[ { "id": "authors:9ap0e-kpw63", "collection": "authors", "collection_id": "9ap0e-kpw63", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191009-090203213", "type": "book_section", "title": "ATLAS probe for the study of galaxy evolution with 300,000,000 galaxy spectra", "book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave", "author": [ { "family_name": "Content", "given_name": "Robert", "clpid": "Content-R" }, { "family_name": "Wang", "given_name": "Yun", "clpid": "Wang-Yun" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" }, { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" }, { "family_name": "Chary", "given_name": "Ranga", "orcid": "0000-0001-7583-0621", "clpid": "Chary-R-R" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" } ], "contributor": [ { "family_name": "Lystrup", "given_name": "Makenzie", "clpid": "Lystrup-M" }, { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Fazio", "given_name": "Giovanni G.", "clpid": "Fazio-G-G" }, { "family_name": "Batalha", "given_name": "Natalie", "clpid": "Batalha-N-M" }, { "family_name": "Siegler", "given_name": "Nicholas", "clpid": "Siegler-N" }, { "family_name": "Tong", "given_name": "Edward C.", "clpid": "Tong-Edward-C" } ], "abstract": "ATLAS (Astrophysics Telescope for Large Area Spectroscopy) Probe is a mission concept for a NASA probe-class space mission with primary science goal the definitive study of galaxy evolution through the capture of 300,000,000 galaxy spectra up to z=7. It is made of a 1.5-m Ritchey-Chretien telescope with a field of view of solid angle 0.4 deg^2. The wavelength range is at least 1 \u03bcm to 4 \u03bcm with a goal of 0.9 \u03bcm to 5 \u03bcm. Average resolution is 600 but with a possible trade-off to get 1000 at the longer wavelengths. The ATLAS Probe instrument is made of 4 identical spectrographs each using a Digital Micro-mirror Device (DMD) as a multi-object mask. It builds on the work done for the ESA SPACE and Phase-A EUCLID projects. Three-mirror fore-optics re-image each sub-field on its DMD which has 2048 x 1080 mirrors 13.6 \u03bcm wide with 2 possible tilts, one sending light to the spectrograph, the other to a light dump. The ATLAS Probe spectrographs use prisms as dispersive elements because of their higher and more uniform transmission, their larger bandwidth, and the ability to control the resolution slope with the choice of glasses. Each spectrograph has 2 cameras. While the collimator is made of 4 mirrors, each camera is made of only one mirror which reduces the total number of optics. All mirrors are aspheric but with a relatively small P-V with respect to their best fit sphere making them easily manufacturable. For imaging, a simple mirror to replace the prism is not an option because the aberrations are globally corrected by the collimator and camera together which gives large aberrations when the mirror is inserted. An achromatic grism is used instead. There are many variations of the design that permit very different packaging of the optics. ATLAS Probe will enable ground-breaking science in all areas of astrophysics. It will (1) revolutionize galaxy evolution studies by tracing the relation between galaxies and dark matter from the local group to cosmic voids and filaments, from the epoch of reionization through the peak era of galaxy assembly; (2) open a new window into the dark universe by mapping the dark matter filaments to unveil the nature of the dark Universe using 3D weak lensing with spectroscopic redshifts, and obtaining definitive measurements of dark energy and modification of gravity using cosmic large-scale structure; (3) probe the Milky Way's dust-shrouded regions, reaching the far side of our Galaxy; and (4) characterize asteroids and other objects in the outer solar systems.", "doi": "10.1117/12.2313082", "isbn": "9781510619494", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2018-08-22", "pages": "Art. No. 106980I" }, { "id": "authors:48vrn-shj95", "collection": "authors", "collection_id": "48vrn-shj95", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180913-074150682", "type": "book_section", "title": "Multiwavelength Variability Surveys: Reaping the Stellar Harvest", "book_title": "Astronomical Data Analysis Software and Systems XXV", "author": [ { "family_name": "Cody", "given_name": "Ann Marie", "orcid": "0000-0002-3656-6706", "clpid": "Cody-A-M" }, { "family_name": "Stauffer", "given_name": "John R.", "orcid": "0000-0003-3595-7382", "clpid": "Stauffer-J-R" }, { "family_name": "Rebull", "given_name": "Luisa M.", "orcid": "0000-0001-6381-515X", "clpid": "Rebull-L-M" }, { "family_name": "Hillenbrand", "given_name": "Lynne A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Song", "given_name": "Inseok", "orcid": "0000-0002-5815-7372", "clpid": "Song-Inseok" } ], "contributor": [ { "family_name": "Lorente", "given_name": "Nuria P. F.", "clpid": "Lorente-N-P-F" }, { "family_name": "Shortridge", "given_name": "Keith", "clpid": "Shortridge-K" }, { "family_name": "Wayth", "given_name": "Randall", "clpid": "Wayth-R-B" } ], "abstract": "Over the past decade, a number of dedicated stellar variability surveys have launched from both the ground and space. Many of these programs focus on the detection of specific events, such as exoplanet transits, microlensing amplification, or extragalactic transients. Yet the observed variability behavior encompasses a much larger range of stellar phenomena. To take full advantage of variability survey data, we must detect and classify distinct morphological features in light curves. This task has been particularly challenging for the young (1\u201310 million year old) stars, which are well known to vary at the 1\u2013100% level on timescales of hours to years. Here we highlight recent progress in the identification, classification, and physical understanding of young star variability. We introduce a selection of time series of pre-main sequence stars from state-of-the-art datasets, including the Young Stellar Object Variability (YSOVAR) campaign with the Spitzer Space Telescope. We describe the data storage approaches and time series analysis techniques employed to extract physically meaningful information from the light curves. The lessons learned from YSOVAR and other campaigns should be broadly applicable to massive future surveys such as TESS and LSST.", "isbn": "978-1-58381-908-1", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "2016", "pages": "13-21" }, { "id": "authors:4v7bj-qcw07", "collection": "authors", "collection_id": "4v7bj-qcw07", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170629-130948937", "type": "book_section", "title": "Empirical Limits on Radial Velocity - Planet Detection for Young Stars", "author": [ { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" }, { "family_name": "Isaacson", "given_name": "Howard", "orcid": "0000-0002-0531-1073", "clpid": "Isaacson-H-T" }, { "family_name": "Marcy", "given_name": "Geoffrey", "orcid": "0000-0002-2909-0113", "clpid": "Marcy-G-W" }, { "family_name": "Barenfeld", "given_name": "Scott A.", "orcid": "0000-0001-5222-6851", "clpid": "Barenfeld-S-A" }, { "family_name": "Fischer", "given_name": "Debra A.", "orcid": "0000-0003-2221-0861", "clpid": "Fischer-D-A" }, { "family_name": "Howard", "given_name": "Andrew", "orcid": "0000-0001-8638-0320", "clpid": "Howard-A-W" } ], "contributor": [ { "family_name": "van Belle", "given_name": "G.", "clpid": "van-Belle-G" }, { "family_name": "Harris", "given_name": "H.", "clpid": "Harris-H" } ], "abstract": "We report initial results from our long term search using precision radial velocities for planetary-mass companions located within a few AU of stars younger than the Sun. Based on a sample of >150 stars, we define a floor in the radial velocity scatter, \u03c3_(RV), as a function of the chromospheric activity level R'_(HK). This lower bound to the jitter, which increases with increasing stellar activity, sets the minimum planet mass that could be detected. Adopting a median activity-age relationship reveals the astrophysical limits to planet masses discernable via radial velocity monitoring, as a function of stellar age. Considering solar-mass primaries having the mean jitter-activity level, when they are younger than 100 / 300 / 1000 Myr, the stochastic jitter component in radial velocity measurements restricts detectable companion masses to > 0.3 / 0.2 / 0.1 M_(Jupiter). These numbers require a large number \u2014 several tens \u2014 of radial velocity observations taken over a time frame longer than the orbital period. Lower companion mass limits can be achieved for stars with less than the mean jitter and/or with an increased number of observations.", "doi": "10.48550/arXiv.1408.3475", "publication_date": "2014-06" }, { "id": "authors:zzfew-yc859", "collection": "authors", "collection_id": "zzfew-yc859", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150128-144734095", "type": "book_section", "title": "Ages of Young Stars", "book_title": "Protostars and Planets VI", "author": [ { "family_name": "Soderblom", "given_name": "David R.", "orcid": "0000-0002-0322-8161", "clpid": "Soderblom-D-R" }, { "family_name": "Hillenbrand", "given_name": "Lynne A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Jeffries", "given_name": "Rob D.", "clpid": "Jeffries-R-D" }, { "family_name": "Mamajek", "given_name": "Eric E.", "orcid": "0000-0003-2008-1488", "clpid": "Mamajek-E-E" }, { "family_name": "Naylor", "given_name": "Tim", "orcid": "0000-0002-0506-8501", "clpid": "Naylor-T" } ], "contributor": [ { "family_name": "Beuther", "given_name": "Henrik", "clpid": "Beuther-H" }, { "family_name": "Klessen", "given_name": "Ralf S.", "clpid": "Klessen-R-S" }, { "family_name": "Dullemond", "given_name": "Cornelis P.", "clpid": "Dullemond-C-P" }, { "family_name": "Henning", "given_name": "Thomas", "clpid": "Henning-T" } ], "abstract": "Determining the sequence of events in the formation of stars and planetary systems and their\ntimescales is essential for understanding those processes, yet establishing ages is fundamentally\ndifficult because we lack direct indicators. In this review we discuss the age challenge for\nyoung stars, specifically those less than ~ 100 m.y. old. Most age determination methods that\nwe discuss are primarily applicable to groups of stars but can be used to estimate the age of\nindividual objects. A reliable age scale is established above 20 m.y. from measurement of the\nlithium depletion boundary (LDB) in young clusters, and consistency is shown between these\nages and those from the upper-main-sequence (UMS) and main-sequence (MS) tum-off - if\nmodest core convection and rotation is included in the models of higher-mass stars. Other\navailable methods for age estimation include the kinematics of young groups, placing stars in\nHertzsprung-Russell diagrams (HRDs), pulsations and seismology, surface gravity measurement,\nrotation and activity, and Li abundance. We review each of these methods and present\nknown strengths and weaknesses. Below ~20 m.y., both model-dependent and observational\nuncertainties grow, the situation is confused by the possibility of age spreads, and no reliable\nabsolute ages yet exist. The lack of absolute age calibration below 20 m.y. should be born in\nmind when considering the lifetimes of protostellar phases and circumstellar material.", "doi": "10.2458/azu_uapress_9780816531240-ch010", "isbn": "9780816531240", "publisher": "University of Arizona Press", "place_of_publication": "Tucson, AZ", "publication_date": "2014", "pages": "219-241" }, { "id": "authors:jh02c-per73", "collection": "authors", "collection_id": "jh02c-per73", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180713-113820608", "type": "book_section", "title": "Estimate low- and high-order wavefront using P1640 calibrator measurements", "book_title": "Techniques and Instrumentation for Detection of Exoplanets VI", "author": [ { "family_name": "Zhai", "given_name": "C.", "orcid": "0000-0002-0291-4522", "clpid": "Zhai-Chengxing" }, { "family_name": "Vasisht", "given_name": "G.", "orcid": "0000-0002-1871-6264", "clpid": "Vasisht-G" }, { "family_name": "Shao", "given_name": "M.", "clpid": "Shao-Michael" }, { "family_name": "Lockhart", "given_name": "T.", "clpid": "Lockhart-T-G" }, { "family_name": "Cady", "given_name": "E.", "orcid": "0000-0002-8789-2931", "clpid": "Cady-E-J" }, { "family_name": "Oppenheimer", "given_name": "B.", "orcid": "0000-0001-7130-7681", "clpid": "Oppenheimer-Rebecca" }, { "family_name": "Burruss", "given_name": "R.", "clpid": "Burruss-R" }, { "family_name": "Roberts", "given_name": "J.", "clpid": "Roberts-J" }, { "family_name": "Beichman", "given_name": "C.", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Brenner", "given_name": "D.", "clpid": "Brenner-D" }, { "family_name": "Crepp", "given_name": "J.", "orcid": "0000-0003-0800-0593", "clpid": "Crepp-J-R" }, { "family_name": "Dekany", "given_name": "R.", "clpid": "Dekany-Richard" }, { "family_name": "Hillenbrand", "given_name": "L.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Hinkley", "given_name": "S.", "orcid": "0000-0001-8074-2562", "clpid": "Hinkley-S" }, { "family_name": "Parry", "given_name": "I.", "clpid": "Parry-I-R" }, { "family_name": "Pueyo", "given_name": "L.", "orcid": "0000-0003-3818-408X", "clpid": "Pueyo-L" }, { "family_name": "Rice", "given_name": "E.", "orcid": "0000-0002-3252-5886", "clpid": "Rice-E-L" }, { "family_name": "Roberts", "given_name": "L. C.", "orcid": "0000-0003-3892-2900", "clpid": "Roberts-L-C-Jr" }, { "family_name": "Sivaramakrishnan", "given_name": "A.", "clpid": "Sivaramakrishnan-A" }, { "family_name": "Soummer", "given_name": "R.", "orcid": "0000-0003-2753-2819", "clpid": "Soummer-R" }, { "family_name": "Tang", "given_name": "H.", "clpid": "Tang-Haolan" }, { "family_name": "Vescelus", "given_name": "F.", "clpid": "Vescelus-F-E" }, { "family_name": "Wallace", "given_name": "K.", "clpid": "Wallace-K" }, { "family_name": "Zimmerman", "given_name": "N.", "orcid": "0000-0001-5484-1516", "clpid": "Zimmerman-N" } ], "contributor": [ { "family_name": "Shaklan", "given_name": "Stuart B.", "clpid": "Shaklan-S-B" } ], "abstract": "P1640 high contrast imaging system on the Palomar 200 inch