitude layer that strongly absorbs stellar irradiance, or an isothermal region in the planetary atmosphere. The spectrum of CoRoT-2 is unusual because the 8 \u03bcm contrast is anomalously low. Non-inverted atmospheres could potentially produce the CoRoT-2 spectrum if the planet exhibits line emission from CO at 4.5 \u03bcm, caused by tidal-induced mass loss. However, the viability of that hypothesis is questionable because the emitting region cannot be more than about 30% larger than the planet's transit radius, based on the ingress and egress times at eclipse. An alternative possibility to account for the spectrum of CoRoT-2 is an additional opacity source that acts strongly at wavelengths less than 5 \u03bcm, heating the upper atmosphere while allowing the deeper atmosphere seen at 8 \u03bcm to remain cooler. We obtain a similar result as Gillon et al. for the phase of the secondary eclipse of CoRoT-2, implying an eccentric orbit with e cos(\u03c9) = \u20130.0030 \u00b1 0.0004.", "date": "2011-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "726", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 95", "id_number": "CaltechAUTHORS:20130129-144355630", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-144355630", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "NSF", "grant_number": "AST-0645416" }, { "agency": "NASA", "grant_number": "NNX07AG80G" }, { "agency": "JPL/Spitzer", "grant_number": "1328092" }, { "agency": "JPL/Spitzer", "grant_number": "1348668" }, { "agency": "JPL/Spitzer", "grant_number": "1312647" }, { "agency": "NSF", "grant_number": "PHY05-51164" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/726/2/95", "primary_object": { "basename": "0004-637X_726_2_95.pdf", "url": "https://authors.library.caltech.edu/records/ksjer-da992/files/0004-637X_726_2_95.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Deming, Drake; Knutson, Heather; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/a0r7b-azd91", "eprint_id": 36985, "eprint_status": "archive", "datestamp": "2023-08-22 01:18:15", "lastmod": "2024-02-02 21:07:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ballard-S", "name": { "family": "Ballard", "given": "Sarah" }, "orcid": "0000-0002-3247-5081" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Christiansen-J-L", "name": { "family": "Christiansen", "given": "Jessie L." }, "orcid": "0000-0002-8035-4778" }, { "id": "Holman-M-J", "name": { "family": "Holman", "given": "Matthew J." }, "orcid": "0000-0002-1139-4880" }, { "id": "Fabrycky-D-C", "name": { "family": "Fabrycky", "given": "Daniel" }, "orcid": "0000-0003-3750-0183" }, { "id": "Seager-S", "name": { "family": "Seager", "given": "Sara" }, "orcid": "0000-0002-6892-6948" }, { "id": "A'Hearn-M-F", "name": { "family": "A'Hearn", "given": "Michael F." } } ] }, "title": "A Search for a Sub-Earth-Sized Companion to GJ 436 and a Novel Method to Calibrate Warm Spitzer IRAC Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "Extrasolar Planets", "note": "\u00a9 2010 The Astronomical Society of the Pacific. \n\nReceived 2010 August 12; accepted 2010 September 3; published 2010 October 1.\n\nAccepted Version - 1009.0755.pdf
", "abstract": "We discovered evidence for a possible additional 0.75 R_\u2295 transiting planet in the NASA EPOXI observations of the known M dwarf exoplanetary system GJ 436. Based on an ephemeris determined from the EPOXI data, we predicted a transit event in an extant Spitzer Space Telescope 8 \u03bcm data set of this star. Our subsequent analysis of those Spitzer data confirmed the signal of the predicted depth and at the predicted time, but we found that the transit depth was dependent on the aperture used to perform the photometry. Based on these suggestive findings, we gathered new warm Spitzer observations of GJ 436 at 4.5 \u03bcm spanning a time of transit predicted from the EPOXI and Spitzer 8 \u03bcm candidate events. The 4.5 \u03bcm data permit us to rule out a transit at high confidence, and we conclude that the earlier candidate transit signals resulted from correlated noise in the EPOXI and Spitzer 8 \u03bcm observations. In the course of this investigation, we developed a novel method for correcting the intrapixel sensitivity variations of the 3.6 and 4.5 \u03bcm channels of the Infrared Array Camera (IRAC) instrument. We demonstrate the sensitivity of warm Spitzer observations of M dwarfs to confirm sub-Earth-sized planets. Our analysis will inform similar work that will be undertaken to use warm Spitzer observations to confirm rocky planets discovered by the Kepler mission.", "date": "2010-11", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "122", "number": "897", "publisher": "Astronomical Society of the Pacific", "pagerange": "1341-1352", "id_number": "CaltechAUTHORS:20130219-133505285", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130219-133505285", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/657159", "primary_object": { "basename": "1009.0755.pdf", "url": "https://authors.library.caltech.edu/records/a0r7b-azd91/files/1009.0755.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Ballard, Sarah; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/e2cvr-cc476", "eprint_id": 36664, "eprint_status": "archive", "datestamp": "2023-08-19 04:02:33", "lastmod": "2024-02-02 21:06:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Steffen-J-H", "name": { "family": "Steffen", "given": "Jason H." } }, { "id": "Henry-G-W", "name": { "family": "Henry", "given": "Gregory W." }, "orcid": "0000-0003-4155-8513" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" } ] }, "title": "The Climate of HD 189733b from Fourteen Transits and Eclipses Measured by Spitzer", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems", "note": "\u00a9 2010 American Astronomical Society. \n\nReceived 2010 March 10; accepted 2010 July 25; published 2010 September 14. \n\nThis work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology under contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. E.A. acknowledges the hospitality of the Institute for Theory and Computation at the Harvard-Smithsonian Center for Astrophysics, the Michigan Center for Theoretical Physics, and the Kavli Institute for Theoretical Physics where portions of this work were completed. H.A.K. is supported by a fellowship from the Miller Institute for Basic Research in Science. This research was supported in part by the National Science Foundation under grant No. NSF PHY05-51164 and CAREER grant No. 0645416.\n\nPublished - 0004-637X_721_2_1861.pdf
Accepted Version - 1007.4378.pdf
", "abstract": "We present observations of six transits and six eclipses of the transiting planet system HD 189733 taken with the Spitzer Space Telescope's Infrared Array Camera (IRAC) at 8 \u03bcm, as well as a re-analysis of previously published data. We use several novel techniques in our data analysis, the most important of which is a new correction for the detector \"ramp\" variation with a double-exponential function, which performs better and is a better physical model for this detector variation. Our main scientific findings are (1) an upper limit on the variability of the dayside planet flux of 2.7% (68% confidence); (2) the most precise set of transit times measured for a transiting planet, with an average accuracy of 3 s; (3) a lack of transit-timing variations, excluding the presence of second planets in this system above 20% of the mass of Mars in low-order mean-motion resonance at 95% confidence; (4) a confirmation of the planet's phase variation, finding the night side is 64% as bright as the day side, as well as an upper limit on the nightside variability of 17% (68% confidence); (5) a better correction for stellar variability at 8 \u03bcm causing the phase function to peak 3.5 hr before secondary eclipse, confirming that the advection and radiation timescales are comparable at the 8 \u03bcm photosphere; (6) variation in the depth of transit, which possibly implies variations in the surface brightness of the portion of the star occulted by the planet, posing a fundamental limit on non-simultaneous multi-wavelength transit absorption measurements of planet atmospheres; (7) a measurement of the infrared limb darkening of the star, which is in good agreement with stellar atmosphere models; (8) an offset in the times of secondary eclipse of 69 s, which is mostly accounted for by a 31 s light-travel time delay and 33 s delay due to the shift of ingress and egress by the planet hot spot; this confirms that the phase variation is due to an offset hot spot on the planet; (9) a retraction of the claimed eccentricity of this system due to the offset of secondary eclipse, which is now just an upper limit; and (10) high-precision measurements of the parameters of this system. These results were enabled by the exquisite photometric precision of Spitzer IRAC; for repeat observations the scatter is less than 0.35 mmag over the 590 day timescale of our observations after decorrelating with detector parameters.", "date": "2010-10-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "721", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1861-1877", "id_number": "CaltechAUTHORS:20130129-140352262", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-140352262", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "NSF", "grant_number": "PHY05-51164" }, { "agency": "NSF", "grant_number": "AST-0645416" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/721/2/1861", "primary_object": { "basename": "0004-637X_721_2_1861.pdf", "url": "https://authors.library.caltech.edu/records/e2cvr-cc476/files/0004-637X_721_2_1861.pdf" }, "related_objects": [ { "basename": "1007.4378.pdf", "url": "https://authors.library.caltech.edu/records/e2cvr-cc476/files/1007.4378.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Agol, Eric; Cowan, Nicolas B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/rkzx5-vdb78", "eprint_id": 36222, "eprint_status": "archive", "datestamp": "2023-08-22 00:31:46", "lastmod": "2023-10-20 22:53:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Irwin-J", "name": { "family": "Irwin", "given": "Jonathan" } }, { "id": "Buchhave-L-A", "name": { "family": "Buchhave", "given": "Lars" }, "orcid": "0000-0003-1605-5666" }, { "id": "Berta-Z-K", "name": { "family": "Berta", "given": "Zachory K." } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Burke-C-J", "name": { "family": "Burke", "given": "Christopher J." } }, { "id": "Esquerdo-G-A", "name": { "family": "Esquerdo", "given": "Gilbert A." }, "orcid": "0000-0002-9789-5474" }, { "id": "Everett-M-E", "name": { "family": "Everett", "given": "Mark E." }, "orcid": "0000-0002-0885-7215" }, { "id": "Holman-M-J", "name": { "family": "Holman", "given": "Matthew J." }, "orcid": "0000-0002-1139-4880" }, { "id": "Nutzman-P", "name": { "family": "Nutzman", "given": "Philip" } }, { "id": "Berlind-P", "name": { "family": "Berlind", "given": "Perry" } }, { "id": "Calkins-M-L", "name": { "family": "Calkins", "given": "Michael L." }, "orcid": "0000-0002-2830-5661" }, { "id": "Falco-E-E", "name": { "family": "Falco", "given": "Emilio E." } }, { "id": "Winn-J-N", "name": { "family": "Winn", "given": "Joshua N." }, "orcid": "0000-0002-4265-047X" }, { "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "orcid": "0000-0001-9808-7172" }, { "id": "Gazak-J-Z", "name": { "family": "Gazak", "given": "J. Zachary" } } ] }, "title": "NLTT 41135: A Field M Dwarf + Brown Dwarf Eclipsing Binary in a Triple System, Discovered by the MEarth Observatory", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing; brown dwarfs; stars: individual (NLTT 41135); stars: low-mass", "note": "\u00a9 2010 American Astronomical Society. Received 2010 February 23; accepted 2010 June 8; published 2010 July 14. The MEarth team gratefully acknowledges funding from\nthe David and Lucile Packard Fellowship for Science and\nEngineering (awarded to DC). This material is based upon\nwork supported by the National Science Foundation under grant number AST-0807690. L.B. and D.W.L. acknowledge partial support from the NASA Kepler mission under cooperative agreement NCC2-1390. J.A.J. thanks the NSF Astronomy and Astrophysics Postdoctoral Fellowship program for support in the years leading to the completion of this work, and acknowledges support from NSF grant AST-0702821. We thank Isabelle Baraffe for providing NextGen and cond models in the z band, Daniel Fabrycky for helpful discussions regarding dynamics, and Timothy Brown and the rest of the team at the Las Cumbres Observatory Global Telescope for their efforts in trying to obtain a resolved light curve of the system. The MEarth team is greatly indebted to the staff at the Fred Lawrence Whipple\nObservatory for their efforts in construction and maintenance of the facility, and would like to explicitly thank Wayne Peters, Ted Groner, Karen Erdman-Myres, Grace Alegria, Rodger Harris, Bob Hutchins,Dave Martina, Dennis Jankovsky, and Tom Welsh for their support. Finally, we thank the referee for a thorough and helpful report, which has substantially improved the manuscript. This research is based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by\nDenmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This research has made extensive use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF, NASA's Astrophysics Data System (ADS), and the SIMBAD database, operated at CDS, Strasbourg, France. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with\nthe permission of these institutions. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval\nObservatory, and the University of Washington. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna\nKea has always had within the indigenous Hawaiian community.\nWe are most fortunate to have the opportunity to conduct\nobservations from this mountain. \nFacilities: UH:2.2m (OPTIC), FLWO:1.2m (KeplerCam),\nFLWO:1.5m (TRES), NOT (FIES)\n\nPublished - 0004-637X_718_2_1353.pdf
", "abstract": "We report the discovery of an eclipsing companion to NLTT 41135, a nearby M5 dwarf that was already known to have a wider, slightly more massive common proper motion companion, NLTT 41136, at 2\".4 separation. Analysis of combined-light and RV curves of the system indicates that NLTT 41135B is a (31-34) \u00b1 3M_(Jup) brown dwarf (where the range depends on the unknown metallicity of the host star) on a circular orbit. The visual M dwarf pair appears to be physically bound, so the system forms a hierarchical triple, with masses approximately in the ratio 8:6:1. The eclipses are grazing, preventing an unambiguous measurement of the secondary radius, but follow-up observations of the secondary eclipse (e.g., with the James Webb Space Telescope) could permit measurements of the surface brightness ratio between the two objects, and thus place constraints on models of brown dwarfs.", "date": "2010-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "718", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1353-1366", "id_number": "CaltechAUTHORS:20130108-072919967", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130108-072919967", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "David and Lucile Packard Foundation" }, { "agency": "NSF", "grant_number": "AST-0807690" }, { "agency": "NASA", "grant_number": "NCC2-1390" }, { "agency": "NSF Astronomy and Astrophysics Fellowship", "grant_number": "AST-0702821" }, { "agency": "NASA" }, { "agency": "NSF" }, { "agency": "NASA's Astrophysics Data System (ADS)" }, { "agency": "SIMBAD database" }, { "agency": "NASA", "grant_number": "NAG W-2166" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" }, { "agency": "Space Telescope Science Institute" } ] }, "doi": "10.1088/0004-637X/718/2/1353", "primary_object": { "basename": "0004-637X_718_2_1353.pdf", "url": "https://authors.library.caltech.edu/records/rkzx5-vdb78/files/0004-637X_718_2_1353.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Irwin, Jonathan; Buchhave, Lars; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/wgxh4-n3m40", "eprint_id": 36656, "eprint_status": "archive", "datestamp": "2023-08-21 23:33:40", "lastmod": "2024-02-02 21:06:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fressin-F", "name": { "family": "Fressin", "given": "Francois" } }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "Georgi" } }, { "id": "Spiegel-D-S", "name": { "family": "Spiegel", "given": "David" } } ] }, "title": "The Broadband Infrared Emission Spectrum of the Exoplanet TrES-3", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; infrared: stars; planetary systems; stars: individual (TrES-3); techniques: photometric", "note": "Copyright is not claimed for this article. \n\nReceived 2009 September 24; accepted 2010 January 11; published 2010 February 10. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA.\n\nPublished - 0004-637X_711_1_374.pdf
Accepted Version - 0909.5221.pdf
", "abstract": "We use the Spitzer Space Telescope to estimate the dayside thermal emission of the exoplanet TrES-3 integrated in the 3.6, 4.5, 5.8, and 8.0 \u03bcm bandpasses of the Infrared Array Camera (IRAC) instrument. We observe two secondary eclipses and find relative eclipse depths of 0.00346 \u00b1 0.00035, 0.00372 \u00b1 0.00054, 0.00449 \u00b1 0.00097, and 0.00475 \u00b1 0.00046, respectively, in the four IRAC bandpasses. We combine our results with the earlier K-band measurement of De Mooij et al., and compare them with models of the planetary emission. We find that the planet does not require the presence of an inversion layer in the high atmosphere. This is the first very strongly irradiated planet that does not have a temperature inversion, which indicates that stellar or planetary characteristics other than temperature have an important impact on temperature inversion. De Mooij & Snellen also detected a possible slight offset in the timing of the secondary eclipse in the K band. However, based on our four Spitzer channels, we place a 3\u03c3 upper limit of |ecos(\u03c9)| < 0.0056, where e is the planet's orbital eccentricity and \u03c9 is the longitude of the periastron. This result strongly indicates that the orbit is circular, as expected from tidal circularization theory.", "date": "2010-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "711", "number": "1", "publisher": "American Astronomical Society", "pagerange": "374-379", "id_number": "CaltechAUTHORS:20130129-132702403", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-132702403", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/711/1/374", "primary_object": { "basename": "0004-637X_711_1_374.pdf", "url": "https://authors.library.caltech.edu/records/wgxh4-n3m40/files/0004-637X_711_1_374.pdf" }, "related_objects": [ { "basename": "0909.5221.pdf", "url": "https://authors.library.caltech.edu/records/wgxh4-n3m40/files/0909.5221.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Fressin, Francois; Knutson, Heather A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/x29k6-hqf57", "eprint_id": 17603, "eprint_status": "archive", "datestamp": "2023-08-21 23:24:47", "lastmod": "2024-02-02 21:08:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Harrington-J", "name": { "family": "Harrington", "given": "Joseph" } }, { "id": "Madhusudhan-N", "name": { "family": "Madhusudhan", "given": "N." }, "orcid": "0000-0002-4869-000X" }, { "id": "Seager-S", "name": { "family": "Seager", "given": "Sara" }, "orcid": "0000-0002-6892-6948" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" } ] }, "title": "Detection of Planetary Emission from the Exoplanet Tres-2 Using Spitzer/IRAC", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; infrared: stars; planetary systems; stars: individual (GSC 03549-02811); techniques: photometric", "note": "\u00a9 2010 American Astronomical Society. \n\nPrint publication: Issue 2 (2010 February 20); received 2009 September 16; accepted for publication 2010 January 2; published 2010 February 1. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration (NASA). This research was supported in part by NASA under grant NNG05GJ29G (issued through the Origins of Solar Systems Program) and also by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center (administered by Oak Ridge Associated Universities through a contract with NASA). \n\nFacilities: Spitzer (IRAC)\n\nPublished - ODonovan2010p7149Astrophys_J.pdf
Accepted Version - 0909.3073.pdf
", "abstract": "We present here the results of our observations of TrES-2 using the Infrared Array Camera on Spitzer. We monitored this transiting system during two secondary eclipses, when the planetary emission is blocked by the star. The resulting decrease in flux is 0.127% \u00b1 0.021%, 0.230% \u00b1 0.024%, 0.199% \u00b1 0.054%, and 0.359% \u00b1 0.060% at 3.6 \u03bcm, 4.5 \u03bcm, 5.8 \u03bcm, and 8.0 \u03bcm, respectively. We show that three of these flux contrasts are well fit by a blackbody spectrum with T_(eff) = 1500 K, as well as by a more detailed model spectrum of a planetary atmosphere. The observed planet-to-star flux ratios in all four IRAC channels can be explained by models with and without a thermal inversion in the atmosphere of TrES-2, although with different atmospheric chemistry. Based on the assumption of thermochemical equilibrium, the chemical composition of the inversion model seems more plausible, making it a more favorable scenario. TrES-2 also falls in the category of highly irradiated planets which have been theoretically predicted to exhibit thermal inversions. However, more observations at infrared and visible wavelengths would be needed to confirm a thermal inversion in this system. Furthermore, we find that the times of the secondary eclipses are consistent with previously published times of transit and the expectation from a circular orbit. This implies that TrES-2 most likely has a circular orbit, and thus does not obtain additional thermal energy from tidal dissipation of a non-zero orbital eccentricity, a proposed explanation for the large radius of this planet.", "date": "2010-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "710", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1551-1556", "id_number": "CaltechAUTHORS:20100225-165652168", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100225-165652168", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG05GJ29G" }, { "agency": "NASA Postdoctoral Program" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/710/2/1551", "primary_object": { "basename": "0909.3073.pdf", "url": "https://authors.library.caltech.edu/records/x29k6-hqf57/files/0909.3073.pdf" }, "related_objects": [ { "basename": "ODonovan2010p7149Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/x29k6-hqf57/files/ODonovan2010p7149Astrophys_J.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "O'Donovan, Francis T.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/py32v-p0192", "eprint_id": 36654, "eprint_status": "archive", "datestamp": "2023-08-21 22:23:09", "lastmod": "2024-02-02 21:06:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Henry-G-W", "name": { "family": "Henry", "given": "Gregory W." }, "orcid": "0000-0003-4155-8513" } ] }, "title": "The 8 \u03bcm Phase Variation of the Hot Saturn HD 149026b", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; planetary systems; stars: individual (HD 149026b); techniques: photometric", "note": "\u00a9 2009 American Astronomical Society. \n\nReceived 2009 May 22; accepted 2009 August 6; published 2009 September 1. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. H.A.K. was supported by a National Science Foundation Graduate Research Fellowship.\n\nPublished - 0004-637X_703_1_769.pdf
Accepted Version - 0908.1977.pdf
", "abstract": "We monitor the star HD 149026 and its Saturn-mass planet at 8.0 \u03bcm over slightly more than half an orbit using the Infrared Array Camera on the Spitzer Space Telescope. We find an increase of 0.0227% \u00b1 0.0066% (3.4\u03c3 significance) in the combined planet-star flux during this interval. The minimum flux from the planet is 45% \u00b1 19% of the maximum planet flux, corresponding to a difference in brightness temperature of 480 \u00b1 140 K between the two hemispheres. We derive a new secondary eclipse depth of 0.0411% \u00b1 0.0076% in this band, corresponding to a dayside brightness temperature of 1440 \u00b1 150 K. Our new secondary eclipse depth is half that of a previous measurement (3.0\u03c3 difference) in this same bandpass by Harrrington et al. We re-fit the Harrrington et al. data and obtain a comparably good fit with a smaller eclipse depth that is consistent with our new value. In contrast to earlier claims, our new eclipse depth suggests that this planet's dayside emission spectrum is relatively cool, with an 8 \u03bcm brightness temperature that is less than the maximum planet-wide equilibrium temperature. We measure the interval between the transit and secondary eclipse and find that that the secondary eclipse occurs 20.9^(+7.2)_(\u20136.5) minutes earlier (2.9\u03c3) than predicted for a circular orbit, a marginally significant result. This corresponds to ecos(\u03c9) = \u20130.0079^(+0.0027)_(\u20130.0025), where e is the planet's orbital eccentricity and \u03c9 is the argument of pericenter.", "date": "2009-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "703", "number": "1", "publisher": "American Astronomical Society", "pagerange": "769-784", "id_number": "CaltechAUTHORS:20130129-130607171", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-130607171", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF Graduate Research Fellowship" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/703/1/769", "primary_object": { "basename": "0004-637X_703_1_769.pdf", "url": "https://authors.library.caltech.edu/records/py32v-p0192/files/0004-637X_703_1_769.pdf" }, "related_objects": [ { "basename": "0908.1977.pdf", "url": "https://authors.library.caltech.edu/records/py32v-p0192/files/0908.1977.pdf" } ], "resource_type": "article", "pub_year": "2009", "author_list": "Knutson, Heather A.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/95mgg-24t04", "eprint_id": 95507, "eprint_status": "archive", "datestamp": "2023-08-22 00:37:19", "lastmod": "2024-02-02 21:05:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Lian-Yuan", "name": { "family": "Lian", "given": "Yuan" } }, { "id": "Marley-M-S", "name": { "family": "Marley", "given": "Mark S." }, "orcid": "0000-0002-5251-2943" }, { "id": "Freedman-R-S", "name": { "family": "Freedman", "given": "Richard S." } }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" } ] }, "title": "Atmospheric circulation of hot Jupiters: Coupled radiative-dynamical general circulation model simulations of HD 189733b and HD 209458b", "ispublished": "pub", "full_text_status": "public", "keywords": "atmospheric effects \u2013 methods: numerical \u2013 planets and satellites: general \u2013 planets and satellites: individual (HD 209458b, HD 189733b)", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2008 September 7; accepted 2009 May 4; published 2009 June 12. \n\nThis research was supported by NASA Origins grant NNX08AF27G and Planetary Atmospheres grants NNX07AF35G and NNG06GF28G to A.P.S.\n\nPublished - Showman_2009_ApJ_699_564.pdf
Accepted Version - 0809.2089.pdf
", "abstract": "We present global, three-dimensional numerical simulations of HD 189733b and HD 209458b that couple the atmospheric dynamics to a realistic representation of nongray cloud-free radiative transfer. The model, which we call the Substellar and Planetary Atmospheric Radiation and Circulation model, adopts the MITgcm for the dynamics and uses the radiative model of McKay, Marley, Fortney, and collaborators for the radiation. Like earlier work with simplified forcing, our simulations develop a broad eastward equatorial jet, mean westward flow at higher latitudes, and substantial flow over the poles at low pressure. For HD 189733b, our simulations without TiO and VO opacity can explain the broad features of the observed 8 and 24 \u03bcm light curves, including the modest day-night flux variation and the fact that the planet/star flux ratio peaks before the secondary eclipse. Our simulations also provide reasonable matches to the Spitzer secondary-eclipse depths at 4.5, 5.8, 8, 16, and 24 \u03bcm and the ground-based upper limit at 2.2 \u03bcm. However, we substantially underpredict the 3.6 \u03bcm secondary-eclipse depth, suggesting that our simulations are too cold in the 0.1-1 bar region. Predicted temporal variability in secondary-eclipse depths is ~1% at Spitzer bandpasses, consistent with recent observational upper limits at 8 \u03bcm. We also show that nonsynchronous rotation can significantly alter the jet structure. For HD 209458b, we include TiO and VO opacity; these simulations develop a hot (>2000 K) dayside stratosphere whose horizontal dimensions are small at depth but widen with altitude. Despite this stratosphere, we do not reproduce current Spitzer photometry of this planet. Light curves in Spitzer bandpasses show modest phase variation and satisfy the observational upper limit on day-night phase variation at 8 \u03bcm.", "date": "2009-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "699", "number": "1", "publisher": "American Astronomical Society", "pagerange": "564-584", "id_number": "CaltechAUTHORS:20190515-102317810", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190515-102317810", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX08AF27G" }, { "agency": "NASA", "grant_number": "NNX07AF35G" }, { "agency": "NASA", "grant_number": "NNG06GF28G" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637x/699/1/564", "primary_object": { "basename": "0809.2089.pdf", "url": "https://authors.library.caltech.edu/records/95mgg-24t04/files/0809.2089.pdf" }, "related_objects": [ { "basename": "Showman_2009_ApJ_699_564.pdf", "url": "https://authors.library.caltech.edu/records/95mgg-24t04/files/Showman_2009_ApJ_699_564.pdf" } ], "resource_type": "article", "pub_year": "2009", "author_list": "Showman, Adam P.; Fortney, Jonathan J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/r7dfp-nmq70", "eprint_id": 36653, "eprint_status": "archive", "datestamp": "2023-08-22 00:19:54", "lastmod": "2024-02-02 21:06:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nutzman-P", "name": { "family": "Nutzman", "given": "Philip" } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Winn-J-N", "name": { "family": "Winn", "given": "Joshua N." }, "orcid": "0000-0002-4265-047X" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Holman-M-J", "name": { "family": "Holman", "given": "Matthew J." }, "orcid": "0000-0002-1139-4880" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" } ] }, "title": "A Precise Estimate of the Radius of the Exoplanet HD 149026b from Spitzer Photometry", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems \u2013 techniques: photometric", "note": "\u00a9 2009 American Astronomical Society. \n\nReceived 2008 May 6; accepted 2008 October 20; published 2009 February 18. \n\nWe are grateful to F. van Leeuwen for providing parallax data for HD 149026, and to G. Takeda for discussions regarding the spectroscopic determination of stellar properties. We are especially grateful to G. Henry for sharing many seasons of photometric data. We would also like to thank an anonymous referee for specific and helpful recommendations. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.\n\nPublished - 0004-637X_692_1_229.pdf
Accepted Version - 0805.0777.pdf
", "abstract": "We present Spitzer 8 \u03bcm transit observations of the extrasolar planet HD 149026b. At this wavelength, transit light curves are weakly affected by stellar limb darkening, allowing for a simpler and more accurate determination of planetary parameters. We measure a planet\u2013star radius ratio of R_p/R_\u2605 = 0.05158 \u00b1 0.00077, and in combination with ground-based data and independent constraints on the stellar mass and radius, we derive an orbital inclination of i = 85.\u25e64^(+0.\u25e69)_(\u22120.\u25e68) and a planet radius of R_p = 0.755 \u00b1 0.040 R_J. These measurements further support models in which the planet is greatly enriched in heavy elements.", "date": "2009-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "692", "number": "1", "publisher": "American Astronomical Society", "pagerange": "229-235", "id_number": "CaltechAUTHORS:20130129-115304761", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-115304761", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/692/1/229", "primary_object": { "basename": "0004-637X_692_1_229.pdf", "url": "https://authors.library.caltech.edu/records/r7dfp-nmq70/files/0004-637X_692_1_229.pdf" }, "related_objects": [ { "basename": "0805.0777.pdf", "url": "https://authors.library.caltech.edu/records/r7dfp-nmq70/files/0805.0777.pdf" } ], "resource_type": "article", "pub_year": "2009", "author_list": "Nutzman, Philip; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/fzykh-sea34", "eprint_id": 15848, "eprint_status": "archive", "datestamp": "2023-08-21 20:46:14", "lastmod": "2023-10-19 17:18:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sozzetti-A", "name": { "family": "Sozzetti", "given": "Alessandro" } }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Winn-J-N", "name": { "family": "Winn", "given": "Joshua N." }, "orcid": "0000-0002-4265-047X" }, { "id": "Korzennik-S-G", "name": { "family": "Korzennik", "given": "Sylvain G." } }, { "id": "Holman-M-J", "name": { "family": "Holman", "given": "Matthew J." }, "orcid": "0000-0002-1139-4880" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Laird-J-B", "name": { "family": "Laird", "given": "John B." } }, { "id": "Fernandez-J", "name": { "family": "Fernandez", "given": "Jos\u00e9" } }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "Georgi" } }, { "id": "Dunham-E", "name": { "family": "Dunham", "given": "Edward" } }, { "id": "Everett-M-E", "name": { "family": "Everett", "given": "Mark E." }, "orcid": "0000-0002-0885-7215" }, { "id": "Esquerdo-G-A", "name": { "family": "Esquerdo", "given": "Gilbert A." }, "orcid": "0000-0002-9789-5474" }, { "id": "Rabus-M", "name": { "family": "Rabus", "given": "Markus" } }, { "id": "Belmonte-J-A", "name": { "family": "Belmonte", "given": "Juan A." } }, { "id": "Deeg-H-J", "name": { "family": "Deeg", "given": "Hans J." } }, { "id": "Brown-T-N", "name": { "family": "Brown", "given": "Timothy N." } }, { "id": "Hidas-M-G", "name": { "family": "Hidas", "given": "M\u00e1rton G." } }, { "id": "Baliber-N", "name": { "family": "Baliber", "given": "Nairn" } } ] }, "title": "A New Spectroscopic and Photometric Analysis of the Transiting Planet Systems TrES-3 and TrES-4", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: abundances; stars: fundamental parameters; stars: individual (TrES-3, TrES-4); planetary systems", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2008 August 31; accepted 2008 September 25; published 2009 February 2.\n\nAS gratefully acknowledges the Kepler mission for partial\nsupport under NASA Cooperative Agreement NCC 2-1390.\nG.T. acknowledges partial support for this work from NASA\nOrigins grant NNG04LG89G. D.C. is supported in part by\nNASA Origins grant NNG05GJ29G. F.T.O.D. acknowledges\npartial support for this work provided through the NASA Postdoctoral\nProgram at the Goddard Space Flight Center, administered\nby Oak Ridge Associated Universities through a contract\nwith NASA. J.B.L. gratefully acknowledges support from\nNSF grant AST-0307340. Some of the data presented herein\nwere obtained at the W. M. Keck Observatory, which is operated\nas a scientific partnership among the California Institute of\nTechnology, the University of California and the National Aeronautics\nand Space Administration. The Observatory was made\npossible by the generous financial support of the W. M. Keck\nFoundation. The authors wish to recognize and acknowledge\nthe very significant cultural role and reverence that the summit\nof Mauna Kea has always had within the indigenous Hawaiian\ncommunity. We are most fortunate to have the opportunity\nto conduct observations from this mountain. This research has\nmade use of NASA's Astrophysics Data System Abstract Service\nand of the SIMBAD database, operated at CDS, Strasbourg,\nFrance.\n\nPublished - Sozzetti2009p24010.10880004-637X69121145.pdf
", "abstract": "We report new spectroscopic and photometric observations of the parent stars of the recently discovered transiting planets TrES-3 and TrES-4. A detailed abundance analysis based on high-resolution spectra yields [Fe/H] = \u20130.19 \u00b1 0.08, T_(eff) = 5650 \u00b1 75 K, and log g = 4.4 \u00b1 0.1 for TrES-3, and [Fe/H] = +0.14 \u00b1 0.09, T_(eff) = 6200 \u00b1 75 K, and log g = 4.0 \u00b1 0.1 for TrES-4. The accuracy of the effective temperatures is supported by a number of independent consistency checks. The spectroscopic orbital solution for TrES-3 is improved with our new radial velocity measurements of that system, as are the light-curve parameters for both systems based on newly acquired photometry for TrES-3 and a reanalysis of existing photometry for TrES-4. We have redetermined the stellar parameters taking advantage of the strong constraint provided by the light curves in the form of the normalized separation a/R_* (related to the stellar density) in conjunction with our new temperatures and metallicities. The masses and radii we derive are M_* = 0.928^(+0.028)_(\u20130.048) M_\u2299, R_* = 0.829^(+0.015)_(\u20130.022) R_\u2299, and M_* = 1.404^(+0.066)_(\u20130.134) M_\u2299, R_* = 1.846^(+0.096)_(\u20130.087) R_\u2299 for TrES-3 and TrES-4, respectively. With these revised stellar parameters, we obtain improved values for the planetary masses and radii. We find M_p = 1.910^(+0.075)_(\u20130.080) M_(Jup), R_p = 1.336^(+0.031)_(\u20130.036) R_(Jup) for TrES-3, and M_p = 0.925 \u00b1 0.082 M_(Jup), R_p = 1.783^(+0.093)_(\u20130.086) R_(Jup) for TrES-4. We confirm TrES-4 as the planet with the largest radius among the currently known transiting hot Jupiters.", "date": "2009-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "691", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1145-1158", "id_number": "CaltechAUTHORS:20090915-085812152", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090915-085812152", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NCC 2-1390" }, { "agency": "NASA", "grant_number": "NNG04LG89G" }, { "agency": "NASA", "grant_number": "NNG05GJ29G" }, { "agency": "NSF", "grant_number": "AST-0307340" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "doi": "10.1088/0004-637X/691/2/1145", "primary_object": { "basename": "Sozzetti2009p24010.10880004-637X69121145.pdf", "url": "https://authors.library.caltech.edu/records/fzykh-sea34/files/Sozzetti2009p24010.10880004-637X69121145.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Sozzetti, Alessandro; Torres, Guillermo; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2wb2w-w1m62", "eprint_id": 37308, "eprint_status": "archive", "datestamp": "2023-08-22 00:19:21", "lastmod": "2024-02-02 21:07:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pont-F", "name": { "family": "Pont", "given": "F." }, "orcid": "0000-0003-0076-5444" }, { "id": "Gilliland-R-L", "name": { "family": "Gilliland", "given": "R. L." }, "orcid": "0000-0002-1554-5578" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "H." }, "orcid": "0000-0002-5375-4725" }, { "id": "Holman-M", "name": { "family": "Holman", "given": "M." } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "D." }, "orcid": "0000-0002-9003-484X" } ] }, "title": "Transit infrared spectroscopy of the hot Neptune around GJ 436 with the Hubble Space Telescope", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems", "note": "\u00a9 2008 The Authors. Journal compilation \u00a9 2008 RAS.\n\nAccepted 2008 October 29. Received 2008 October 29; in original form 2008 August 18.\n\nBased on observations with the NASA/ESA Hubble Space Telescope, obtained\nat the Space Telescope Science Institute, which is operated by AURA,\nInc., under NASA contract NAS 5-26555.\n\nThe authors wish to thank Eliza Miller-Ricci and Sara Seager for atmosphere models provided in advance of publication and insightful comments, Michel Mayor for support with the observing proposal, Daniel Fabrycky for helpful discussions about transit timing variations in the GJ 436 system and the anonymous referee for numerous helpful comments.\n\nPublished - MNRAS-2009-Pont-L6-L10.pdf
", "abstract": "The nearby transiting system GJ 436b offers a unique opportunity to probe the structure and atmosphere of an extrasolar 'hot Neptune'. In this Letter, we present the main results of observations covering two transit events with the Near Infrared Camera and Multi Object Spectrograph (NICMOS) camera on the Hubble Space Telescope (HST). The data consist in high-cadence time series of grism spectra covering the 1.1\u20131.9 \u00b5m spectral range. We find R_pl= 4.04 \u00b1 0.10 R_\u2295 and R_*= 0.446 \u00b1 0.011 R_\u2299 for the planet and star radius, confirming and improving earlier measurements with a ground-based photometry and a Spitzer light curve at 8 \u00b5m, as opposed to a much higher value obtained with the Fine Guidance Sensor on the HST. We measure no departure from strict periodicity in the transits to the level of \u223c7s. This strongly disfavours the proposed explanation of the orbital eccentricity of GJ 436b in terms of the perturbation by another close-by planet. We measure a flat transmission spectrum at the level of a few parts per 10 000 in flux, with no significant signal in the 1.4-\u00b5m water band to a level comparable to the maximum amplitude of the effect predicted by planetary atmosphere models.", "date": "2009-02-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "393", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "L6-L10", "id_number": "CaltechAUTHORS:20130305-114608529", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130305-114608529", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1111/j.1745-3933.2008.00582.x", "primary_object": { "basename": "MNRAS-2009-Pont-L6-L10.pdf", "url": "https://authors.library.caltech.edu/records/2wb2w-w1m62/files/MNRAS-2009-Pont-L6-L10.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Pont, F.; Gilliland, R. L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/wt2x9-a4979", "eprint_id": 36652, "eprint_status": "archive", "datestamp": "2023-08-22 14:15:36", "lastmod": "2024-02-02 21:06:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "Georgi" } } ] }, "title": "Detection of A Temperature Inversion in the Broadband Infrared Emission Spectrum of TrES-4", "ispublished": "pub", "full_text_status": "public", "keywords": "eclipses; planetary systems; stars: individual: (TrES-4); techniques: photometric", "note": "\u00a9 2009 American Astronomical Society. \n\nReceived 2008 August 1; accepted 2008 September 30; published 2009 January 19. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. H.A.K. was supported by a National Science Foundation Graduate Research Fellowship. A.B. acknowledges the support of NASA through grant NNX07AG80G and JPL/Spitzer Agreement no. 1328902 and through the NASA Astrobiology Institute under Cooperative Agreement no. CAN-02-OSS-02 issued through the Office of Space Science. A.B. would also like to acknowledge Laurent Ibgui for checking the model results. F.T.O'D. was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA.\n\nPublished - 0004-637X_691_1_866.pdf