Telescope consists of an apodized-pupil Lyot coronagraph, the PALM-3000 adaptive optics (P3K-AO), and P1640 Calibrator (CAL). Science images are recorded by an integral field spectrograph covering J-H bands for detecting and characterizing stellar companions. With aberrations from atmosphere corrected by the P3K-AO, instrument performance is limited mainly by the quasi-static speckles due to noncommon path wavefront aberrations for the light to propagate to the P3K-AO wavefront sensor and to the coronagraph mask. The non-common path wavefront aberrations are sensed by CAL, which measures the post-coronagraph E-field using interferometry, and can be effectively corrected by offsetting the P3K-AO deformable mirror target position accordingly. Previously, we have demonstrated using CAL measurements to correct high order wavefront aberrations, which is directly connected to the static speckles in the image plane. Low order wavefront, on the other hand, usually of larger amplitudes, causes light to leak through the coronagraph making the whole image plane brighter. Knowledge error in low order wavefront aberrations can also affect the estimation of the high order wavefront. Even though, CAL is designed to sense efficiently high order wavefront aberrations, the low order wavefront front can be inferred with less sensitivity. Here, we describe our method for estimating both low and high order wavefront aberrations using CAL measurements by propagating the post-coronagraph E-field to a pupil before the coronagraph. We present the results from applying this method to both simulated and experiment data.", "doi": "10.1117/12.2024754", "isbn": "9780819497147", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2013-09-26", "pages": "Art. No. 88640L" }, { "id": "authors:ynka0-zev62", "collection": "authors", "collection_id": "ynka0-zev62", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180717-155315869", "type": "book_section", "title": "Electric field conjugation with the project 1640 coronagraph", "book_title": "Techniques and Instrumentation for Detection of Exoplanets VI", "author": [ { "family_name": "Cady", "given_name": "Eric", "orcid": "0000-0002-8789-2931", "clpid": "Cady-E-J" }, { "family_name": "Baranec", "given_name": "Christoph", "orcid": "0000-0002-1917-9157", "clpid": "Baranec-C" }, { "family_name": "Beichman", "given_name": "Charles", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Dekany", "given_name": "Richard", "clpid": "Dekany-Richard" }, { "family_name": "Hale", "given_name": "David", "clpid": "Hale-D-D-S" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" }, { "family_name": "Hinkley", "given_name": "Sasha", "orcid": "0000-0001-8074-2562", "clpid": "Hinkley-S" } ], "contributor": [ { "family_name": "Shaklan", "given_name": "Stuart", "clpid": "Shaklan-S-B" } ], "abstract": "The Project 1640 instrument on the 200-inch Hale telescope at Palomar Observatory is a coronagraphic instru- ment with an integral eld spectrograph at the back end, designed to nd young, self-luminous planets around nearby stars. To reach the necessary contrast for this, the PALM-3000 adaptive optics system corrects for fast atmospheric speckles, while CAL, a phase-shifting interferometer in a Mach-Zehnder con guration, measures the quasistatic components of the complex electric eld in the pupil plane following the coronagraphic stop. Two additional sensors measure and control low-order modes. These eld measurements may then be combined with a system model and data taken separately using a white-light source internal to the AO system to correct for both phase and amplitude aberrations. Here, we discuss and demonstrate the procedure to maintain a half-plane dark hole in the image plane while the spectrograph is taking data, including initial on-sky performance.", "doi": "10.1117/12.2024635", "isbn": "9780819497147", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2013-09-26", "pages": "Art. No. 88640K" }, { "id": "authors:kwjgz-8cp37", "collection": "authors", "collection_id": "kwjgz-8cp37", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161024-150653410", "type": "book_section", "title": "A first order wavefront estimation algorithm for P1640 calibrator", "book_title": "Adaptive Optics Systems III", "author": [ { "family_name": "Zhai", "given_name": "C.", "orcid": "0000-0002-0291-4522", "clpid": "Zhai-Chengxing" }, { "family_name": "Vasisht", "given_name": "G.", "orcid": "0000-0002-1871-6264", "clpid": "Vasisht-G" }, { "family_name": "Shao", "given_name": "M.", "clpid": "Shao-Michael" }, { "family_name": "Lockhart", "given_name": "T.", "clpid": "Lockhart-T-G" }, { "family_name": "Cady", "given_name": "E.", "orcid": "0000-0002-8789-2931", "clpid": "Cady-E-J" }, { "family_name": "Oppenheimer", "given_name": "B.", "orcid": "0000-0001-7130-7681", "clpid": "Oppenheimer-Rebecca" }, { "family_name": "Burruss", "given_name": "R.", "clpid": "Burruss-R-S" }, { "family_name": "Roberts", "given_name": "J.", "clpid": "Roberts-J-E" }, { "family_name": "Beichman", "given_name": "C.", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Brenner", "given_name": "D.", "clpid": "Brenner-D" }, { "family_name": "Crepp", "given_name": "J.", "orcid": "0000-0003-0800-0593", "clpid": "Crepp-J-R" }, { "family_name": "Dekany", "given_name": "R.", "clpid": "Dekany-Richard" }, { "family_name": "Hinkley", "given_name": "S.", "orcid": "0000-0001-8074-2562", "clpid": "Hinkley-S" }, { "family_name": "Hillenbrand", "given_name": "L.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Ligon", "given_name": "E. R.", "clpid": "Ligon-E-R" }, { "family_name": "Parry", "given_name": "I.", "clpid": "Parry-I-R" }, { "family_name": "Pueyo", "given_name": "L.", "orcid": "0000-0003-3818-408X", "clpid": "Pueyo-L" }, { "family_name": "Rice", "given_name": "E.", "orcid": "0000-0002-3252-5886", "clpid": "Rice-E-L" }, { "family_name": "Roberts", "given_name": "L. C., Jr.", "orcid": "0000-0003-3892-2900", "clpid": "Roberts-L-C-Jr" }, { "family_name": "Sivaramakrishnan", "given_name": "A.", "clpid": "Sivaramakrishnan-A" }, { "family_name": "Soummer", "given_name": "R.", "orcid": "0000-0003-2753-2819", "clpid": "Soummer-R" }, { "family_name": "Vescelus", "given_name": "F.", "clpid": "Vescelus-F-E" }, { "family_name": "Wallace", "given_name": "K.", "clpid": "Wallace-K" }, { "family_name": "Zimmerman", "given_name": "N.", "orcid": "0000-0001-5484-1516", "clpid": "Zimmerman-N" } ], "contributor": [ { "family_name": "Ellerbroek", "given_name": "Brent L.", "clpid": "Ellerbroek-B-L" }, { "family_name": "Marchetti", "given_name": "Enrico", "clpid": "Marchetti-E" }, { "family_name": "V\u00e9ran", "given_name": "Jean-Pierre", "clpid": "V\u00e9ran-J-P" } ], "abstract": "P1640 calibrator is a wavefront sensor working with the P1640 coronagraph and the Palomar 3000 actuator adaptive optics system (P3K) at the Palomar 200 inch Hale telescope. It measures the wavefront by interfering post-coronagraph light with a reference beam formed by low-pass filtering the blocked light from the coronagraph focal plane mask. The P1640 instrument has a similar architecture to the Gemini Planet Imager (GPI) and its performance is currently limited by the quasi-static speckles due to non-common path wavefront errors, which comes from the non-common path for the light to arrive at the AO wavefront sensor and the coronagraph mask. By measuring the wavefront after the coronagraph mask, the non-common path wavefront error can be estimated and corrected by feeding back the error signal to the deformable mirror (DM) of the P3K AO system. Here, we present a first order wavefront estimation algorithm and an instrument calibration scheme used in experiments done recently at Palomar observatory. We calibrate the P1640 calibrator by measuring its responses to poking DM actuators with a sparse checkerboard pattern at different amplitudes. The calibration yields a complex normalization factor for wavefront estimation and establishes the registration of the DM actuators at the pupil camera of the P1640 calibrator, necessary for wavefront correction. Improvement of imaging quality after feeding back the wavefront correction to the AO system demonstrated the efficacy of the algorithm.", "doi": "10.1117/12.927015", "isbn": "9780819491480", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2012-09-13", "pages": "Art. No. 84476W" }, { "id": "authors:vbqfz-kj225", "collection": "authors", "collection_id": "vbqfz-kj225", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161026-082716327", "type": "book_section", "title": "Project 1640: the world's first ExAO coronagraphic hyperspectral imager for comparative planetary science", "book_title": "Adaptive Optics Systems III", "author": [ { "family_name": "Oppenheimer", "given_name": "Ben R.", "orcid": "0000-0001-7130-7681", "clpid": "Oppenheimer-Rebecca" }, { "family_name": "Beichman", "given_name": "Charles", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Brenner", "given_name": "Douglas", "clpid": "Brenner-D" }, { "family_name": "Burruss", "given_name": "Rick", "clpid": "Burruss-R-S" }, { "family_name": "Cady", "given_name": "Eric", "orcid": "0000-0002-8789-2931", "clpid": "Cady-E-J" }, { "family_name": "Crepp", "given_name": "Justin", "orcid": "0000-0003-0800-0593", "clpid": "Crepp-J-R" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" }, { "family_name": "Hinkley", "given_name": "Sasha", "orcid": "0000-0001-8074-2562", "clpid": "Hinkley-S" }, { "family_name": "Ligon", "given_name": "E. R.", "clpid": "Ligon-E-R" }, { "family_name": "Lockhart", "given_name": "Thomas", "clpid": "Lockhart-T-G" }, { "family_name": "Parry", "given_name": "Ian", "clpid": "Parry-I-R" }, { "family_name": "Pueyo", "given_name": "Laurent", "orcid": "0000-0003-3818-408X", "clpid": "Pueyo-L" }, { "family_name": "Rice", "given_name": "Emily", "orcid": "0000-0002-3252-5886", "clpid": "Rice-E-L" }, { "family_name": "Roberts", "given_name": "Lewis