Accepted Version - 0810.0021.pdf
", "abstract": "We estimate the strength of the bandpass-integrated thermal emission from the extrasolar planet TrES-4 at 3.6, 4.5, 5.8, and 8.0 \u03bc using the Infrared Array Camera on the Spitzer Space Telescope. We find relative eclipse depths of 0.137% \u00b1 0.011%, 0.148% \u00b1 0.016%, 0.261% \u00b1 0.059%, and 0.318% \u00b1 0.044% in these four bandpasses, respectively. We also place a 2\u03c3 upper limit of 0.37% on the depth of the secondary eclipse in the 16 \u03bc IRS peak-up array. These eclipse depths reveal that TrES-4 has an emission spectrum similar to that of HD 209458b, which requires the presence of water emission bands created by a thermal inversion layer high in the atmosphere in order to explain the observed features. TrES-4 receives more radiation from its star than HD 209458b and has a correspondingly higher effective temperature, therefore the presence of a temperature inversion in this planet's atmosphere lends support to the idea that inversions might be correlated with the irradiance received by the planet. We find no evidence for any offset in the timing of the secondary eclipse, and place a 3\u03c3 upper limit of |ecos(\u03c9)| < 0.0058, where e is the planet's orbital eccentricity and \u03c9 is the argument of pericenter. From this we conclude that tidal heating from ongoing orbital circularization is unlikely to be the explanation for TrES-4's inflated radius.", "date": "2009-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "691", "number": "1", "publisher": "American Astronomical Society", "pagerange": "866-874", "id_number": "CaltechAUTHORS:20130129-113951785", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-113951785", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NASA", "grant_number": "NNX07AG80G" }, { "agency": "JPL", "grant_number": "1328902" }, { "agency": "NASA", "grant_number": "CAN-02-OSS-02" }, { "agency": "NASA Postdoctoral Program" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/691/1/866", "primary_object": { "basename": "0004-637X_691_1_866.pdf", "url": "https://authors.library.caltech.edu/records/wt2x9-a4979/files/0004-637X_691_1_866.pdf" }, "related_objects": [ { "basename": "0810.0021.pdf", "url": "https://authors.library.caltech.edu/records/wt2x9-a4979/files/0810.0021.pdf" } ], "resource_type": "article", "pub_year": "2009", "author_list": "Knutson, Heather A.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/r3b32-kaj16", "eprint_id": 36648, "eprint_status": "archive", "datestamp": "2023-08-22 14:09:48", "lastmod": "2024-02-02 21:06:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Henry-G-W", "name": { "family": "Henry", "given": "Gregory W." }, "orcid": "0000-0003-4155-8513" }, { "id": "Everett-M-E", "name": { "family": "Everett", "given": "Mark E." }, "orcid": "0000-0002-0885-7215" }, { "id": "Allen-L-E", "name": { "family": "Allen", "given": "Lori E." } } ] }, "title": "Multiwavelength Constraints on the Day-Night Circulation Patterns of HD 189733b", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing; infrared: stars; planetary systems; stars: individual (HD 189733); techniques: photometric", "note": "\u00a9 2009 American Astronomical Society. \n\nReceived 2008 February 13; accepted 2008 September 9; published 2008 December 1. \n\nWe thank David Latham, Matthew Holman, Joshua Winn, Gilbert Esquerdo, Jos\u00e9 Fernandez, Gaspar Bakos, and C\u00e9sar Fuentes for their assistance in obtaining observations of HD 189733 with the FLWO 1.2 m telescope, and for sharing time on their previously scheduled nights to obtain these observations. We thank Mark Marley for helpful discussions, and the referee for a thoughtful and detailed review. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. We also utilize observations made with KeplerCam, which was developed with partial support from the Kepler mission under Cooperative Agreement NCC2-1390. Support for this work was provided by NASA through an award issued by Jet Propulsion Laboratory/California Institute of Technology. H.A.K. was supported by a National Science Foundation Graduate Research Fellowship.\n\nPublished - 0004-637X_690_1_822.pdf
Accepted Version - 0802.1705.pdf
", "abstract": "We present new Spitzer observations of the phase variation of the hot Jupiter HD 189733b in the MIPS 24 \u03bcm bandpass, spanning the same part of the planet's orbit as our previous observations in the IRAC 8 \u03bcm bandpass (Knutson et al. 2007). We find that the minimum hemisphere-averaged flux from the planet in this bandpass is 76% \u00b1 3% of the maximum flux; this corresponds to minimum and maximum hemisphere-averaged brightness temperatures of 984 \u00b1 48 K and 1220 \u00b1 47 K, respectively. The planet reaches its maximum flux at an orbital phase of 0.396 \u00b1 0.022, corresponding to a hot region shifted 20\u00b0-30\u00b0 east of the substellar point. Because tidally locked hot Jupiters would have enormous day-night temperature differences in the absence of winds, the small amplitude of the observed phase variation indicates that the planet's atmosphere efficiently transports thermal energy from the day side to the night side at the 24 \u03bcm photosphere, leading to modest day-night temperature differences. The similarities between the 8 and 24 \u03bcm phase curves for HD 189733b lead us to conclude that the circulation on this planet behaves in a fundamentally similar fashion across the range of pressures sensed by these two wavelengths. One-dimensional radiative transfer models indicate that the 8 \u03bcm band should probe pressures 2-3 times greater than at 24 \u03bcm, although the uncertain methane abundance complicates the interpretation. If these two bandpasses do probe different pressures, it would indicate that the temperature varies only weakly between the two sensed depths, and hence that the atmosphere is not convective at these altitudes. We also present an analysis of the possible contribution of star spots to the time series at both 8 and 24 \u03bcm based on near-simultaneous ground-based observations and additional Spitzer observations. Accounting for the effects of these spots results in a slightly warmer night-side temperature for the planet in both bandpasses, but does not otherwise affect our conclusions.", "date": "2009-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "690", "number": "1", "publisher": "American Astronomical Society", "pagerange": "822-836", "id_number": "CaltechAUTHORS:20130129-111401265", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-111401265", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NCC2-1390" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF Graduate Research Fellowship" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/690/1/822", "primary_object": { "basename": "0004-637X_690_1_822.pdf", "url": "https://authors.library.caltech.edu/records/r3b32-kaj16/files/0004-637X_690_1_822.pdf" }, "related_objects": [ { "basename": "0802.1705.pdf", "url": "https://authors.library.caltech.edu/records/r3b32-kaj16/files/0802.1705.pdf" } ], "resource_type": "article", "pub_year": "2009", "author_list": "Knutson, Heather A.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/98s0q-qp783", "eprint_id": 13519, "eprint_status": "archive", "datestamp": "2023-08-22 13:51:33", "lastmod": "2023-10-17 23:57:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl J." }, "orcid": "0000-0003-4072-169X" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Stauffer-J-R", "name": { "family": "Stauffer", "given": "John" }, "orcid": "0000-0003-3595-7382" }, { "id": "Meadows-V-S", "name": { "family": "Meadows", "given": "Victoria" } }, { "id": "van-Cleve-J", "name": { "family": "van Cleve", "given": "Jeffrey" } }, { "id": "von-Braun-K", "name": { "family": "von Braun", "given": "Kaspar" }, "orcid": "0000-0002-5823-4630" }, { "id": "Levine-D-A", "name": { "family": "Levine", "given": "Deborah" } } ] }, "title": "Strong water absorption in the dayside emission spectrum of the planet HD189733b", "ispublished": "pub", "full_text_status": "restricted", "keywords": "extrasolar giant planets; exoplanet HD 189733B; infrared-emission; space-telescope; light curves; hot Jupiters; 209458B; atmosphere; inversion; contrast", "note": "\u00a9 2008 Nature Publishing Group.\nReceived 13 August 2008; Accepted 17 October 2008.\n\nThis work is based on observations made with the Spitzer\nSpace Telescope, which is operated by the Jet Propulsion Laboratory (JPL),\nCalifornia Institute of Technology (Caltech), under a contract with NASA. Support\nfor this work was provided by NASA through an award issued by JPL/Caltech. This\nstudy was supported in part by NASA (grant NNGO4GL22G).", "abstract": "Recent observations of the extrasolar planet HD189733b did not reveal the presence of water in the emission spectrum of the planet^1. Yet models of such 'hot-Jupiter' planets predict an abundance of atmospheric water vapour^2. Validating and constraining these models is crucial to understanding the physics and chemistry of planetary atmospheres in extreme environments. Indications of the presence of water in the atmosphere of HD189733b have recently been found in transmission spectra^3,4, where the planet's atmosphere selectively absorbs the light of the parent star, and in broadband photometry^5. Here we report the detection of strong water absorption in a high- signal- to- noise, mid- infrared emission spectrumof the planet itself. We find both a strong downturn in the flux ratio below 10 \u00b5m and discrete spectral features that are characteristic of strong absorption by water vapour. The differences between these and previous observations are significant and admit the possibility that predicted planetary- scale dynamical weather structures^6 may alter the emission spectrum over time. Models that match the observed spectrum and the broadband photometry suggest that heat redistribution from the dayside to the nightside is weak. Reconciling this with the high nightside temperature^7 will require a better understanding of atmospheric circulation or possible additional energy sources.", "date": "2008-12-11", "date_type": "published", "publication": "Nature", "volume": "456", "number": "7223", "publisher": "Nature Publishing Group", "pagerange": "767-769", "id_number": "CaltechAUTHORS:GRInat08", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:GRInat08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG04GL22G" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1038/nature07574", "resource_type": "article", "pub_year": "2008", "author_list": "Grillmair, Carl J.; Burrows, Adam; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/a72bx-81m51", "eprint_id": 13760, "eprint_status": "archive", "datestamp": "2023-08-22 13:34:08", "lastmod": "2023-10-18 00:07:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Devor-J", "name": { "family": "Devor", "given": "Jonathan" } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" }, { "id": "Blake-C-H", "name": { "family": "Blake", "given": "Cullen H." } }, { "id": "White-R-J", "name": { "family": "White", "given": "Russel J." }, "orcid": "0000-0001-5313-7498" }, { "id": "Rabus-M", "name": { "family": "Rabus", "given": "Markus" } }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "Georgi" } }, { "id": "Bakos-G-\u00c1", "name": { "family": "Bakos", "given": "Gaspar \u00c1." }, "orcid": "0000-0001-7204-6727" }, { "id": "F\u0171r\u00e9sz-G", "name": { "family": "F\u0171r\u00e9sz", "given": "G\u00e1bor" } }, { "id": "Szentgyorgyi-A", "name": { "family": "Szentgyorgyi", "given": "Andrew" } } ] }, "title": "T-Lyr1-17236 : a long-period low-mass eclipsing binary", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: close; binaries: eclipsing; stars: fundamental parameters; stars: individual (T-Lyr1-17236); stars: late-type", "note": "\u00a9 2008 The American Astronomical Society.\nReceived 2008 April 4; accepted 2008 July 22.\nWe would like to thank Joel Hartman and Doug Mink for\ntheir help in operating a few of the software analysis tools used\nfor this paper, and we would like to thank Sarah Dykstra for her\neditorial assistance. Valeri Hambaryan provided expert assistance\nin examining archival ROSAT images of T-Lyr1-17236,\nfor which we are grateful, and we thank the referee for a number\nof helpful comments that have improved the paper. G. T.\nacknowledges partial support from NSF grant AST 07-08229\nand NASA's MASSIF SIM Key Project (BLF57-04). This\nresearch has made use of NASA's Astrophysics Data System\nBibliographic Services, as well as the SIMBAD database operated\nat CDS, Strasbourg, France. This publication also used\ndata products from the Two Micron All Sky Survey, which is a\njoint project of the University of Massachusetts and the Infrared\nProcessing and Analysis Center, California Institute of\nTechnology, and is funded by NASA and the National Science\nFoundation. Some of the data presented herein were obtained\nat the W. M. Keck Observatory, which is operated as a scientific\npartnership among Caltech, the University of California,\nand NASA. The Observatory was made possible by the generous\nfinancial support of the W. M. Keck Foundation. The authors\nwish to recognize and acknowledge the very significant cultural\nrole and reverence that the summit of Mauna Kea has always had\nwithin the indigenous Hawaiian community. We are most fortunate\nto have the opportunity to conduct observations from this\nmountain.\n\nPublished - DEVapj08.pdf
", "abstract": "We describe the discovery of a 0.68+0.52 M\u2299 eclipsing binary (EB) with an 8.4 day orbital period, found through a systematic search of 10 fields of the Trans-atlantic Exoplanet Survey (TrES). Such long-period low-mass EBs constitute critical test cases for resolving the long-standing discrepancy between the theoretical and observational mass-radius relations at the bottom of the main sequence. It has been suggested that this discrepancy may be related to strong stellar magnetic fields, which are not properly accounted for in current theoretical models. All previously well-characterized low-mass main-sequence EBs have periods of a few days or less, and their components are therefore expected to be rotating rapidly as a result of tidal synchronization, thus generating strong magnetic fields. In contrast, the binary system described here has a period that is more than 3 times longer than previously characterized low-mass main-sequence EBs, and its components rotate relatively slowly. It is therefore expected to have a weaker magnetic field and to better match the assumptions of theoretical stellar models. Our follow-up observations of this EB yield preliminary stellar properties that suggest it is indeed consistent with current models. If further observations confirm a low level of activity in this system, these determinations would provide support for the hypothesis that the mass-radius discrepancy is at least partly due to magnetic activity.", "date": "2008-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "687", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1253-1263", "id_number": "CaltechAUTHORS:DEVapj08", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:DEVapj08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 07-08229" }, { "agency": "NASA", "grant_number": "BLF57-04" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1086/592080", "primary_object": { "basename": "DEVapj08.pdf", "url": "https://authors.library.caltech.edu/records/a72bx-81m51/files/DEVapj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Devor, Jonathan; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/kt1ed-d4r22", "eprint_id": 36645, "eprint_status": "archive", "datestamp": "2023-08-19 23:48:01", "lastmod": "2024-02-02 21:06:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Barman-T-S", "name": { "family": "Barman", "given": "Travis" }, "orcid": "0000-0002-7129-3002" }, { "id": "Allen-L-E", "name": { "family": "Allen", "given": "Lori E." } }, { "id": "Mayor-M", "name": { "family": "Mayor", "given": "Michel" } }, { "id": "Megeath-S-T", "name": { "family": "Megeath", "given": "S. Thomas" }, "orcid": "0000-0001-7629-3573" }, { "id": "Queloz-D", "name": { "family": "Queloz", "given": "Didier" }, "orcid": "0000-0002-3012-0316" }, { "id": "Udry-S", "name": { "family": "Udry", "given": "St\u00e9phane" } } ] }, "title": "The Broadband Infrared Emission Spectrum of the Exoplanet HD 189733b", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2008 American Astronomical Society. \n\nReceived 2008 February 6; accepted 2008 July 7. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. H. A. K. was supported by a National Science\nFoundation Graduate Research Fellowship. \n\nFacilities: Spitzer ( IRAC, IRS, MIPS).\n\nPublished - 0004-637X_686_2_1341.pdf
Accepted Version - 0802.0845.pdf
", "abstract": "We present Spitzer Space Telescope time series photometry of the exoplanet system HD 189733 spanning two times of secondary eclipse, when the planet passes out of view behind the parent star. We estimate the relative eclipse depth in five distinct bands and find the planet-to-star flux ratio to be 0.256% \u00b1 0.014% (3.6 \u03bcm), 0.214% \u00b1 0.020% (4.5 \u03bcm), 0.310% \u00b1 0.034% (5.8 \u03bcm), 0.391% \u00b1 0.022% (8.0 \u03bcm), and 0.598% \u00b1 0.038% (24 \u03bcm). For consistency, we reanalyze a previously published time series to deduce a contrast ratio in an additional band, 0.519% \u00b1 0.020% (16 \u03bcm). Our data are strongly inconsistent with a Planck spectrum, and we clearly detect emission near 4 \u03bcm as predicted by published theoretical models in which this feature arises from a corresponding opacity window. Unlike recent results for the exoplanet HD 209458b, we find that the emergent spectrum from HD 189733b is best matched by models that do not include an atmospheric temperature inversion. Taken together, these two studies provide initial observational support for the idea that hot Jupiter atmospheres diverge into two classes, in which a thermal inversion layer is present for the more strongly irradiated objects.", "date": "2008-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "686", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1341-1348", "id_number": "CaltechAUTHORS:20130129-105835699", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-105835699", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF Graduate Research Fellowship" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/591635", "primary_object": { "basename": "0004-637X_686_2_1341.pdf", "url": "https://authors.library.caltech.edu/records/kt1ed-d4r22/files/0004-637X_686_2_1341.pdf" }, "related_objects": [ { "basename": "0802.0845.pdf", "url": "https://authors.library.caltech.edu/records/kt1ed-d4r22/files/0802.0845.pdf" } ], "resource_type": "article", "pub_year": "2008", "author_list": "Charbonneau, David; Knutson, Heather A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/tx01d-7zb58", "eprint_id": 95643, "eprint_status": "archive", "datestamp": "2023-08-22 11:40:43", "lastmod": "2024-02-02 21:12:02", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nutzman-P", "name": { "family": "Nutzman", "given": "Philip" } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Winn-J-N", "name": { "family": "Winn", "given": "Joshua N." }, "orcid": "0000-0002-4265-047X" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Holman-M-J", "name": { "family": "Holman", "given": "Matthew J." }, "orcid": "0000-0002-1139-4880" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" } ] }, "title": "A Precise Estimate of the Radius of HD 149026b", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2009 International Astronomical Union.\n\nPublished - precise_estimate_of_the_radius_of_hd_149026b.pdf
Accepted Version - 0807.1318.pdf
", "abstract": "We present Spitzer 8 \u03bcm transit observations of the extrasolar planet system HD 149026b. At this wavelength, transit light curves are weakly affected by stellar limb-darkening, allowing for a simpler and more accurate determination of planetary parameters. We measure a planet-star radius ratio of R_p/R\u2217=0.05158\u00b10.00077, and in combination with ground-based data and independent constraints on the stellar mass and radius, we derive an orbital inclination of i = 85\u00b0.4^(+0\u00b0.9)_(\u22120\u00b0.8) and a planet radius of 0.755 \u00b1 0.040 R_J. These measurements further support models in which the planet is greatly enriched in heavy elements.", "date": "2008-05", "date_type": "published", "publisher": "Cambridge University Press", "place_of_pub": "Cambridge", "pagerange": "466-469", "id_number": "CaltechAUTHORS:20190521-112359091", "isbn": "9780521889841", "book_title": "Transiting Planets", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190521-112359091", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "contributors": { "items": [ { "id": "Pont-F", "name": { "family": "Pont", "given": "Fr\u00e9d\u00e9ric" } }, { "id": "Sasselov-D", "name": { "family": "Sasselov", "given": "Dimitar" } }, { "id": "Holman-M", "name": { "family": "Holman", "given": "Matthews" } } ] }, "doi": "10.1017/s1743921308026951", "primary_object": { "basename": "0807.1318.pdf", "url": "https://authors.library.caltech.edu/records/tx01d-7zb58/files/0807.1318.pdf" }, "related_objects": [ { "basename": "precise_estimate_of_the_radius_of_hd_149026b.pdf", "url": "https://authors.library.caltech.edu/records/tx01d-7zb58/files/precise_estimate_of_the_radius_of_hd_149026b.pdf" } ], "resource_type": "book_section", "pub_year": "2008", "author_list": "Nutzman, Philip; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/g6adn-35j69", "eprint_id": 36981, "eprint_status": "archive", "datestamp": "2023-08-22 11:23:24", "lastmod": "2024-02-02 21:07:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pont-F", "name": { "family": "Pont", "given": "F." }, "orcid": "0000-0003-0076-5444" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "H." }, "orcid": "0000-0002-5375-4725" }, { "id": "Gilliland-R-L", "name": { "family": "Gilliland", "given": "R. L." }, "orcid": "0000-0002-1554-5578" }, { "id": "Moutou-C", "name": { "family": "Moutou", "given": "C." } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "D." }, "orcid": "0000-0002-9003-484X" } ] }, "title": "Detection of atmospheric haze on an extrasolar planet: the 0.55\u20131.05 \u03bcm transmission spectrum of HD 189733b with the Hubble Space Telescope", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis \u2013 planetary systems \u2013 techniques: spectroscopic", "note": "\u00a9 2008 The Authors. Journal compilation \u00a9 2008 RAS.\nAccepted 2007 December 11. Received 2007 December 9; in original form 2007 October 1.\nThe authors wish to thank Mark Swain and Giovanna Tinetti for\nvery helpful discussions, and the anonymous referee for numerous suggestions that helped improving the manuscript.\n\nPublished - j.1365-2966.2008.12852.x.pdf
", "abstract": "The nearby transiting planet HD 189733b was observed during three transits with the Advanced Camera for Surveys of the Hubble Space Telescope in spectroscopic mode. The resulting time-series of 675 spectra covers the 550\u20131050 nm range, with a resolution element of \u223c8 nm, at extremely high accuracy (signal-to-noise ratio up to 10 000 in 50-nm intervals in each individual spectrum). Using these data, we disentangle the effects of limb darkening, measurement systematics and spots on the surface of the host star, to calculate the wavelength dependence of the effective transit radius to an accuracy of \u223c50 km. This constitutes the 'transmission spectrum' of the planetary atmosphere. It indicates at each wavelength at what height the planetary atmosphere becomes opaque to the grazing stellar light during the transit. In this wavelength range, strong features due to sodium, potassium and water are predicted by atmosphere models for a planet like HD 189733b, but they can be hidden by broad absorption from clouds or hazes higher up in the atmosphere.\n\nWe observed an almost featureless transmission spectrum between 550 and 1050 nm, with no indication of the expected sodium or potassium atomic absorption features. Comparison of our results with the transit radius observed in the near and mid-infrared (2\u20138 \u03bcm), and the slope of the spectrum, suggest the presence of a haze of submicrometre particles in the upper atmosphere of the planet.", "date": "2008-03-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "385", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "109-118", "id_number": "CaltechAUTHORS:20130219-110113552", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130219-110113552", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1111/j.1365-2966.2008.12852.x", "primary_object": { "basename": "j.1365-2966.2008.12852.x.pdf", "url": "https://authors.library.caltech.edu/records/g6adn-35j69/files/j.1365-2966.2008.12852.x.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Pont, F.; Knutson, H.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/44ep9-t9d34", "eprint_id": 13277, "eprint_status": "archive", "datestamp": "2023-08-22 11:12:17", "lastmod": "2023-10-17 23:22:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Deeg-H-J", "name": { "family": "Deeg", "given": "H. J." } }, { "id": "Oca\u00f1a-B", "name": { "family": "Oca\u00f1a", "given": "B." } }, { "id": "Kozhevnikov-V-P", "name": { "family": "Kozhevnikov", "given": "V. P." } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "D." }, "orcid": "0000-0002-9003-484X" }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "F. T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Doyle-L-R", "name": { "family": "Doyle", "given": "L. R." } } ] }, "title": "Extrasolar planet detection by binary stellar eclipse timing: evidence for a third body around CM Draconis", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: individual: CM Dra; stars: binaries: eclipsing; eclipses; stars: planetary systems", "note": "\u00a9 ESO 2008. \n\nReceived 5 November 2007 / Accepted 28 December 2007. \n\nSome of the observations published in this article were made with the IAC80 telescope operated by the Instituto de Astrof\u00edsica de Tenerife in the Observatorio del Teide, and with the INT telelescope operated by the Isaac Newtown Group of Telescopes in the Observatorio del Roque de los Muchachos. This research was supported by Grant ESP2004-03855-C03-03 of the Spanish Education and Science Ministry. Some material presented here is based on work supported by NASA under the grant NNG05GJ29G, issued through the Origins of Solar Systems Program.\n\nPublished - DEEaanda08.pdf
", "abstract": "Aims. Our objective is to elucidate the physical process that causes the observed observed-minus-calculated (O-C) behavior in the M4.5/ M4.5 binary CM Dra and to test for any evidence of a third body around the CM Dra system. \n\nMethods. New eclipse minimum timings of CM Dra were obtained between the years 2000 and 2007. The O-C times of the system are fitted against several functions, representing different physical origins of the timing variations. \n\nResults. Using our observational data in conjunction with published timings going back to 1977, a clear non-linearity in O-C times is apparent. An analysis using model-selection statistics gives about equal weight to a parabolic and to a sinusoidal fitting function. Attraction from a third body, either at large distance in a quasi-constant constellation across the years of observations or from a body on a shorter orbit generating periodicities in O-C times is the most likely source of the observed O-C times. The white dwarf GJ 630.1B, a proper motion companion of CM Dra, can however be rejected as the responsible third body. Also, no further evidence of the short-periodic planet candidate described by Deeg et al. (2000, A&A, 358, L5) is found, whereas other mechanisms, such as period changes from stellar winds or Applegate's mechanism can be rejected. \n\nConclusions. A third body, being either a few-Jupiter-mass object with a period of 18.5 \u00b1 4.5 years or an object in the mass range of 1.5 M-jup to 0.1 M\u2609 with periods of hundreds to thousands of years is the most likely origin of the observed minimum timing behavior.", "date": "2008-03", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "480", "number": "2", "publisher": "EDP Sciences", "pagerange": "563-571", "id_number": "CaltechAUTHORS:DEEaanda08", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:DEEaanda08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministerio de Educaci\u00f3n y Ciencia (Spain)", "grant_number": "ESP2004-03855-C03-03" }, { "agency": "NASA", "grant_number": "NNG05GJ29G" } ] }, "doi": "10.1051/0004-6361:20079000", "primary_object": { "basename": "DEEaanda08.pdf", "url": "https://authors.library.caltech.edu/records/44ep9-t9d34/files/DEEaanda08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Deeg, H. J.; Oca\u00f1a, B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/n3np8-w6r31", "eprint_id": 13280, "eprint_status": "archive", "datestamp": "2023-08-22 11:12:22", "lastmod": "2023-10-17 23:22:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Devor-J", "name": { "family": "Devor", "given": "Jonathan" } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "Georgi" } }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" } ] }, "title": "Identification, classifications, and absolute properties of 773 eclipsing binaries found in the Trans-Atlantic Exoplanet Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing; catalogs; methods: data analysis; stars: statistics; techniques: photometric", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2007 September 5; accepted 2007 December 5; published 2008 February 5. Print publication: Issue 3 (2008 March). \n\nWe would like to thank Tsevi Mazeh for many useful discussions, as well as S\u00f8ren Meibom for his repeated help. We would also like to thank Sarah Dykstra for her continuous support throughout the preparation of this paper. We are grateful to the staff of the Palomar Observatory for their assistance in operating the Sleuth instrument, and we acknowledge support from NASA through grant NNG05GJ29G issued through the Origins of Solar Systems Program. This research has made use of the NASA's Astrophysics Data System Bibliographic Services, the SIMBAD database, operated at CDS, Strasbourg, and the VSX database, which was created by Christopher Watson for the AAVSO. This publication also utilizes data products from 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and NSF. Finally, we would like to thank the anonymous referee for very insightful comments and suggestions, which significantly improved this manuscript. \n\n[D..C. was an] Alfred P. Sloan Research Fellow.\n\nPublished - DEVaj08.pdf
", "abstract": "In recent years, we have witnessed an explosion of photometric time-series data, collected for the purpose of finding a small number of rare sources, such as transiting extrasolar planets and gravitational microlenses. Once combed, these data are often set aside, and are not further searched for the many other variable sources that they undoubtedly contain. To this end, we describe a pipeline that is designed to systematically analyze such data, while requiring minimal user interaction. We ran our pipeline on a subset of the Trans-Atlantic Exoplanet Survey dataset, and used it to identify and model 773 eclipsing binary systems. For each system we conducted a joint analysis of its light curve, colors, and theoretical isochrones. This analysis provided us with estimates of the binary's absolute physical properties, including the masses and ages of their stellar components, as well as their physical separations and distances. We identified three types of eclipsing binaries that are of particular interest and merit further observations. The first category includes 11 low-mass candidates, which may assist current efforts to explain the discrepancies between the observation and the models of stars at the bottom of the main sequence. The other two categories include 34 binaries with eccentric orbits, and 20 binaries with abnormal light curves. Finally, this uniform catalog enabled us to identify a number of relations that provide further constraints on binary population models and tidal circularization theory.", "date": "2008-03", "date_type": "published", "publication": "Astronomical Journal", "volume": "135", "number": "3", "publisher": "American Astronomical Society", "pagerange": "850-877", "id_number": "CaltechAUTHORS:DEVaj08", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:DEVaj08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG05GJ29G" }, { "agency": "NSF" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "doi": "10.1088/0004-6256/135/3/850", "primary_object": { "basename": "DEVaj08.pdf", "url": "https://authors.library.caltech.edu/records/n3np8-w6r31/files/DEVaj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Devor, Jonathan; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/y2bzn-mzf24", "eprint_id": 36644, "eprint_status": "archive", "datestamp": "2023-08-22 11:01:01", "lastmod": "2024-02-02 21:06:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Allen-L-E", "name": { "family": "Allen", "given": "Lori E." } }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "Adam" }, "orcid": "0000-0002-3099-5024" }, { "id": "Megeath-S-T", "name": { "family": "Megeath", "given": "S. Thomas" }, "orcid": "0000-0001-7629-3573" } ] }, "title": "The 3.6-8.0 \u03bcm Broadband Emission Spectrum of HD 209458b: Evidence for an Atmospheric Temperature Inversion", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2008 American Astronomical Society. \n\nReceived 2007 July 31; accepted 2007 September 24. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. H. A. K. was supported by a National Science Foundation Graduate Research Fellowship.A. B.would like to acknowledge support from NASA under grants NNG04GL22G and NNX07AG80G and through the NASA Astrobiology Institute under cooperative agreement CAN-02-OSS-02 issued through the Office of Space Science. We would also like to thank J. Matthews for sharing MOST results in advance of publication.\n\nPublished - 0004-637X_673_1_526.pdf
Accepted Version - 0709.3984.pdf
", "abstract": "We estimate the strength of the bandpass-integrated thermal emission from the extrasolar planet HD 209458b at 3.6, 4.5, 5.8, and 8.0 \u03bcm using the Infrared Array Camera (IRAC) on the Spitzer Space Telescope. We observe a single secondary eclipse simultaneously in all four bandpasses and find relative eclipse depths of 0.00094 \u00b1 0.00009, 0.00213 \u00b1 0.00015, 0.00301 \u00b1 0.00043, and 0.00240 \u00b1 0.00026, respectively. These eclipse depths reveal that the shape of the inferred emission spectrum for the planet differs significantly from the predictions of standard atmosphere models; instead, the most plausible explanation would require the presence of an inversion layer high in the atmosphere leading to significant water emission in the 4.5 and 5.8 \u03bcm bandpasses. This is the first clear indication of such a temperature inversion in the atmosphere of a hot Jupiter, as previous observations of other planets appeared to be in reasonably good agreement with the predictions of models without such an inversion layer.", "date": "2008-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "673", "number": "1", "publisher": "American Astronomical Society", "pagerange": "526-531", "id_number": "CaltechAUTHORS:20130129-104056356", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130129-104056356", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NASA", "grant_number": "NNG04GL22G" }, { "agency": "NASA", "grant_number": "NNX07AG80G" }, { "agency": "NASA", "grant_number": "CAN-02-OSS-02" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/523894", "primary_object": { "basename": "0004-637X_673_1_526.pdf", "url": "https://authors.library.caltech.edu/records/y2bzn-mzf24/files/0004-637X_673_1_526.pdf" }, "related_objects": [ { "basename": "0709.3984.pdf", "url": "https://authors.library.caltech.edu/records/y2bzn-mzf24/files/0709.3984.pdf" } ], "resource_type": "article", "pub_year": "2008", "author_list": "Knutson, Heather A.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/wz1r9-wjv10", "eprint_id": 37336, "eprint_status": "archive", "datestamp": "2023-08-22 10:16:27", "lastmod": "2024-02-02 21:07:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "A. S." }, "orcid": "0000-0002-3099-5024" }, { "id": "Hubeny-I", "name": { "family": "Hubeny", "given": "I." } }, { "id": "Budaj-J", "name": { "family": "Budaj", "given": "J." } }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "H. A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "D." }, "orcid": "0000-0002-9003-484X" } ] }, "title": "Theoretical Spectral Models of the Planet HD 209458b with a Thermal Inversion and Water Emission Bands", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems; planets and satellites: general; stars: individual (HD 209458)", "note": "\u00a9 2007 American Astronomical Society. Received 2007 August 1; accepted 2007 August 28; published 2007 September 26. We thank Drake Deming, Bill Hubbard, Maki Hattori, Mike\nCushing, and Drew Milsom for helpful discussions. This study\nwas supported in part by NASA grants NNG04GL22G and\nNNX07AG80G and through the NASA Astrobiology Institute\nunder cooperative agreement CAN-02-OSS-02 issued through\nthe Office of Space Science.\n\nPublished - 1538-4357_668_2_L171.pdf
", "abstract": "We find that a theoretical fit to all the HD 209458b data at secondary eclipse requires that the day-side atmosphere of HD 209458b have a thermal inversion and a stratosphere. This inversion is caused by the capture of optical stellar flux by an absorber of uncertain origin that resides at altitude. One consequence of stratospheric heating and temperature inversion is the flipping of water absorption features into emission features from the near- to the mid-infrared, and we see evidence of such a water emission feature in the recent HD 209458b IRAC data of Knutson et al. In addition, an upper-atmosphere optical absorber may help explain both the weaker-than-expected Na D feature seen in transit and the fact that the transit radius at 24 \u03bcm is smaller than the corresponding radius in the optical. Moreover, it may be a factor in why HD 209458b's optical transit radius is as large as it is. We speculate on the nature of this absorber and the planets whose atmospheres may, or may not, be affected by its presence.", "date": "2007-10-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "668", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L171-L174", "id_number": "CaltechAUTHORS:20130306-092436832", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130306-092436832", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG04GL22G" }, { "agency": "NASA", "grant_number": "NNX07AG80G" }, { "agency": "NASA", "grant_number": "CAN-02-OSS-02" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/522834", "primary_object": { "basename": "1538-4357_668_2_L171.pdf", "url": "https://authors.library.caltech.edu/records/wz1r9-wjv10/files/1538-4357_668_2_L171.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Burrows, A. S.; Hubeny, I.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/15j82-ekf33", "eprint_id": 17395, "eprint_status": "archive", "datestamp": "2023-08-22 10:11:13", "lastmod": "2023-10-19 23:51:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "Georgi" } }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Bakos-G-\u00c1", "name": { "family": "Bakos", "given": "G\u00e1sp\u00e1r \u00c1." }, "orcid": "0000-0001-7204-6727" }, { "id": "Dunham-E-W", "name": { "family": "Dunham", "given": "Edward W." } }, { "id": "Sozzetti-A", "name": { "family": "Sozzetti", "given": "Alessandro" } }, { "id": "Fern\u00e1ndez-J-M", "name": { "family": "Fern\u00e1ndez", "given": "Jos\u00e9 M." } }, { "id": "Esquerdo-G-A", "name": { "family": "Esquerdo", "given": "Gilbert A." }, "orcid": "0000-0002-9789-5474" }, { "id": "Everett-M-E", "name": { "family": "Everett", "given": "Mark E." }, "orcid": "0000-0002-0885-7215" }, { "id": "Brown-T-M", "name": { "family": "Brown", "given": "Timothy M." }, "orcid": "0000-0002-1793-9968" }, { "id": "Rabus-M", "name": { "family": "Rabus", "given": "Markus" } }, { "id": "Belmonte-J-A", "name": { "family": "Belmonte", "given": "Juan A." } }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." } } ] }, "title": "TrES-4: A Transiting Hot Jupiter of Very Low Density", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems; techniques : photometric; techniques : radial velocities; techniques : spectroscopic", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2007 June 18; accepted 2007 August 6; published 2007 September 14.\nWe thank Travis Barman for useful discussions. This\nLetter is based on work supported in part by NASA\ngrants NNG04GN74G, NNG04LG89G, NNG05GI57G,\nNNG05GJ29G, and NNH05AB88I through the Origins of Solar\nSystems Program, and NASA Planetary Major Equipment grant\nN4G5-12229.We acknowledge support from the NASA Kepler\nmission under cooperative agreement NCC2-1390. Work by\nG. A\u00b4. B. was supported by NASA through Hubble Fellowship\ngrant HST-HF-01170.01-A. Observing time on Keck I was\nawarded by NASA.\n\nPublished - MANapjl07.pdf