C.", "orcid": "0000-0003-3892-2900", "clpid": "Roberts-L-C-Jr" }, { "family_name": "Roberts", "given_name": "Jennifer", "clpid": "Roberts-J-E" }, { "family_name": "Shao", "given_name": "Michael", "clpid": "Shao-Michael" }, { "family_name": "Sivaramakrishnan", "given_name": "Anand", "clpid": "Sivaramakrishnan-A" }, { "family_name": "Soummer", "given_name": "R\u00e9mi", "orcid": "0000-0003-2753-2819", "clpid": "Soummer-R" }, { "family_name": "Vasisht", "given_name": "Gautam", "orcid": "0000-0002-1871-6264", "clpid": "Vasisht-G" }, { "family_name": "Vescelus", "given_name": "Fred", "clpid": "Vescelus-F-E" }, { "family_name": "Wallace", "given_name": "J. Kent", "clpid": "Wallace-J-K" }, { "family_name": "Zhai", "given_name": "Chengxing", "orcid": "0000-0002-0291-4522", "clpid": "Zhai-Chengxing" }, { "family_name": "Zimmerman", "given_name": "Neil", "orcid": "0000-0001-5484-1516", "clpid": "Zimmerman-N" } ], "contributor": [ { "family_name": "Ellerbroek", "given_name": "Brent L.", "clpid": "Ellerbroek-B-L" }, { "family_name": "Marchetti", "given_name": "Enrico", "clpid": "Marchetti-E" }, { "family_name": "V\u00e9ran", "given_name": "Jean-Pierre", "clpid": "V\u00e9ran-J-P" } ], "abstract": "Project 1640, a high-contrast spectral-imaging effort involving a coordinated set of instrumentation and software, built at AMNH, JPL, Cambridge and Caltech, has been commissioned and is fully operational. This novel suite of instrumentation includes a 3388+241-actuator adaptive optics system, an optimized apodized pupil Lyot coronagraph, an integral field spectrograph, and an interferometric calibration wave front sensor. Project 1640 is the first of its kind of instrumentation, designed to image and characterize planetary systems around nearby stars, employing a variety of techniques to break the speckle-noise barrier. It is operational roughly one year before any similar project, with the goal of reaching a contrast of 10^(-7) at 1 arcsecond separation. We describe the instrument, highlight recent results, and document on-sky performance at the start of a 3-year, 99-night survey at the Palomar 5-m Hale telescope.", "doi": "10.1117/12.926419", "isbn": "978-0-8194-9148-0", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2012-09-13", "pages": "Art. No. 844720" }, { "id": "authors:9dkxk-8xj54", "collection": "authors", "collection_id": "9dkxk-8xj54", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150522-083914095", "type": "book_section", "title": "Coronagraphic Imaging of Debris Disks From a High Altitude Balloon Platform", "book_title": "Space Telescopes and Instrumentation 2012: Optical, Infrared, and Millimeter Wave", "author": [ { "family_name": "Unwin", "given_name": "Stephen", "clpid": "Unwin-S-C" }, { "family_name": "Traub", "given_name": "Wesley", "clpid": "Traub-W-A" }, { "family_name": "Bryden", "given_name": "Geoffrey", "clpid": "Bryden-G" }, { "family_name": "Brugarolas", "given_name": "Paul", "clpid": "Brugarolas-P-B" }, { "family_name": "Chen", "given_name": "Pin", "clpid": "Chen-Pin" }, { "family_name": "Guyon", "given_name": "Olivier", "orcid": "0000-0002-1097-9908", "clpid": "Guyon-O" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" }, { "family_name": "Krist", "given_name": "John", "clpid": "Krist-John-E" }, { "family_name": "Macintosh", "given_name": "Bruce", "orcid": "0000-0003-1212-7538", "clpid": "Macintosh-B-A" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Mennesson", "given_name": "Bertrand", "orcid": "0000-0003-4205-4800", "clpid": "Mennesson-B" }, { "family_name": "Moody", "given_name": "Dwight", "clpid": "Moody-D-C" }, { "family_name": "Roberts", "given_name": "Lewis C., Jr.", "orcid": "0000-0003-3892-2900", "clpid": "Roberts-L-C-Jr" }, { "family_name": "Stapelfeldt", "given_name": "Karl", "orcid": "0000-0002-2805-7338", "clpid": "Stapelfeldt-K-R" }, { "family_name": "Stuchlik", "given_name": "David", "clpid": "Stuchlik-D" }, { "family_name": "Trauger", "given_name": "John", "clpid": "Trauger-J-T" }, { "family_name": "Vasisht", "given_name": "Gautam", "orcid": "0000-0002-1871-6264", "clpid": "Vasisht-G" } ], "contributor": [ { "family_name": "Clampin", "given_name": "Mark C.", "clpid": "Clampin-M-C" }, { "family_name": "Fazio", "given_name": "Giovanni G.", "clpid": "Fazio-G-G" }, { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Oschmann", "given_name": "Jacobus