", "abstract": "We report the discovery of TrES-4, a hot Jupiter that transits the star GSC 02620-00648 every 3.55 days. From high-resolution spectroscopy of the star, we estimate a stellar effective temperature of T_(eff) = 6100 \u00b1 150 K, and from high-precision z and B photometry of the transit we constrain the ratio of the semimajor axis a and the stellar radius R_* to be a/R_* = 6.03 \u00b1 0.13. We compare these values to model stellar isochrones to constrain the stellar mass to be M_* = 1.22 \u00b1 0.17 M_\u2299. Based on this estimate and the photometric time series, we constrain the stellar radius to be R_* = 1.738 \u00b1 0.092 R_\u2299 and the planet radius to be R_p = 1.674 \u00b1 0.094 R_(Jup). We model our radial velocity data assuming a circular orbit and find a planetary mass of 0.84 \u00b1 0.10 M_(Jup). Our radial velocity observations rule out line-bisector variations that would indicate a specious detection resulting from a blend of an eclipsing binary system. TrES-4 has the largest radius and lowest density of any of the known transiting planets. It presents a challenge to current models of the physical structure of hot Jupiters and indicates that the diversity of physical properties among the members of this class of exoplanets has yet to be fully explored.", "date": "2007-10-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "667", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L195-L198", "id_number": "CaltechAUTHORS:20100205-095420946", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100205-095420946", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG04GN74G" }, { "agency": "NASA", "grant_number": "NNG04LG89G" }, { "agency": "NASA", "grant_number": "NNG05GI57G" }, { "agency": "NASA", "grant_number": "NNG05GJ29G" }, { "agency": "NASA", "grant_number": "NNH05AB88I" }, { "agency": "NASA Planetary Major Equipment", "grant_number": "N4G5-12229" }, { "agency": "NASA Kepler mission", "grant_number": "NCC2-1390" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01170.01-A" } ] }, "doi": "10.1086/522115", "primary_object": { "basename": "MANapjl07.pdf", "url": "https://authors.library.caltech.edu/records/15j82-ekf33/files/MANapjl07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Mandushev, Georgi; O'Donovan, Francis T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/666zq-aq474", "eprint_id": 17402, "eprint_status": "archive", "datestamp": "2023-08-22 09:41:35", "lastmod": "2023-10-19 23:51:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sozzetti-A", "name": { "family": "Sozzetti", "given": "Alessandro" } }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Holman-M-J", "name": { "family": "Holman", "given": "Matthew J." }, "orcid": "0000-0002-1139-4880" }, { "id": "Winn-J-N", "name": { "family": "Winn", "given": "Joshua N." }, "orcid": "0000-0002-4265-047X" }, { "id": "Laird-J-B", "name": { "family": "Laird", "given": "John B." } }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" } ] }, "title": "Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES-2", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems; stars: abundances; stars: fundamental parameters; stars: individual (TrES-2)", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 August 1); received 2007 March 12; accepted for publication 2007 April 21.\n\nWe thank K. Biazzo (Catania Astrophysical Observatory) for\nproviding the LDR calibrations in advance of publication, and A. Burrows and A. Spagna for helpful discussions. G. T. acknowledges partial support for this work from NASA Origins grant NNG04LG89G.D.C. is supported in part by NASA Origins grant NNG05GJ29G.A. S. gratefully acknowledges the Kepler mission for partial support under NASA cooperative agreement NCC 2-1390. J. B. L gratefully acknowledges support from NSF grant AST 03-07340. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific\npartnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M.Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within\nthe indigenous Hawaiian community. We are most fortunate to\nhave the opportunity to conduct observations from this mountain.\nThis research hasmade use of NASA's Astrophysics Data System\nAbstract Service and of the SIMBAD database, operated at CDS,\nStrasbourg, France.\n\nPublished - SOZapj07.pdf
", "abstract": "We report on a spectroscopic determination of the atmospheric parameters and chemical abundance of the parent star of the recently discovered transiting planet TrES-2. A detailed LTE analysis of a set of Fe I and Fe II lines from our Keck spectra yields T_(eff) = 5850 \u00b1 50 K, log g = 4.4 \u00b1 0.1, and [Fe/H] = -0.15 \u00b1 0.10. Several independent checks (e.g., additional spectroscopy, line-depth ratios) confirm the reliability of our spectroscopic T_(eff) estimate. The mass and radius of the star, needed to determine the properties of the planet, are traditionally inferred by comparison with stellar evolution models using T_(eff) and some measure of the stellar luminosity, such as the spectroscopic surface gravity. We apply here a new method in which we use instead of log g the normalized separation a/R_* (related to the stellar density), directly measurabele from the light curves of transiting planets with much greater precision. With the a/R_* value from the light-curve analysis of Holman and coworkers and our T_(eff) estimate, we obtain M_* = 0.980 \u00b1 0.062 M_\u2609 and R_* = 1.000^(+0.036)_(-0.033) R_\u2609, and an evolutionary age of 5.1^(+2.7)_(-2.3) Gyr, in good agreement with other constraints (Ca II H and K line cores, lithium abundance, and rotation). The new stellar parameters yield improved values for the planetary mass and radius of M_p = 1.198 \u00b1 0.053 M_J and R_p = 1.220^(+0.045)_(-0.042) R_J, confirming that TrES-2 is the most massive among the currently known nearby (d \u2272 300 pc) transiting hot Jupiters. The surface gravity of the planet, log g_p = 3.299 \u00b1 0.016, can be derived independently of the knowledge of the stellar parameters (i.e., directly from observations), and with a very high precision rivaling that of the best known double-lined eclipsing binaries.", "date": "2007-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "664", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1190-1198", "id_number": "CaltechAUTHORS:20100205-112554338", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100205-112554338", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG04LG89G" }, { "agency": "NASA", "grant_number": "NNG05GJ29G" }, { "agency": "NASA", "grant_number": "NCC 2-1390" }, { "agency": "NSF", "grant_number": "AST 03-07340" } ] }, "doi": "10.1086/519214", "primary_object": { "basename": "SOZapj07.pdf", "url": "https://authors.library.caltech.edu/records/666zq-aq474/files/SOZapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Sozzetti, Alessandro; Torres, Guillermo; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/w6psp-mfs35", "eprint_id": 12966, "eprint_status": "archive", "datestamp": "2023-08-22 09:41:18", "lastmod": "2023-10-17 21:40:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Holman-M-J", "name": { "family": "Holman", "given": "Matthew J." }, "orcid": "0000-0002-1139-4880" }, { "id": "Winn-J-N", "name": { "family": "Winn", "given": "Joshua N." }, "orcid": "0000-0002-4265-047X" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" }, { "id": "Sozzetti-A", "name": { "family": "Sozzetti", "given": "Alessandro" } }, { "id": "Fernandez-J", "name": { "family": "Fernandez", "given": "Jose" } }, { "id": "Everett-M-E", "name": { "family": "Everett", "given": "Mark E." }, "orcid": "0000-0002-0885-7215" } ] }, "title": "The Transit Light Curve (TLC) Project. VI. Three Transits of the Exoplanet TrES-2", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems; stars: individual (GSC 03549-02811); techniques: photometric", "note": "\u00a9 2007. The American Astronomical Society. \n\nReceived 2007 March 20; accepted 2007 April 20. Print publication: Issue 2 (2007 August 1). \n\nWe thank E. Falco for accommodating our observing schedule changes. KeplerCam was developed with partial support from the Kepler mission under NASA Cooperative Agreement NCC2-1390 (PI: D. Latham), and the KeplerCam observations described in this paper were partly supported by grants from the Kepler mission to SAO and PSI. N.M.J.H. acknowledges support for this work NASA Origins grant NG06GH69G. Work by F.T.O'D. and D.C. was supported by NASA under grant NNG05GJ29G, issued through the Origins of Solar Systems Program. A.S. gratefully acknowledges the Kepler mission for partial support under NASA Cooperative Agreement NCC 2-1390. G.T. acknowledges partial support for this work from NASA Origins grant NNG04LG89G.\n\nPublished - HOLapj07.pdf
", "abstract": "Of the nearby transiting exoplanets that are amenable to detailed study, TrES-2 is both the most massive and the one with the largest impact parameter. We present z-band photometry of three transits of TrES-2. We improve on the estimates of the planetary, stellar, and orbital parameters, in conjunction with the spectroscopic analysis of the host star by Sozzetti and coworkers. We find the planetary radius to be Rp = 1.222 \u00b1 0.038 RJup and the stellar radius to be R* = 1.003 \u00b1 0.027 R\u2609. The quoted uncertainties include the systematic error due to the uncertainty in the stellar mass (M* = 0.980 \u00b1 0.062 M\u2609). The timings of the transits have an accuracy of 25 s and are consistent with a uniform period, thus providing a baseline for future observations with the NASA Kepler satellite, whose field of view will include TrES-2.", "date": "2007-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "664", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1185-1189", "id_number": "CaltechAUTHORS:HOLapj07", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:HOLapj07", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NCC2-1390" }, { "agency": "NASA", "grant_number": "NG06GH69G" }, { "agency": "NASA", "grant_number": "NNG05GJ29G" }, { "agency": "NASA", "grant_number": "NNG04LG89G" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "doi": "10.1086/519077", "primary_object": { "basename": "HOLapj07.pdf", "url": "https://authors.library.caltech.edu/records/w6psp-mfs35/files/HOLapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Holman, Matthew J.; Winn, Joshua N.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9zbh4-bms24", "eprint_id": 18015, "eprint_status": "archive", "datestamp": "2023-08-22 09:28:36", "lastmod": "2023-10-20 15:30:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Bakos-G-\u00c1", "name": { "family": "Bakos", "given": "G\u00e1sp\u00e1r \u00c1." }, "orcid": "0000-0001-7204-6727" }, { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "Georgi" } }, { "id": "Dunham-E-W", "name": { "family": "Dunham", "given": "Edward W." } }, { "id": "Brown-T-M", "name": { "family": "Brown", "given": "Timothy M." }, "orcid": "0000-0002-1793-9968" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" }, { "id": "Sozzetti-A", "name": { "family": "Sozzetti", "given": "Alessandro" } }, { "id": "Kov\u00e1cs-G", "name": { "family": "Kov\u00e1cs", "given": "G\u00e9za" } }, { "id": "Everett-M-E", "name": { "family": "Everett", "given": "Mark E." }, "orcid": "0000-0002-0885-7215" }, { "id": "Baliber-N", "name": { "family": "Baliber", "given": "Nairn" } }, { "id": "Hidas-M-G", "name": { "family": "Hidas", "given": "M\u00e1rton G." } }, { "id": "Esquerdo-G-A", "name": { "family": "Esquerdo", "given": "Gilbert A." }, "orcid": "0000-0002-9789-5474" }, { "id": "Rabus-M", "name": { "family": "Rabus", "given": "Markus" } }, { "id": "Deeg-H-J", "name": { "family": "Deeg", "given": "Hans J." } }, { "id": "Belmonte-J-A", "name": { "family": "Belmonte", "given": "Juan A." } }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." } }, { "id": "Stefanik-R-P", "name": { "family": "Stefanik", "given": "Robert P." } } ] }, "title": "TrES-3: A Nearby, Massive, Transiting Hot Jupiter in a 31 Hour Orbit", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems; stars: individual (GSC 03089\u201300929, GSC 03089\u201300929); techniques: photometric; techniques: radial velocities", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2007 April 27; accepted 2007 May 14; published 2007 June 14.\n\nWe thank B. S. Gaudi for a useful discussion. We thank the\nreferee for helpful comments that improved the Letter. This material\nis based on work supported by NASA under grants\nNNG04GN74G, NNG04LG89G, NNG05GI57G, NNG05GJ29G,\nand NNH05AB88I issued through the Origins of Solar Systems\nProgram. We acknowledge support from the NASA Kepler mission\nunder cooperative agreement NCC2-1390. Work by G.A. B.\nwas supported by NASA through Hubble Fellowship Grant HSTHF-\n01170.01-A. G. K. acknowledges the support of OTKA K-60750.\n\nPublished - ODOapjl07.pdf
", "abstract": "We describe the discovery of a massive transiting hot Jupiter with a very short orbital period (1.30619 days), which we name TrES-3. From spectroscopy of the host star GSC 03089-00929, we measure T_(eff) = 5720 \u00b1 150 K, log g = 4.6 \u00b1 0.3, and v sin i < 2 km s^(-1) and derive a stellar mass of 0.90 \u00b1 0.15 M_\u2609. We estimate a planetary mass of 1.92 \u00b1 0.23 M_(Jup), based on the sinusoidal variation of our high-precision radial velocity measurements. This variation has a period and phase consistent with our transit photometry. Our spectra show no evidence of line bisector variations that would indicate a blended eclipsing binary star. From detailed modeling of our B and z photometry of the 2.5% deep transits, we determine a stellar radius 0.802 \u00b1 0.046 R_\u2609 and a planetary radius 1.295 \u00b1 0.081 R_(Jup). TrES-3 has one of the shortest orbital periods of the known transiting exoplanets, facilitating studies of orbital decay and mass loss due to evaporation, and making it an excellent target for future studies of infrared emission and reflected starlight.", "date": "2007-07-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "663", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L37-L40", "id_number": "CaltechAUTHORS:20100419-103543556", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100419-103543556", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG04GN74G" }, { "agency": "NASA", "grant_number": "NNG04LG89G" }, { "agency": "NASA", "grant_number": "NNG05GI57G" }, { "agency": "NASA", "grant_number": "NNG05GJ29G" }, { "agency": "NASA", "grant_number": "NNH05AB88I" }, { "agency": "NASA", "grant_number": "NCC2-1390" }, { "agency": "NASA", "grant_number": "HST-HF-01170.01-A" }, { "agency": "OTKA", "grant_number": "K-60750" } ] }, "doi": "10.1086/519793", "primary_object": { "basename": "ODOapjl07.pdf", "url": "https://authors.library.caltech.edu/records/9zbh4-bms24/files/ODOapjl07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "O'Donovan, Francis T.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/n0k4k-2xq40", "eprint_id": 16708, "eprint_status": "archive", "datestamp": "2023-08-22 09:18:07", "lastmod": "2023-10-19 22:29:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Alonso-R", "name": { "family": "Alonso", "given": "Roi" } }, { "id": "Brown-T-M", "name": { "family": "Brown", "given": "Timothy M." }, "orcid": "0000-0002-1793-9968" }, { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "Georgi" } }, { "id": "Dunham-E-W", "name": { "family": "Dunham", "given": "Edward W." } }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Stefanik-R-P", "name": { "family": "Stefanik", "given": "Robert P." } }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" }, { "id": "Everett-M-E", "name": { "family": "Everett", "given": "Mark E." }, "orcid": "0000-0002-0885-7215" } ] }, "title": "Outcome of Six Candidate Transiting Planets from a TrES Field in Andromeda", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems; techniques : photometric; techniques : radial velocities", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 July 22; accepted 2007 February 7.\nF. T. O'D, and D. C. thank Lynne Hillenbrand for her supervision\nof this thesis work. This material is based on work supported\nby the National Aeronautics and Space Administration\nunder grants NNG05GJ29G, NNG05GI57G, NNH05AB88I, and\nNNG04LG89G, issued through the Origins of Solar Systems\nProgram. We acknowledge support for this work from the Kepler\nmission via NASA Cooperative Agreement NCC2\u20131390. This\nresearch has made use of the SIMBAD database, operated at CDS,\nStrasbourg, France, and NASA's Astrophysics Data System Bibliographic\nServices. This publication also utilizes data products\nfrom the Two Micron All Sky Survey, which is a joint project of\nthe University of Massachusetts and the Infrared Processing and\nAnalysis Center/California Institute of Technology, funded by the\nNational Aeronautics and Space Administration and the National\nScience Foundation.\n\nPublished - ODOapj07.pdf
", "abstract": "Driven by the incomplete understanding of the formation of gas giant extrasolar planets and of their mass-radius relationship, several ground-based, wide-field photometric campaigns are searching the skies for new transiting extrasolar gas giants. As part of the Trans-atlantic Exoplanet Survey (TrES), in 2003/2004 we monitored approximately 30,000 stars (9.5 \u2264 V \u2264 15.5) in a 5.7\u00b0 \u00d7 5.7\u00b0 field in Andromeda with three telescopes over 5 months. We identified six candidate transiting planets from the stellar light curves. From subsequent follow-up observations we rejected each of these as an astrophysical false positive, i.e., a stellar system containing an eclipsing binary, whose light curve mimics that of a Jupiter-sized planet transiting a Sunlike star. We discuss here the procedures followed by the TrES team to reject false positives from our list of candidate transiting hot Jupiters. We present these candidates as early examples of the various types of astrophysical false positives found in the TrES campaign, and discuss what we learned from the analysis.", "date": "2007-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "662", "number": "1", "publisher": "American Astronomical Society", "pagerange": "658-668", "id_number": "CaltechAUTHORS:20091116-081808006", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091116-081808006", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG05GJ29G" }, { "agency": "NASA", "grant_number": "NNG05GI57G" }, { "agency": "NASA", "grant_number": "NNH05AB88I" }, { "agency": "NASA", "grant_number": "NNG04LG89G" }, { "agency": "NASA", "grant_number": "NCC2\u20131390" }, { "agency": "NSF" } ] }, "doi": "10.1086/513684", "primary_object": { "basename": "ODOapj07.pdf", "url": "https://authors.library.caltech.edu/records/n0k4k-2xq40/files/ODOapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "O'Donovan, Francis T.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/gbr29-xb779", "eprint_id": 36927, "eprint_status": "archive", "datestamp": "2023-08-22 09:12:46", "lastmod": "2024-02-02 21:07:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Richardson-L-J", "name": { "family": "Richardson", "given": "L. Jeremy" } } ] }, "title": "A Ground-based Search for Thermal Emission from the Exoplanet TrES-1", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2007 Astronomical Society of the Pacific. \n\nReceived 2007 April 19; accepted 2007 May 24; published 2007 June 12. \n\nThis work is based on observations obtained as part of program GN-2006A-Q-3 at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Particle Physics and Astronomy Research Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil) and CONICET (Argentina). We are grateful to Chad Trujillo and the entire Gemini team for their assistance throughout this process. H. A. K. was supported by a National Science Foundation Graduate Research Fellowship. L. J. R. was supported by a NASA Postdoctoral Fellowship at NASA Goddard.\n\nAccepted Version - 0705.4288.pdf
", "abstract": "Eclipsing planetary systems give us an important window on extrasolar planet atmospheres. By measuring the depth of the secondary eclipse, when the planet moves behind the star, we can estimate the strength of the thermal emission from the day side of the planet. Obtaining a ground\u2010based detection of one of these eclipses has proven to be a significant challenge, as time\u2010dependent variations in instrument throughput and atmospheric seeing and absorption overwhelm the small signal of the eclipse at infrared wavelengths. We gathered a series of simultaneous L grism spectra of the transiting planet system TrES\u20101 and a nearby comparison star of comparable brightness, allowing us to correct for these effects, in principle. Combining the data from two eclipses, we demonstrate a detection sensitivity of 0.15% in the eclipse depth relative to the stellar flux. This approaches the sensitivity required to detect the planetary emission, which theoretical models predict should lie between 0.05% and 0.1% of the stellar flux in our 2.9\u20134.3 \u03bcm bandpass. We explore the factors that ultimately limit the precision of this technique, and discuss potential avenues for future improvements.", "date": "2007-06", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "119", "number": "856", "publisher": "Astronomical Society of the Pacific", "pagerange": "616-622", "id_number": "CaltechAUTHORS:20130214-104217298", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130214-104217298", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NASA Postdoctoral Fellowship" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/520098", "primary_object": { "basename": "0705.4288.pdf", "url": "https://authors.library.caltech.edu/records/gbr29-xb779/files/0705.4288.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Knutson, Heather A.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zhmxk-qg426", "eprint_id": 36636, "eprint_status": "archive", "datestamp": "2023-08-19 20:11:37", "lastmod": "2024-02-02 21:06:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Allen-L-E", "name": { "family": "Allen", "given": "Lori E." } }, { "id": "Fortney-J-J", "name": { "family": "Fortney", "given": "Jonathan J." }, "orcid": "0000-0002-9843-4354" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas B." }, "orcid": "0000-0001-6129-5699" }, { "id": "Showman-A-P", "name": { "family": "Showman", "given": "Adam P." } }, { "id": "Cooper-C-S", "name": { "family": "Cooper", "given": "Curtis S." } }, { "id": "Megeath-S-T", "name": { "family": "Megeath", "given": "S. Thomas" }, "orcid": "0000-0001-7629-3573" } ] }, "title": "A map of the day\u2013night contrast of the extrasolar planet HD 189733b", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2007 Nature Publishing Group, a division of Macmillan Publishers Limited. \n\nReceived 8 February; accepted 23 March 2007. \n\nWe thank J. Winn for sharing data from a recent paper describing the behaviour of the spots on the star, and D. Sasselov and E. Miller-Ricci for discussions on the properties of these spots. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We are grateful to the entire Spitzer team for their assistance throughout this process. H.A.K. was supported by a National Science Foundation Graduate Research Fellowship.\n\nAccepted Version - 0705.0993.pdf