M., Jr.", "clpid": "Oschmann-J-M-Jr" } ], "abstract": "Debris disks around nearby stars are tracers of the planet formation process, and they are a key element of our understanding of the formation and evolution of extrasolar planetary systems. With multi-color images of a significant number of disks, we can probe important questions: can we learn about planetary system evolution; what materials are the disks made of; and can they reveal the presence of planets? Most disks are known to exist only through their infrared flux excesses as measured by the Spitzer Space Telescope, and through images measured by Herschel. The brightest, most extended disks have been imaged with HST, and a few, such as Fomalhaut, can be observed using ground-based telescopes. But the number of good images is still very small, and there are none of disks with densities as low as the disk associated with the asteroid belt and Edgeworth\u00ad Kuiper belt in our own Solar System. Direct imaging of disks is a major observational challenge, demanding high angular resolution and extremely high dynamic range close to the parent star. The ultimate experiment requires a space-based platform, but demonstrating much of the needed technology, mitigating the technical risks of a space-based coronagraph, and performing valuable measurements of circumstellar debris disks, can be done from a high-altitude balloon platform. In this paper we present a balloon-borne telescope concept based on the Zodiac II design that could undertake compelling studies of a sample of debris disks.", "doi": "10.1117/12.924175", "isbn": "9780819491435", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2012-08-22", "pages": "Art. No. 84420G" }, { "id": "authors:grnd4-vsb87", "collection": "authors", "collection_id": "grnd4-vsb87", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150526-075815173", "type": "book_section", "title": "Zodiac II: Debris Disk Science from a Balloon", "book_title": "Techniques and Instrumentation for Detection of Exoplanets V", "author": [ { "family_name": "Bryden", "given_name": "Geoffrey", "clpid": "Bryden-G" }, { "family_name": "Traub", "given_name": "Wesley", "clpid": "Traub-W-A" }, { "family_name": "Roberts", "given_name": "Lewis C., Jr.", "orcid": "0000-0003-3892-2900", "clpid": "Roberts-L-C-Jr" }, { "family_name": "Bruno", "given_name": "Robin", "clpid": "Bruno-R" }, { "family_name": "Unwin", "given_name": "Stephen", "clpid": "Unwin-S-C" }, { "family_name": "Backovsky", "given_name": "Stan", "clpid": "Backovsky-S" }, { "family_name": "Brugarolas", "given_name": "Paul", "clpid": "Brugarolas-P-B" }, { "family_name": "Chakrabarti", "given_name": "Supriya", "clpid": "Charkrabarti-S" }, { "family_name": "Chen", "given_name": "Pin", "clpid": "Chen-Pin" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" }, { "family_name": "Krist", "given_name": "John", "clpid": "Krist-J-E" }, { "family_name": "Lillie", "given_name": "Charles", "clpid": "Lillie-C-F" }, { "family_name": "Macintosh", "given_name": "Bruce", "orcid": "0000-0003-1212-7538", "clpid": "Macintosh-B-A" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Mennesson", "given_name": "Bertrand", "orcid": "0000-0003-4205-4800", "clpid": "Mennesson-B" }, { "family_name": "Moody", "given_name": "Dwight", "clpid": "Moody-D-C" }, { "family_name": "Rahman", "given_name": "Zahidul", "clpid": "Rahman-Z" }, { "family_name": "Rey", "given_name": "Justin", "clpid": "Rey-J" }, { "family_name": "Stapelfeldt", "given_name": "Karl", "orcid": "0000-0002-2805-7338", "clpid": "Stapelfeldt-K-R" }, { "family_name": "Stuchlik", "given_name": "David", "clpid": "Stuchlik-D" }, { "family_name": "Trauger", "given_name": "John", "clpid": "Trauger-J-T" }, { "family_name": "Vasisht", "given_name": "Gautam", "orcid": "0000-0002-1871-6264", "clpid": "Vasisht-G" } ], "contributor": [ { "family_name": "Shaklan", "given_name": "Stuart", "clpid": "Shaklan-S-B" } ], "abstract": "Zodiac II is a proposed balloon-borne science investigation of debris disks around nearby stars. Debris disks are analogs of the Asteroid Belt (mainly rocky) and Kuiper Belt (mainly icy) in our Solar System. Zodiac II will measure the size, shape, brightness, and color of a statistically significant sample of disks. These measurements will enable us to probe these fundamental questions: what do debris disks tell us about the evolution of planetary systems; how are debris disks produced; how are debris disks shaped by planets; what materials are debris disks made of; how much dust do debris disks make as they grind down; and how long do debris disks live? In addition, Zodiac II will observe hot, young exoplanets as targets of opportunity. The Zodiac II