", "abstract": "'Hot Jupiter' extrasolar planets are expected to be tidally locked because they are close (<0.05 astronomical units, where 1 au is the average Sun\u2013Earth distance) to their parent stars, resulting in permanent daysides and nightsides. By observing systems where the planet and star periodically eclipse each other, several groups have been able to estimate the temperatures of the daysides of these planets. A key question is whether the atmosphere is able to transport the energy incident upon the dayside to the nightside, which will determine the temperature at different points on the planet's surface. Here we report observations of HD 189733, the closest of these eclipsing planetary systems, over half an orbital period, from which we can construct a 'map' of the distribution of temperatures. We detected the increase in brightness as the dayside of the planet rotated into view. We estimate a minimum brightness temperature of 973 \u00b1 33 K and a maximum brightness temperature of 1,212 \u00b1 11 K at a wavelength of 8 mum, indicating that energy from the irradiated dayside is efficiently redistributed throughout the atmosphere, in contrast to a recent claim for another hot Jupiter. Our data indicate that the peak hemisphere-integrated brightness occurs 16 \u00b1 6\u00b0 before opposition, corresponding to a hotspot shifted east of the substellar point. The secondary eclipse (when the planet moves behind the star) occurs 120 \u00b1 24 s later than predicted, which may indicate a slightly eccentric orbit.", "date": "2007-05-10", "date_type": "published", "publication": "Nature", "volume": "447", "number": "7141", "publisher": "Nature Publishing Group", "pagerange": "183-186", "id_number": "CaltechAUTHORS:20130128-154306263", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130128-154306263", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF Graduate Research Fellowship" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/nature05782", "primary_object": { "basename": "0705.0993.pdf", "url": "https://authors.library.caltech.edu/records/zhmxk-qg426/files/0705.0993.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Knutson, Heather A.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/hs3kg-y6m18", "eprint_id": 18168, "eprint_status": "archive", "datestamp": "2023-08-22 08:50:48", "lastmod": "2023-10-20 15:49:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "C. J." }, "orcid": "0000-0003-4072-169X" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "D." }, "orcid": "0000-0002-9003-484X" }, { "id": "Burrows-A-S", "name": { "family": "Burrows", "given": "A. S." }, "orcid": "0000-0002-3099-5024" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Stauffer-J-R", "name": { "family": "Stauffer", "given": "J. R." }, "orcid": "0000-0003-3595-7382" }, { "id": "Meadows-V", "name": { "family": "Meadows", "given": "V." } }, { "id": "Van-Cleve-J", "name": { "family": "Van Cleve", "given": "J." } }, { "id": "Levine-D-A", "name": { "family": "Levine", "given": "D." } } ] }, "title": "A Spitzer Spectrum of the Exoplanet HD 189733b", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing; planetary systems; stars: individual (HD 189733, HD 189733)", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2007 January 19; accepted 2007 February 12; published 2007 February 23.\n\nWe are grateful to an anonymous referee for several suggestions\nthat significantly improved the analysis and presentation\nof this work. This work is based on observations made\nwith the Spitzer Space Telescope, which is operated by the Jet\nPropulsion Laboratory, California Institute of Technology, under\na contract with NASA. Support for this work was provided\nby NASA through an award issued by JPL/Caltech. This study\nwas supported in part by NASA grant NNGO4GL22G and\nthrough the NASA Astrobiology Institute under Cooperative\nAgreement CAN-02-OSS-02 issued through the Office of\nSpace Science.\n\nPublished - GRIapjl07.pdf
", "abstract": "We report on the measurement of the 7.5-14.7 \u03bcm spectrum for the transiting extrasolar giant planet HD 189733b using the Infrared Spectrograph on the Spitzer Space Telescope. Although the observations comprise only 12 hr of telescope time, the continuum is well measured and has a flux ranging from 0.6 to 1.8 mJy over the wavelength range, or 0.49% \u00b1 0.02% of the flux of the parent star. The variation in the measured fractional flux is very nearly flat over the entire wavelength range and shows no indication of significant absorption by water or methane, in contrast with the predictions of most atmospheric models. Models with strong day/night differences appear to be disfavored by the data, suggesting that heat redistribution to the night side of the planet is highly efficient.", "date": "2007-04-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "658", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L115-L118", "id_number": "CaltechAUTHORS:20100506-122421966", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100506-122421966", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNGO4GL22G" }, { "agency": "NASA", "grant_number": "CAN-02-OSS-02" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/513741", "primary_object": { "basename": "GRIapjl07.pdf", "url": "https://authors.library.caltech.edu/records/hs3kg-y6m18/files/GRIapjl07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Grillmair, C. J.; Charbonneau, D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7354s-9xn42", "eprint_id": 37030, "eprint_status": "archive", "datestamp": "2023-08-22 08:09:28", "lastmod": "2024-02-02 21:07:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Noyes-R-W", "name": { "family": "Noyes", "given": "Robert W." } }, { "id": "Brown-T-M", "name": { "family": "Brown", "given": "Timothy M." }, "orcid": "0000-0002-1793-9968" }, { "id": "Gilliland-R-L", "name": { "family": "Gilliland", "given": "Ronald L." }, "orcid": "0000-0002-1554-5578" } ] }, "title": "Using Stellar Limb-Darkening to Refine the Properties of HD 209458b", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing; planetary systems; stars: individual (HD 209458); techniques: photometric", "note": "\u00a9 2007 American Astronomical Society. Received 2006 March 20; accepted 2006 October 5. We are grateful to R. Kurucz for his assistance in calculating the limb-darkening for HD 209458. Support for program number HST-GO-09447 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by AURA under NASA contract NAS5-26555. H. K. was supported by a National Science Foundation Graduate Research Fellowship.\n\nPublished - 0004-637X_655_1_564.pdf
", "abstract": "We use multiband photometry to refine estimates for the planetary radius and orbital inclination of the transiting planet system HD 209458. We gathered 1066 spectra over four distinct transits with the STIS spectrometer on the Hubble Space Telescope using two gratings with a resolution R = 1500 and a combined wavelength range of 290-1030 nm. We divide the spectra into 10 spectrophotometric bandpasses, five for each grating, of equal wavelength span within each grating, and fit a transit curve over all bandpasses simultaneously. In our fit we use theoretical values for the stellar limb-darkening to further constrain the planetary radius. We find that the radius of HD 209458b is (1.320 \u00b1 0.025)R_(Jup), which is a factor of 2 more precise than current estimates. We also obtain improved estimates for the orbital period P and time of center of transit T_C. Although in principle the photon-limited precision of the STIS data should allow us to measure the timing of individual transits to a precision of 2-7 s, we find that uncertainties in the stellar limb-darkening coefficients and residual noise in the data degrade these measurements to a typical precision of \u00b114 s. Within this level of error, we find no significant variations in the timing of the eight events examined in this work.", "date": "2007-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "655", "number": "1", "publisher": "American Astronomical Society", "pagerange": "564-575", "id_number": "CaltechAUTHORS:20130220-143513269", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130220-143513269", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09447" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "Space Telescope Science Institute" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/510111", "primary_object": { "basename": "0004-637X_655_1_564.pdf", "url": "https://authors.library.caltech.edu/records/7354s-9xn42/files/0004-637X_655_1_564.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Knutson, Heather A.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/kj31j-mx972", "eprint_id": 37178, "eprint_status": "archive", "datestamp": "2023-08-22 07:57:07", "lastmod": "2024-02-02 21:11:56", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" }, "orcid": "0000-0001-5727-4094" }, { "id": "Agol-E", "name": { "family": "Agol", "given": "Eric" }, "orcid": "0000-0002-0802-9145" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Cowan-N-B", "name": { "family": "Cowan", "given": "Nicolas" }, "orcid": "0000-0001-6129-5699" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather" }, "orcid": "0000-0002-5375-4725" }, { "id": "Marengo-M", "name": { "family": "Marengo", "given": "Massimo" }, "orcid": "0000-0001-9910-9230" } ] }, "title": "Observations of Extrasolar Planets During the non-Cryogenic Spitzer Space Telescope Mission", "ispublished": "unpub", "full_text_status": "public", "keywords": "astronomical observatories; astronomical telescopes; extrasolar planets; astronomical photometry", "note": "\u00a9 2007 American Institute of Physics.\n\nWe thank the Spitzer Science Center for the opportunity to consider and discuss the potential for exoplanet science during the warm mission. We are grateful to Josh Winn and\nAndy Gould for helpful conversations and remarks regarding the relative merits of of ground-based vs. space-borne photometry. We also acknowledge informative conversations\nwith Greg Laughlin on the effects of heating in eccentric orbits.\n\nPublished - APC000089.pdf
", "abstract": "Precision infrared photometry from Spitzer has enabled the first direct studies of light from extrasolar planets, via observations at secondary eclipse in transiting systems. Current Spitzer results include the first longitudinal temperature map of an extrasolar planet, and the first spectra of their atmospheres. Spitzer has also measured a temperature and precise radius for the first transiting Neptune\u2010sized exoplanet, and is beginning to make precise transit timing measurements to infer the existence of unseen low mass planets. The lack of stellar limb darkening in the infrared facilitates precise radius and transit timing measurements of transiting planets. Warm Spitzer will be capable of a precise radius measurement for Earth\u2010sized planets transiting nearby M\u2010dwarfs, thereby constraining their bulk composition. It will continue to measure thermal emission at secondary eclipse for transiting hot Jupiters, and be able to distinguish between planets having broad band emission vs. absorption spectra. It will also be able to measure the orbital phase variation of thermal emission for close\u2010in planets, even non\u2010transiting planets, and these measurements will be of special interest for planets in eccentric orbits. Warm Spitzer will be a significant complement to Kepler, particularly as regards transit timing in the Kepler field. In addition to studying close\u2010in planets, Warm Spitzer will have significant application in sensitive imaging searches for young planets at relatively large angular separations from their parent stars.", "date": "2007", "date_type": "published", "publisher": "American Institute of Physics", "place_of_pub": "Melville, NY", "pagerange": "89-100", "id_number": "CaltechAUTHORS:20130227-111026285", "isbn": "978-0-7354-0457-1", "book_title": "The Science Opportunities of the Warm Spitzer Mission Workshop", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130227-111026285", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "contributors": { "items": [ { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L. J." } }, { "id": "Silbermann-N-A", "name": { "family": "Silbermann", "given": "N. A." } } ] }, "doi": "10.1063/1.2806789", "primary_object": { "basename": "APC000089.pdf", "url": "https://authors.library.caltech.edu/records/kj31j-mx972/files/APC000089.pdf" }, "resource_type": "book_section", "pub_year": "2007", "author_list": "Deming, Drake; Agol, Eric; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/kar9t-s4858", "eprint_id": 20681, "eprint_status": "archive", "datestamp": "2023-08-19 19:14:55", "lastmod": "2024-01-13 00:05:51", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "F. T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "D." }, "orcid": "0000-0002-9003-484X" } ] }, "title": "TrES Exoplanets and False Positives: Finding the Needle in the Haystack", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2007 Astronomical Society of the Pacific. We thank Lynne Hillenbrand for her continued support of this thesis work. This material is based on work supported by the National\nAeronautics and Space Administration under grant NNG05GJ29G, issued through the Origins of Solar Systems Program.\n\nPublished - ODonovan2007p9212Transiting_Extrasolar_Planets_Workshop.pdf
", "abstract": "Our incomplete understanding of the formation of gas giants and\nof their mass\u2013radius relationship has motivated ground\u2013based, wide\u2013field surveys\nfor new transiting extrasolar giant planets. Yet, astrophysical false positives\nhave dominated the yield from these campaigns. Astronomical systems where\nthe light from a faint eclipsing binary and a bright star is blended, producing\na transit\u2013like light curve, are particularly difficult to eliminate. As part of the\nTrans\u2013atlantic Exoplanet Survey, we have encountered numerous false positives\nand have developed a procedure to reject them. We present examples of these\nfalse positives, including the blended system GSC 03885\u201300829 which we showed\nto be a K dwarf binary system superimposed on a late F dwarf star. This transit\ncandidate in particular demonstrates the careful analysis required to identify\nastrophysical false positives in a transit survey. From amongst these impostors,\nwe have found two transiting planets. We discuss our follow-up observations of\nTrES\u20132, the first transiting planet in the Kepler field.", "date": "2007", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco", "pagerange": "58-63", "id_number": "CaltechAUTHORS:20101105-090929145", "isbn": "978-1-583812-34-1", "book_title": "Transiting Extrasolar Planets Workshop", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101105-090929145", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG05GJ29G" } ] }, "contributors": { "items": [ { "id": "Afonso-C", "name": { "family": "Afonso", "given": "C." } }, { "id": "Weldrake-D", "name": { "family": "Weldrake", "given": "D." } }, { "id": "Henning-Th", "name": { "family": "Henning", "given": "Th." } } ] }, "primary_object": { "basename": "ODonovan2007p9212Transiting_Extrasolar_Planets_Workshop.pdf", "url": "https://authors.library.caltech.edu/records/kar9t-s4858/files/ODonovan2007p9212Transiting_Extrasolar_Planets_Workshop.pdf" }, "resource_type": "book_section", "pub_year": "2007", "author_list": "O'Donovan, F. T. and Charbonneau, D." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/8mxb9-s3908", "eprint_id": 24032, "eprint_status": "archive", "datestamp": "2023-08-22 07:52:11", "lastmod": "2023-10-23 20:15:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Morales-Calder\u00f3n-M", "name": { "family": "Morales-Calder\u00f3n", "given": "M." } }, { "id": "Stauffer-J-R", "name": { "family": "Stauffer", "given": "J. R." }, "orcid": "0000-0003-3595-7382" }, { "id": "Kirkpatrick-J-D", "name": { "family": "Kirkpatrick", "given": "J. Davy" }, "orcid": "0000-0003-4269-260X" }, { "id": "Carey-S-J", "name": { "family": "Carey", "given": "S." }, "orcid": "0000-0002-0221-6871" }, { "id": "Gelino-C-R", "name": { "family": "Gelino", "given": "C. R." } }, { "id": "Barrado-y-Navascu\u00e9s-D", "name": { "family": "Barrado y Navascu\u00e9s", "given": "D." } }, { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "L." }, "orcid": "0000-0001-6381-515X" }, { "id": "Lowrance-P-J", "name": { "family": "Lowrance", "given": "P." }, "orcid": "0000-0001-8014-0270" }, { "id": "Marley-M-S", "name": { "family": "Marley", "given": "M. S." }, "orcid": "0000-0002-5251-2943" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "D." }, "orcid": "0000-0002-9003-484X" }, { "id": "Patten-B-M", "name": { "family": "Patten", "given": "B. M." } }, { "id": "Megeath-S-T", "name": { "family": "Megeath", "given": "S. T." }, "orcid": "0000-0001-7629-3573" }, { "id": "Buzasi-D", "name": { "family": "Buzasi", "given": "D." } } ] }, "title": "A Sensitive Search for Variability in Late L Dwarfs: The Quest for Weather", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: individual (DENIS-P J0255\u20134700, 2MASS J0908+5032, 2MASS J2244+2043); stars: low-mass, brown dwarfs; stars: variables: other", "note": "Copyright is not claimed for this article.\n\nReceived 2006 June 2; accepted 2006 July 21.\n\nWe acknowledge use of the L and T dwarf archives at http://dwarfarchives.org, maintained by two of us (J. D. K. and C.R.G.) and Adam Burgasser. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. M. M.-C. also acknowledges the funding provided by the Spitzer Visiting Graduate Students Fellowship Program.\nFacilities: Spitzer ( IRAC)\n\nPublished - MORapj06.pdf
", "abstract": "We have conducted a photometric monitoring program of three field late L brown dwarfs (DENIS-P J0255-4700, 2MASS J0908+5032, and 2MASS J2244+2043) looking for evidence of nonaxisymmetric structure or temporal variability in their photospheres. The observations were performed using Spitzer IRAC 4.5 and 8 \u03bcm bandpasses and were designed to cover at least one rotational period of each object; 1 \u03c3 rms uncertainties of less than 3 mmag at 4.5 \u03bcm and around 9 mmag at 8 \u03bcm were achieved. Two out of the three objects studied exhibit some modulation in their light curves at 4.5 \u03bcm\u2014but not 8 \u03bcm\u2014with periods of 7.4 hr (DENIS 0255) and 4.6 hr (2MA 2244) and peak-to-peak amplitudes of 10 and 8 mmag. Although the lack of detectable 8 \u03bcm variation suggests an instrumental origin for the detected variations, the data may nevertheless still be consistent with intrinsic variability, since the shorter wavelength IRAC bandpasses probe more deeply into late L dwarf atmospheres than the longer wavelengths. A cloud feature occupying a small percentage (1%-2%) of the visible hemisphere could account for the observed amplitude of variation. If, instead, the variability is indeed instrumental in origin, then our nonvariable L dwarfs could be either completely covered with clouds or objects whose clouds are smaller and uniformly distributed. Such scenarios would lead to very small photometric variations. Follow-up IRAC photometry at 3.6 and 5.8 \u03bcm bandpasses should distinguish between the two cases. In any event, the present observations provide the most sensitive search to date for structure in the photospheres of late L dwarfs at mid-IR wavelengths, and our photometry provides stringent upper limits to the extent to which the photospheres of these transition L dwarfs are structured.", "date": "2006-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "653", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1454-1463", "id_number": "CaltechAUTHORS:20110616-112409859", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110616-112409859", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Spitzer Visiting Graduate Student Fellowship" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "primary_object": { "basename": "MORapj06.pdf", "url": "https://authors.library.caltech.edu/records/8mxb9-s3908/files/MORapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Morales-Calder\u00f3n, M.; Stauffer, J. R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/tmgek-rrd17", "eprint_id": 12965, "eprint_status": "archive", "datestamp": "2023-08-22 07:45:21", "lastmod": "2023-10-17 21:40:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Holman-M-J", "name": { "family": "Holman", "given": "Matthew J." }, "orcid": "0000-0002-1139-4880" }, { "id": "Winn-J-N", "name": { "family": "Winn", "given": "Joshua N." }, "orcid": "0000-0002-4265-047X" }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Bakos-G-\u00c1", "name": { "family": "Bakos", "given": "G\u00e1sp\u00e1r A." }, "orcid": "0000-0001-7204-6727" }, { "id": "Esquerdo-G-A", "name": { "family": "Esquerdo", "given": "Gilbert A." }, "orcid": "0000-0002-9789-5474" }, { "id": "Hergenrother-C", "name": { "family": "Hergenrother", "given": "Carl" } }, { "id": "Everett-M-E", "name": { "family": "Everett", "given": "Mark E." }, "orcid": "0000-0002-0885-7215" }, { "id": "P\u00e1l-P", "name": { "family": "P\u00e1l", "given": "Andr\u00e1s" } } ] }, "title": "The Transit Light Curve Project. I. Four Consecutive Transits of the Exoplanet XO-1b", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems; stars: individual (GSC 02041-01657); techniques: photometric", "note": "\u00a9 2006. The American Astronomical Society. \n\nReceived 2006 June 19; accepted 2006 July 26. Print publication: Issue 2 (2006 December 1). \n\nWe thank T. Spahr for swapping telescope nights on short notice, E. Falco for accommodating our observing schedule changes, S. Gaudi for lengthy discussions about the MCMC method and numerous suggestions for improving the manuscript, J. Fern\u00e1ndez for helpful discussions about fitting transit light curves, G. Torres for help with stellar isochrones, and R. Kurucz for calculations of limb-darkening coefficients. We thank A. Soderberg, S. B. Cenko, and E. O. Ofek for their help in obtaining the Palomar 1.5 m photometry. We also thank the anonymous referee for an exceptionally careful review of the manuscript. KeplerCam was developed with partial support from the Kepler mission under NASA Cooperative Agreement NCC2-1390 (PI: D. Latham), and the KeplerCam observations described in this paper were partly supported by grants from the Kepler mission to SAO and PSI. The TopHAT observations were supported by NASA grant NNG04GN74G. Work by G.B. was supported by NASA through grant HST-HF-01170.01-A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Work by F.T.O'D and D.C. was supported by NASA under grant NNG05GJ29G, issued through the Origins of Solar Systems Program.\n\nPublished - HOLapj06.pdf
", "abstract": "We present RIz photometry of four consecutive transits of the newly discovered exoplanet XO-1b. We improve on the estimates of the transit parameters, finding the planetary radius to be RP = 1.184 +0.028 -0.018 RJ, and the stellar radius to be R* = 0.928 +0.018 -0.013 R\u2609, assuming a stellar mass of M* = (1.00 \u00b1 0.03) M\u2609. The uncertainties in the planetary and stellar radii are dominated by the uncertainty in the stellar mass. These uncertainties increase by a factor of 2-3 if a more conservative uncertainty of 0.10 M\u2609 is assumed for the stellar mass. Our estimate of the planetary radius is smaller than that reported by McCullough and coworkers, and the resulting estimate for the mean density of XO-1b is intermediate between that of the low-density planet HD 209458b and the higher density planets TrES-1 and HD 189733b. The timings of the transits have an accuracy ranging from 0.2 to 2.5 minutes and are marginally consistent with a uniform period.", "date": "2006-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "652", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1715-1723", "id_number": "CaltechAUTHORS:HOLapj06", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:HOLapj06", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NCC2-1390" }, { "agency": "NASA", "grant_number": "NNG04GN74G" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01170.01-A" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NASA", "grant_number": "NNG05GJ29G" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Space Telescope Science Institute" } ] }, "doi": "10.1086/508155", "primary_object": { "basename": "HOLapj06.pdf", "url": "https://authors.library.caltech.edu/records/tmgek-rrd17/files/HOLapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Holman, Matthew J.; Winn, Joshua N.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6mhsf-beq45", "eprint_id": 24279, "eprint_status": "archive", "datestamp": "2023-08-22 07:11:01", "lastmod": "2023-10-23 20:26:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." }, "orcid": "0000-0002-4858-6106" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "Georgi" } }, { "id": "Dunham-E-W", "name": { "family": "Dunham", "given": "Edward W." } }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Torres-G", "name": { "family": "Torres", "given": "Guillermo" }, "orcid": "0000-0002-5286-0251" }, { "id": "Sozzetti-A", "name": { "family": "Sozzetti", "given": "Alessandro" } }, { "id": "Brown-T-M", "name": { "family": "Brown", "given": "Timothy M." }, "orcid": "0000-0002-1793-9968" }, { "id": "Trauger-J-T", "name": { "family": "Trauger", "given": "John T." } }, { "id": "Belmont-J-A", "name": { "family": "Belmonte", "given": "Juan A." } }, { "id": "Rabus-M", "name": { "family": "Rabus", "given": "Markus" } }, { "id": "Almenara-J-M", "name": { "family": "Almenara", "given": "Jos\u00e9 M." } }, { "id": "Alonso-R", "name": { "family": "Alonso", "given": "Roi" } }, { "id": "Deeg-H-J", "name": { "family": "Deeg", "given": "Hans J." } }, { "id": "Esquerdo-G-A", "name": { "family": "Esquerdo", "given": "Gilbert A." }, "orcid": "0000-0002-9789-5474" }, { "id": "Falco-E-E", "name": { "family": "Falco", "given": "Emilio E." } }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." } }, { "id": "Roussanova-A", "name": { "family": "Roussanova", "given": "Anna" } }, { "id": "Stefanik-R-P", "name": { "family": "Stefanik", "given": "Robert P." } }, { "id": "Winn-J-N", "name": { "family": "Winn", "given": "Joshua N." }, "orcid": "0000-0002-4265-047X" } ] }, "title": "TrES-2: The First Transiting Planet in the Kepler Field", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems\u2014stars: individual (GSC 03549-02811); techniques: photometric; techniques: radial velocities", "note": "\u00a9 2006 American Astronomical Society.\n\nReceived 2006 August 21; accepted 2006 September 12; published 2006 October 16.\nSome of the data presented herein were obtained at the W. M. Keck Observatory,\nwhich is operated as a scientific partnership among Caltech, the University\nof California, and NASA. The Observatory was made possible by the\ngenerous financial support of the W. M. Keck Foundation.\nWe sincerely thank R. Brucato, M. Doyle, K. Dunscombe, R.\nEllis, B. Gordon, J. Henning, L. Kroll, S. Kunsman, J. Mueller, H. Petrie, A. Pickles, N. Scoville, M. Sweet, R. Thicksten, G. van Idsinga, R. Wetzel, and D. Zieber for their assistance with the Sleuth instrument. We thank the referee, S. Gaudi, for his detailed comments that helped improve the Letter. We are indebted to S. Fern\u00e1ndez Acosta, who accommodated the unscheduled transit observation at the IAC80, which is operated by the IAC in its Observatorio del Teide. This material is based on work supported by NASA under grants NNG 05GJ29G, NNG05GI57G, NNH 05AB88I, and NNG 04LG89G, issued through the Origins of Solar Systems Program. We acknowledge support from the NASA Kepler mission.\n\nPublished - ODOapjl06.pdf
", "abstract": "We announce the discovery of the second transiting hot Jupiter discovered by the Trans-atlantic Exoplanet Survey. The planet, which we dub TrES-2, orbits the nearby star GSC 03549-02811 every 2.47063 days. From high-resolution spectra, we determine that the star has T_eff = 5960 \u00b1 100 K and log g = 4.4 \u00b1 0.2, implying a spectral type of G0 V and a mass of 1.08^(+0.11)_(-0.05) M_\u2609. High-precision radial velocity measurements confirm a sinusoidal variation with the period and phase predicted by the photometry, and rule out the presence of line bisector variations that would indicate that the spectroscopic orbit is spurious. We estimate a planetary mass of 1.28^(+0.09)_(-0.04)M_Jup. We model B, r, R, and I photometric time series of the 1.4% deep transits and find a planetary radius of 1.24^(+0.09)_(-0.06) R_Jup. This planet lies within the field of view of the NASA Kepler mission, ensuring that hundreds of upcoming transits will be monitored with exquisite precision and permitting a host of unprecedented investigations.", "date": "2006-11-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "651", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L61-L64", "id_number": "CaltechAUTHORS:20110630-112850465", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110630-112850465", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Kepler Mission" } ] }, "doi": "10.1086/509123", "primary_object": { "basename": "ODOapjl06.pdf", "url": "https://authors.library.caltech.edu/records/6mhsf-beq45/files/ODOapjl06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "O'Donovan, Francis T.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/gpvvy-1q090", "eprint_id": 36627, "eprint_status": "archive", "datestamp": "2023-08-22 07:02:00", "lastmod": "2024-02-02 21:06:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bakos-G-\u00c1", "name": { "family": "Bakos", "given": "G. \u00c1." }, "orcid": "0000-0001-7204-6727" }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "H." }, "orcid": "0000-0002-5375-4725" }, { "id": "Pont-F", "name": { "family": "Pont", "given": "F." }, "orcid": "0000-0003-0076-5444" }, { "id": "Moutou-C", "name": { "family": "Moutou", "given": "C." } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "D." }, "orcid": "0000-0002-9003-484X" }, { "id": "Shporer-A", "name": { "family": "Shporer", "given": "A." }, "orcid": "0000-0002-1836-3120" }, { "id": "Bouchy-F", "name": { "family": "Bouchy", "given": "F." } }, { "id": "Everett-M-E", "name": { "family": "Everett", "given": "M." }, "orcid": "0000-0002-0885-7215" }, { "id": "Hergenrother-C", "name": { "family": "Hergenrother", "given": "C." } }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "D. W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Mayor-M", "name": { "family": "Mayor", "given": "M." } }, { "id": "Mazeh-T", "name": { "family": "Mazeh", "given": "T." } }, { "id": "Noyes-R-W", "name": { "family": "Noyes", "given": "R. W." } }, { "id": "Queloz-D", "name": { "family": "Queloz", "given": "D." }, "orcid": "0000-0002-3012-0316" }, { "id": "P\u00e1l-A", "name": { "family": "P\u00e1l", "given": "A." } }, { "id": "Udry-S", "name": { "family": "Udry", "given": "S." } } ] }, "title": "Refined Parameters of the Planet Orbiting HD 189733", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems \u2014 stars: individual (HD 189733)", "note": "\u00a9 2006 American Astronomical Society. Received 2006 March 8; accepted 2006 May 18. Part of this work was funded by NASA grant NNG04GN74G. Work by G. \u00c1 . B. was supported by NASA through grant HST-HF-01170.01-A (Hubble Fellowship). H. K. is supported by a National Science Foundation Graduate Research Fellowship. D. W. L. thanks the Kepler mission for support through NASA Cooperative Agreement NCC2-1390. A. P. wishes to acknowledge the hospitality of the Harvard-Smithsonian Center for Astrophysics, where part of this work has been carried out. Work of A. P. was also supported by Hungarian OTKA grant T-038437. Research of T. M. and A. S.was partially supported by the German-Israeli Foundation for Scientific Research and Development. This publication makes use of data products from the Two Micron All Sky Survey (2MASS). We thank M. Hicken and R. Kirshner for\nswapping nights on the FLWO 1.2 m telescope on short notice.\n\nPublished - 0004-637X_650_2_1160.pdf
", "abstract": "We report on the BVRI multiband follow-up photometry of the transiting extrasolar planet HD 189733b. We revise the transit parameters and find a planetary radius of R_P = 1.154 \u00b1 0.033R_J and an inclination of i_P = 85\u00ba.79 \u00b1 0\u00ba.24. The new density (~1 g cm^(-3)) is significantly higher than the former estimate (~0.75 g cm^(-3)); this shows that from the current sample of nine transiting planets, only HD 209458 (and possibly OGLE-10b) have anomalously large radii and low densities. We note that due to the proximity of its parent star, HD 189733b currently has one of the most precise radius determinations among extrasolar planets. We calculate new ephemerides, P = 2.218573 \u00b1 0.000020 days and T_0 = 2453629.39420 \u00b1 0.00024 (HJD), and estimate the timing offsets of the 11 distinct transits with respect to the predictions of a constant orbital period, which can be used to reveal the presence of additional planets in the system.", "date": "2006-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "650", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1160-1171", "id_number": "CaltechAUTHORS:20130128-130906097", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130128-130906097", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG04GN74G" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01170.01-A" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NASA", "grant_number": "NCC2-1390" }, { "agency": "Hungarian Scientific Research Fund (OTKA)", "grant_number": "T-038437" }, { "agency": "German-Israeli Foundation for Scientific Research and Development" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/506316", "primary_object": { "basename": "0004-637X_650_2_1160.pdf", "url": "https://authors.library.caltech.edu/records/gpvvy-1q090/files/0004-637X_650_2_1160.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Bakos, G. \u00c1.; Knutson, H.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qy2qm-jeb92", "eprint_id": 36284, "eprint_status": "archive", "datestamp": "2023-08-22 05:08:05", "lastmod": "2024-02-02 21:05:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fischer-D-A", "name": { "family": "Fischer", "given": "Debra A." }, "orcid": "0000-0003-2221-0861" }, { "id": "Laughlin-G-P", "name": { "family": "Laughlin", "given": "Gregory" }, "orcid": "0000-0002-3253-2621" }, { "id": "Marcy-G-W", "name": { "family": "Marcy", "given": "Geoffrey W." }, "orcid": "0000-0002-2909-0113" }, { "id": "Butler-R-P", "name": { "family": "Butler", "given": "R. Paul" } }, { "id": "Vogt-S-S", "name": { "family": "Vogt", "given": "Steven S." } }, { "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "orcid": "0000-0001-9808-7172" }, { "id": "Henry-G-W", "name": { "family": "Henry", "given": "Gregory W." }, "orcid": "0000-0003-4155-8513" }, { "id": "McCarthy-C", "name": { "family": "McCarthy", "given": "Chris" } }, { "id": "Ammons-M", "name": { "family": "Ammons", "given": "Mark" } }, { "id": "Robinson-S", "name": { "family": "Robinson", "given": "Sarah" } }, { "id": "Strader-J", "name": { "family": "Strader", "given": "Jay" }, "orcid": "0000-0002-1468-9668" }, { "id": "Valenti-J-A", "name": { "family": "Valenti", "given": "Jeff A." }, "orcid": "0000-0003-3305-6281" }, { "id": "McCullough-P-R", "name": { "family": "McCullough", "given": "P. R." }, "orcid": "0000-0001-9165-9799" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Haislip-J", "name": { "family": "Haislip", "given": "Joshua" } }, { "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725" }, { "id": "Reichart-D-E", "name": { "family": "Reichart", "given": "Daniel E." }, "orcid": "0000-0002-5060-3673" }, { "id": "McGee-P", "name": { "family": "McGee", "given": "Padric" } }, { "id": "Monard-B", "name": { "family": "Monard", "given": "Berto" } }, { "id": "Wright-J-T", "name": { "family": "Wright", "given": "Jason T." }, "orcid": "0000-0001-6160-5888" }, { "id": "Ida-Shigeru", "name": { "family": "Ida", "given": "Shigeru" } }, { "id": "Sato-Bun'ei", "name": { "family": "Sato", "given": "Bun'ei" } }, { "id": "Minniti-D", "name": { "family": "Minniti", "given": "Dante" }, "orcid": "0000-0002-7064-099X" } ] }, "title": "The N2K Consortium. III. Short-Period Planets Orbiting HD 149143 and HD 109749", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2006 American Astronomical Society. \n\nReceived 2005 September 6; accepted 2005 October 3. \n\nBased on observations obtained at the W. M. Keck Observatory, which is\noperated as a scientific partnership among the California Institute of Technology,\nthe University of California, and the National Aeronautics and Space\nAdministration (NASA). The Observatory was made possible by the generous\nfinancial support of the W. M. Keck Foundation. The authors wish to recognize\nand acknowledge the very significant cultural role and reverence that the summit\nof Mauna Kea has always had within the indigenous Hawaiian community. We\nare most fortunate to have the opportunity to conduct observations from this\nmountain. Keck time has been granted by the National Optical Astronomy\nObservatory (NOAO) and NASA.\n\n\nWe gratefully acknowledge the dedication and support of the Keck Observatory staff, in particular Grant Hill for support with\nHIRES. We thank Rebeccah Winnick (at Yale University) for\nscheduling the SMARTS observations. We thank the NOAO and\nNASA telescope assignment committees for generous allocations of telescope time. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to NASA through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank the Michaelson Science Center for travel support and support through the KDPA program. D. A. F. is a Cottrell Science Scholar of Research Corporation. We acknowledge support from NASA grant NNG05G164G (to D. A. F.); NASA grant NCC5-511 and NSF grant HRD-9706268 (to G. W. H.); NASA grant NAG5-75005 (to G. W. M.); NSF grant AST 99-88358 and NASA grant NAG5-4445 (to S. S. V.); NASA grant NAG5-13285 to P. B.; and NASA grant NNA04CC99A (to G. L.). D. M. is supported by FONDAPN. 15010003.D. E.R. gratefully acknowledges support from NSF's MRI, CAREER, PREST, and REU programs, NASA's APRA, Swift GI, and IDEAS programs, and especially Leonard Goodman and Henry Cox. Work by H. A. K. was supported by a National Science Foundation Graduate Research Fellowship. This research has made use of the Simbad database, operated at CDS, Strasbourg, France.\n\nPublished - 0004-637X_637_2_1094.pdf
", "abstract": "We report the detection of two short-period planets discovered at Keck Observatory. HD 149143 is a metal-rich G0 IV star with a planet of M sin i = 1.33M_J and an orbital radius of 0.053 AU. The best-fit Keplerian model has an orbital period, P = 4.072 days, semivelocity amplitude, K = 149.6 m s^(-1), and eccentricity, e = 0.016 \u00b1 0.01. The host star is chromospherically inactive and metal-rich, with [Fe/H] = 0.26. Based on the T_(eff) and stellar luminosity, we derive a stellar radius of 1.49 R_\u2609. Photometric observations of HD 149143 were carried out using the automated photometric telescopes at Fairborn Observatory. HD 149143 is photometrically constant over the radial velocity period to 0.0003 \u00b1 0.0002 mag, supporting the existence of the planetary companion. No transits were detected down to a photometric limit of approximately 0.02%, eliminating transiting planets with a variety of compositions and constraining the orbital inclination to less than 83\u00b0. A short-period planet was also detected around HD 109749, a G3 IV star. HD 109749 is chromospherically inactive, with [Fe/H] = 0.25 and a stellar radius of 1.24. The radial velocities for HD 109749 are modeled by a Keplerian with P = 5.24 days and K = 28.7 m s^(-1). The inferred planet mass is M sin i = 0.28M_J and the semimajor axis of this orbit is 0.0635 AU. Photometry of HD 109749 was obtained with the SMARTS consortium telescope, the PROMPT telescope, and by transitsearch.org observers in Adelaide and Pretoria. These observations did not detect a decrement in the brightness of the host star at the predicted ephemeris time, and they constrain the orbital inclination to less than 85\u00b0 for gas giant planets with radii down to 0.7R_J.", "date": "2006-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "637", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1094-1101", "id_number": "CaltechAUTHORS:20130109-153237794", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130109-153237794", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "Cottrell Scholar of Research Corporation" }, { "agency": "NASA", "grant_number": "NG05G164G" }, { "agency": "NASA", "grant_number": "NCC5-511" }, { "agency": "NSF", "grant_number": "HRD-9706268" }, { "agency": "NASA", "grant_number": "NAG5-75005" }, { "agency": "NSF", "grant_number": "AST 99-88358" }, { "agency": "NASA", "grant_number": "NAG5-4445" }, { "agency": "NASA", "grant_number": "NAG5-13285" }, { "agency": "NASA", "grant_number": "NNA04CC99A" }, { "agency": "Fondo de Financiamiento de Centros de Investigaci\u00f3n en \u00c1reas Prioritarias (FONDAP)", "grant_number": "15010003" }, { "agency": "NSF Graduate Research Fellowship" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/498557", "primary_object": { "basename": "0004-637X_637_2_1094.pdf", "url": "https://authors.library.caltech.edu/records/qy2qm-jeb92/files/0004-637X_637_2_1094.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Fischer, Debra A.; Laughlin, Gregory; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/k6zgd-1sb76", "eprint_id": 36247, "eprint_status": "archive", "datestamp": "2023-08-19 16:29:00", "lastmod": "2023-10-20 22:55:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Winn-J-N", "name": { "family": "Winn", "given": "Joshua N." }, "orcid": "0000-0002-4265-047X" }, { "id": "Noyes-R-W", "name": { "family": "Noyes", "given": "Robert W." } }, { "id": "Holman-M-J", "name": { "family": "Holman", "given": "Matthew J." }, "orcid": "0000-0002-1139-4880" }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Ohta-Yasuhiro", "name": { "family": "Ohta", "given": "Yasuhiro" } }, { "id": "Taruya-Atsushi", "name": { "family": "Taruya", "given": "Atsushi" } }, { "id": "Suto-Yasushi", "name": { "family": "Suto", "given": "Yasushi" } }, { "id": "Narita-Norio", "name": { "family": "Narita", "given": "Norio" } }, { "id": "Turner-E-L", "name": { "family": "Turner", "given": "Edwin L." } }, { "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "orcid": "0000-0001-9808-7172" }, { "id": "Marcy-G-W", "name": { "family": "Marcy", "given": "Geoffrey W." }, "orcid": "0000-0002-2909-0113" }, { "id": "Butler-R-P", "name": { "family": "Butler", "given": "R. Paul" } }, { "id": "Vogt-S-S", "name": { "family": "Vogt", "given": "Steven S." } } ] }, "title": "Measurement of Spin-Orbit Alignment in an Extrasolar Planetary System", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2005 American Astronomical Society. Received 2005 April 25; accepted 2005 June 3. We acknowledge helpful discussions with T. Brown, E. Chiang, S. Gaudi, D. Lin, and G. Torres. We are grateful to J. Wisdom for advice on calculating the rate of tidal heating.Work by J.N.W. was supported by NASA through Hubble Fellowship grant HST-HF-01180.02-A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. The visit of E. L. T. to the University of Tokyo was supported by an invitation fellowship program for research in Japan from the Japan Society for Promotion of Science (JSPS). This work was partly supported by a Grant-in-Aid for Scientific\nResearch from JSPS (grants 14102004 and 16340053) and by\nNASA grant NAG5-13148.\n\nPublished - 0004-637X_631_2_1215.pdf
", "abstract": "We determine the stellar, planetary, and orbital properties of the transiting planetary system HD 209458 through a joint analysis of high-precision radial velocities, photometry, and timing of the secondary eclipse. Of primary interest is the strong detection of the Rossiter-McLaughlin effect, the alteration of photospheric line profiles that occurs because the planet occults part of the rotating surface of the star. We develop a new technique for modeling this effect and use it to determine the inclination of the planetary orbit relative to the apparent stellar equator (\u03bb = -4\u00ba.4 \u00b1 1\u00ba.4), and the line-of-sight rotation speed of the star (v sin /_\u2605 = 4.70 \u00b1 0.16 km s^(-1)). The uncertainty in these quantities has been reduced by an order of magnitude relative to the pioneering measurements by Queloz and collaborators. The small but nonzero misalignment is probably a relic of the planet formation epoch, because the expected timescale for tidal coplanarization is larger than the age of the star. Our determination of v sin /\u2605 is a rare case in which rotational line broadening has been isolated from other broadening mechanisms.", "date": "2005-10-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "631", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1215-1226", "id_number": "CaltechAUTHORS:20130108-143826499", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130108-143826499", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01180.02-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Japan Society for Promotion of Science (JSPS)", "grant_number": "14102004" }, { "agency": "Japan Society for Promotion of Science (JSPS)", "grant_number": "16340053" }, { "agency": "NASA", "grant_number": "NAG5-13148" } ] }, "doi": "10.1086/432571", "primary_object": { "basename": "0004-637X_631_2_1215.pdf", "url": "https://authors.library.caltech.edu/records/k6zgd-1sb76/files/0004-637X_631_2_1215.pdf" }, "resource_type": "article", "pub_year": "2005", "author_list": "Winn, Joshua N.; Noyes, Robert W.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2wa84-nsf19", "eprint_id": 9921, "eprint_status": "archive", "datestamp": "2023-08-22 02:05:36", "lastmod": "2024-01-12 23:30:01", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Brown-T-M", "name": { "family": "Brown", "given": "Timothy M." }, "orcid": "0000-0002-1793-9968" }, { "id": "Dunham-E-W", "name": { "family": "Dunham", "given": "Edward W." } }, { "id": "Latham-D-W", "name": { "family": "Latham", "given": "David W." }, "orcid": "0000-0001-9911-7388" }, { "id": "Looper-D-L", "name": { "family": "Looper", "given": "Dagny L." } }, { "id": "Mandushev-G", "name": { "family": "Mandushev", "given": "Georgi" } } ] }, "title": "Astrophysical False Positives Encountered in Wide-Field Transit Searches", "ispublished": "unpub", "full_text_status": "public", "keywords": "extrasolar planets, eclipsing binary stars, dwarf stars, astronomical photometry, spectroscopy, astronomical catalogues, transits", "note": "\u00a9 2004 American Institute of Physics. \n\nIssue Date: June 24, 2004.\n\nPublished - CHAaipcp04.pdf
", "abstract": "Wide-field photometric transit surveys for Jupiter-sized planets are inundated by astrophysical false positives, namely systems that contain an eclipsing binary and mimic the desired photometric signature. We discuss several examples of such false alarms. These systems were initially identified as candidates by the PSST instrument at Lowell Observatory. For three of the examples, we present follow-up spectroscopy that demonstrates that these systems consist of (1) an M-dwarf in eclipse in front of a larger star, (2) two main-sequence stars presenting grazing-incidence eclipses, and (3) the blend of an eclipsing binary with the light of a third, brighter star. For an additional candidate, we present multi-color follow-up photometry during a subsequent time of eclipse, which reveals that this candidate consists of a blend of an eclipsing binary and a physically unassociated star. We discuss a couple indicators from publicly-available catalogs that can be used to identify which candidates are likely giant stars, a large source of the contaminants in such surveys.", "date": "2004-06-24", "date_type": "published", "publisher": "American Institute of Physics", "place_of_pub": "Melville, NY", "pagerange": "151-160", "id_number": "CaltechAUTHORS:CHAaipcp04", "isbn": "0-7354-0190-X", "book_title": "The Search for Other Worlds: Fourteenth Astrophysics Conference, College Park, MD, 13-14 October 2003", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:CHAaipcp04", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "contributors": { "items": [ { "id": "Holt-S-S", "name": { "family": "Holt", "given": "Stephen S." } }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" } } ] }, "doi": "10.1063/1.1774515", "primary_object": { "basename": "CHAaipcp04.pdf", "url": "https://authors.library.caltech.edu/records/2wa84-nsf19/files/CHAaipcp04.pdf" }, "resource_type": "book_section", "pub_year": "2004", "author_list": "Charbonneau, David; Brown, Timothy M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/gx3vp-b0v07", "eprint_id": 25164, "eprint_status": "archive", "datestamp": "2023-08-19 13:47:00", "lastmod": "2024-01-13 05:23:19", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Kotredes-L", "name": { "family": "Kotredes", "given": "Lewis" } } ] }, "title": "First Results From Sleuth: The Palomar Planet Finder", "ispublished": "unpub", "full_text_status": "public", "keywords": "extrasolar planets, astronomical telescopes, stars, transits, data acquisition, data analysis", "note": "\u00a9 2004 American Institute of Physics. Issue Date: 24 June 2004.\n\nPublished - ODOaipcp04.pdf
", "abstract": "We discuss preliminary results from our first search campaign for transiting planets performed using Sleuth, an automated 10 cm telescope with a 6 degree square field of view. We monitored a field in Hercules for 40 clear nights between UT 2003 May 10 and July 01, and obtained an rms precision (per 15-min average) over the entire data set of better than 1% on the brightest 2026 stars, and better than 1.5% on the brightest 3865 stars. We identified no strong candidates in the Hercules field. We conducted a blind test of our ability to recover transiting systems by injecting signals into our data and measuring the recovery rate as a function of transit depth and orbital period. About 85% of transit signals with a depth of 0.02 mag were recovered. However, only 50% of transit signals with a depth of 0.01 mag were recovered. We expect that the number of stars for which we can search for transiting planets will increase substantially for our current field in Andromeda, due to the lower Galactic latitude of the field.", "date": "2004-06-24", "date_type": "published", "publisher": "American Institute of Physics", "place_of_pub": "Melville, NY", "pagerange": "169-172", "id_number": "CaltechAUTHORS:20110830-110513513", "isbn": "0-7354-0190-X", "book_title": "The Search for Other Worlds", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110830-110513513", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "contributors": { "items": [ { "id": "Holt-S-S", "name": { "family": "Holt", "given": "Stephen S." } }, { "id": "Deming-D", "name": { "family": "Deming", "given": "Drake" } } ] }, "doi": "10.1063/1.1774518", "primary_object": { "basename": "ODOaipcp04.pdf", "url": "https://authors.library.caltech.edu/records/gx3vp-b0v07/files/ODOaipcp04.pdf" }, "resource_type": "book_section", "pub_year": "2004", "author_list": "O'Donovan, Francis T.; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/db690-y1079", "eprint_id": 25151, "eprint_status": "archive", "datestamp": "2023-08-19 13:46:55", "lastmod": "2024-01-13 05:23:12", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kotredes-L", "name": { "family": "Kotredes", "given": "Lewis" } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" }, { "id": "Looper-D-L", "name": { "family": "Looper", "given": "Dagny L." } }, { "id": "O'Donovan-F-T", "name": { "family": "O'Donovan", "given": "Francis T." } } ] }, "title": "Sherlock: An Automated Follow-Up Telescope for Wide-Field Transit Searches", "ispublished": "unpub", "full_text_status": "public", "keywords": "extrasolar planets, eclipsing binary stars, astronomical telescopes, astronomical photometry, transits", "note": "\u00a9 2004 American Institute of Physics.\nIssue Date: 24 June 2004.\n\nPublished - KOTaipcp04.pdf
", "abstract": "The most significant challenge currently facing photometric surveys for transiting gas-giant planets is that of confusion with eclipsing binary systems that mimic the photometric signature. A simple way to reject most forms of these false positives is high-precision, rapid-cadence monitoring of the suspected transit at higher angular resolution and in several filters. We are currently\nbuilding a system that will perform higher-angular-resolution, multi-color follow-up observations of candidate systems identified by Sleuth (our wide-field transit survey instrument at Palomar), and its two twin system instruments in Tenerife and northern Arizona.", "date": "2004-06-24", "date_type": "published", "publisher": "American Institute of Physics", "place_of_pub": "Melville, NY", "pagerange": "173-176", "id_number": "CaltechAUTHORS:20110829-135131169", "isbn": "0-7354-0190-X", "book_title": "The Search for Other Worlds", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110829-135131169", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "contributors": { "items": [ { "id": "Holt-S-S", "name": { "family": "Holt", "given": "S. S." } }, { "id": "Demings-D", "name": { "family": "Demings", "given": "D." } } ] }, "doi": "10.1063/1.1774519", "primary_object": { "basename": "KOTaipcp04.pdf", "url": "https://authors.library.caltech.edu/records/db690-y1079/files/KOTaipcp04.pdf" }, "resource_type": "book_section", "pub_year": "2004", "author_list": "Kotredes, Lewis; Charbonneau, David; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/bq37f-wfx98", "eprint_id": 85140, "eprint_status": "archive", "datestamp": "2023-08-19 13:25:22", "lastmod": "2023-10-18 17:54:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mugrauer-M", "name": { "family": "Mugrauer", "given": "M." } }, { "id": "Neuh\u00e4user-R", "name": { "family": "Neuh\u00e4user", "given": "R." } }, { "id": "Guenther-E-W", "name": { "family": "Guenther", "given": "E. W." } }, { "id": "Hatzes-A-P", "name": { "family": "Hatzes", "given": "A. P." } }, { "id": "Hu\u00e9lamo-N", "name": { "family": "Hu\u00e9lamo", "given": "N." }, "orcid": "0000-0002-2711-8143" }, { "id": "Fern\u00e1ndez-M", "name": { "family": "Fern\u00e1ndez", "given": "M." } }, { "id": "Ammler-M", "name": { "family": "Ammler", "given": "M." } }, { "id": "Retzlaff-J", "name": { "family": "Retzlaff", "given": "J." } }, { "id": "K\u00f6nig-B", "name": { "family": "K\u00f6nig", "given": "B." } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "D." }, "orcid": "0000-0002-9003-484X" }, { "id": "Jayawardhana-R", "name": { "family": "Jayawardhana", "given": "R." } }, { "id": "Brandner-W", "name": { "family": "Brandner", "given": "W." } } ] }, "title": "HD 77407 and GJ 577: Two new young stellar binaries Detected with the Calar Alto Adaptive Optics system ALFA", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: low mass, brown dwarfs - stars: binaries: general", "note": "\u00a9 2004 ESO. \n\nReceived: 16 May 2003. Accepted: 8 December 2003. \n\nWe are grateful to our referee, Eduardo Mart\u00edn, for several useful comments and the Calar Alto Time Allocation committee for continuous support. R.J. acknowledges support from NASA Origins grant NAG5-11905. The German-Spanish Astronomical Centre Calar Alto is operated by the Max-Planck-Institute for Astronomy, Heidelberg, jointly with the Spanish National Commission for Astronomy. We thank the technical staff of the TLS in Tautenburg for all their help and assistance in carrying out the observations. We thank Jens Woitas, Sebastian Els, and Martin K\u00fcrster for taking some of the spectra of HD 77407. We made use of the 2MASS public data releases and of the Simbad database operated at the Observatoire Strassburg. Some of the data presented herein were obtained at the W. M. Keck Observatory, operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautic and Space Administration. We thank Randy Campbell and David LeMignant for help during the observing run.\n\nPublished - aa3989.pdf
Submitted - 0402104.pdf
", "abstract": "We present the first results from our search for close stellar and sub-stellar companions to young nearby stars on the northern sky. Our infrared imaging observations are obtained with the 3.5\u2009m Calar Alto telescope and the AO system ALFA. With two epoch observations which were separated by about one year, we found two co-moving companion candidates, one close to HD\u200977407 and one close to GJ\u2009577. For the companion candidate near GJ\u2009577, we obtained an optical spectrum showing spectral type M 4.5; this candidate is a bound low-mass stellar companion confirmed by both proper motion and spectroscopy. We estimate the masses for HD\u200977407\u2009B and GJ\u2009577\u2009B to be ~0.3 to 0.5 M_\u2609 and ~0.16 to 0.2 M_\u2609, respectively. Compared to Siess et al. (2000) models, each of the two pairs appears co-eval with HD\u200977407\u2009A, B being 10 to 40\u2009Myrs and GJ\u2009577\u2009A, B being \u2265100\u2009Myrs old. We also took multi-epoch high-resolution spectra of HD\u200977407 to search for sub-stellar companions, but did not find any with 3M_(Jup) as upper mass (m sin i) limit (for up to 4 year orbits); however, we detected a long-term radial velocity trend in HD\u200977407\u2009A, consistent with a ~0.3\u2009M_\u2609 companion at ~50\u2009AU separation, i.e. the one detected by the imaging. Hence, HD\u200977407\u2009B is confirmed to be a bound companion to HD\u200977407\u2009A. We also present limits for undetected, but detectable companions using a deep image of HD\u200977407\u2009A and B, also observed with the Keck NIRC2 AO system; any brown dwarfs were detectable outside of 0.5\u2009arcsec (17\u2009AU at HD\u200977407), giant planets with masses from ~6.5 to 12\u2009M_(Jup) were detectable at \u22651.5\u2009arcsec.", "date": "2004-04-03", "date_type": "published", "publication": "Astronomy & Astrophysics", "volume": "417", "number": "3", "publisher": "EDP Sciences", "pagerange": "1031-1038", "id_number": "CaltechAUTHORS:20180306-133803596", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180306-133803596", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-11905" } ] }, "doi": "10.1051/0004-6361:20040008", "primary_object": { "basename": "0402104.pdf", "url": "https://authors.library.caltech.edu/records/bq37f-wfx98/files/0402104.pdf" }, "related_objects": [ { "basename": "aa3989.pdf", "url": "https://authors.library.caltech.edu/records/bq37f-wfx98/files/aa3989.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Mugrauer, M.; Neuh\u00e4user, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/5qs01-kb943", "eprint_id": 56081, "eprint_status": "archive", "datestamp": "2023-08-19 11:13:22", "lastmod": "2023-10-20 23:37:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "orcid": "0000-0002-9003-484X" } ] }, "title": "Astronomy: Atmosphere out of that world", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2003 Nature Publishing Group.", "abstract": "A planet orbiting very close to a Sun-like star is apparently enveloped by an extended atmosphere of hydrogen atoms, and may be losing mass because of the intense radiation from the parent star.", "date": "2003-03-13", "date_type": "published", "publication": "Nature", "volume": "422", "number": "6928", "publisher": "Nature Publishing Group", "pagerange": "124-125", "id_number": "CaltechAUTHORS:20150325-142027490", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150325-142027490", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1038/422124a", "resource_type": "article", "pub_year": "2003", "author_list": "Charbonneau, David" }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/mpxgf-nsc34", "eprint_id": 85141, "eprint_status": "archive", "datestamp": "2023-08-19 10:16:09", "lastmod": "2023-10-18 17:54:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "K\u00f6nig-B", "name": { "family": "K\u00f6nig", "given": "B." } }, { "id": "Fuhrmann-K", "name": { "family": "Fuhrmann", "given": "K." } }, { "id": "Neuh\u00e4user-R", "name": { "family": "Neuh\u00e4user", "given": "R." } }, { "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "D." }, "orcid": "0000-0002-9003-484X" }, { "id": "Jayawardhana-R", "name": { "family": "Jayawardhana", "given": "R." } } ] }, "title": "Direct detection of the companion of \u03c71 Orionis", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2002 ESO. Article published by EDP Sciences. \n\nReceived 28 August 2002; Accepted 18 September 2002; Published online 21 October 2002. \n\nThis research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. B.K. wants to thank F. Dufey for help with the algebra. R.N. wishes to acknowledge financial support from the Bundesministerium f\u00fcr Bildung und Forschung through the Deutsches Zentrum f\u00fcr Luft- und Raumfahrt e.V. (DLR) under grant number 50 OR 0003. R.J. wishes to acknowledge support from NASA grant NAG5-11905. Some of the Data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and religious significance that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The authors would like to thank Randy Campbell and David LeMignant for help during the observing nights. We thank the referee, G. Gatewood for the helpful comments.\n\nPublished - aaeh282.pdf
Accepted Version - 0209404.pdf
", "abstract": "We present an H-band image of the companion of \u03c71 Orionis taken with the Keck adaptive optic system and NIRC 2 camera equipped with a 300\u2009mas-diameter coronographic mask. The direct detection of this companion star enables us to calculate dynamical masses using only Kepler's laws (M_A = 1.01 \u00b1 0.13 M\u2299, M_B = 0.15 \u00b1 0.02 M\u2299), and to study stellar evolutionary models at a wide spread of masses. The application of Baraffe et al. ([CITE]) pre-main-sequence models implies an age of 70\u2013130\u2009Myrs. This is in conflict to the age of the primary, a confirmed member of the Ursa Major Cluster with a canonical age of 300\u2009Myrs. As a consequence, either the models at low masses underestimate the age or the Ursa Major Cluster is considerably younger than assumed.", "date": "2002-11-02", "date_type": "published", "publication": "Astronomy & Astrophysics", "volume": "394", "number": "3", "publisher": "EDP Sciences", "pagerange": "L43-L46", "id_number": "CaltechAUTHORS:20180306-133951721", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180306-133951721", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Bildung und Forschung (BMBF)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50 OR 0003" }, { "agency": "NASA", "grant_number": "NAG5-11905" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1051/0004-6361:20021377", "primary_object": { "basename": "0209404.pdf", "url": "https://authors.library.caltech.edu/records/mpxgf-nsc34/files/0209404.pdf" }, "related_objects": [ { "basename": "aaeh282.pdf", "url": "https://authors.library.caltech.edu/records/mpxgf-nsc34/files/aaeh282.pdf" } ], "resource_type": "article", "pub_year": "2002", "author_list": "K\u00f6nig, B.; Fuhrmann, K.; et el." } ]