instrument is a 1.1-m diameter SiC telescope and an imaging coronagraph on a gondola carried by a stratospheric balloon. Its data product is a set of images of each targeted debris disk in four broad visiblewavelength bands. Zodiac II will address its science questions by taking high-resolution, multi-wavelength images of the debris disks around tens of nearby stars. Mid-latitude flights are considered: overnight test flights within the United States followed by half-global flights in the Southern Hemisphere. These longer flights are required to fully explore the set of known debris disks accessible only to Zodiac II. On these targets, it will be 100 times more sensitive than the Hubble Space Telescope's Advanced Camera for Surveys (HST/ACS); no existing telescope can match the Zodiac II contrast and resolution performance. A second objective of Zodiac II is to use the near-space environment to raise the Technology Readiness Level (TRL) of SiC mirrors, internal coronagraphs, deformable mirrors, and wavefront sensing and control, all potentially needed for a future space-based telescope for high-contrast exoplanet imaging.", "doi": "10.1117/12.899688", "isbn": "978-0-81948-761-2", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2011-09-15", "pages": "Art. No. 81511E" }, { "id": "authors:sn73b-3qk70", "collection": "authors", "collection_id": "sn73b-3qk70", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180718-112637178", "type": "book_section", "title": "First Keck Interferometer measurements in self-phase referencing mode: spatially resolving circum-stellar line emission of 48 Lib", "book_title": "Optical and Infrared Interferometry II", "author": [ { "family_name": "Pott", "given_name": "J.-U.", "orcid": "0000-0003-4291-2078", "clpid": "Pott-J-U" }, { "family_name": "Akeson", "given_name": "R. L.", "orcid": "0000-0001-9674-1564", "clpid": "Akeson-R-L" }, { "family_name": "Hillenbrand", "given_name": "L. A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Millan-Gabet", "given_name": "R.", "orcid": "0000-0003-0447-5866", "clpid": "Millan-Gabet-R" }, { "family_name": "Colavita", "given_name": "M. M.", "clpid": "Colavita-M-M" }, { "family_name": "Felizardo", "given_name": "C.", "clpid": "Felizardo-C" }, { "family_name": "Herstein", "given_name": "J.", "clpid": "Herstein-J-S" } ], "contributor": [ { "family_name": "Danchi", "given_name": "William C.", "clpid": "Danchi-W-C" }, { "family_name": "Delplancke", "given_name": "Fran\u00e7oise", "clpid": "Delplancke-F" }, { "family_name": "Rajagopal", "given_name": "Jayadev K.", "clpid": "Rajagopal-J-K" } ], "abstract": "Recently, the Keck interferometer was upgraded to do self-phase-referencing (SPR) assisted K-band spectroscopy at R ~ 2000. This means, combining a spectral resolution of 150 km/s with an angular resolution of 2.7 mas, while maintaining high sensitiviy. This SPR mode operates two fringe trackers in parallel, and explores several infrastructural requirements for off-axis phase-referencing, as currently being implemented as the KI-ASTRA project. The technology of self-phasereferencing opens the way to reach very high spectral resolution in near-infrared interferometry. We present the scientific capabilities of the KI-SPR mode in detail, at the example of observations of the Be-star 48 Lib. Several spectral lines of the cirumstellar disk are resolved. We describe the first detection of Pfund-lines in an interferometric spectrum of a Be star, in addition to Br \u03b3. The differential phase signal can be used to (i) distinguish circum-stellar line emission from the star, (ii) to directly measure line asymmetries tracing an asymetric gas density distribution, (iii) to reach a differential, astrometric precision beyond single-telescope limits sufficient for studying the radial disk structure. Our data support the existence of a radius-dependent disk density perturbation, typically used to explain slow variations of Be-disk hydrogen line profiles.", "doi": "10.1117/12.856922", "isbn": "9780819482242", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2010-07-21", "pages": "Art. No. 77340P" }, { "id": "authors:k8x6w-1e781", "collection": "authors", "collection_id": "k8x6w-1e781", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161108-131913267", "type": "book_section", "title": "Science with the Keck Interferometer ASTRA program", "book_title": "Optical and Infrared Interferometry II", "author": [ { "family_name": "Eisner", "given_name": "J. A.", "clpid": "Eisner-J-A" }, { "family_name": "Akeson", "given_name": "R.", "orcid": "0000-0001-9674-1564", "clpid": "Akeson-R-L" }, { "family_name": "Colavita", "given_name": "M.", "clpid": "Colavita-M-M" }, { "family_name": "Ghez", "given_name": "A.", "orcid": "0000-0003-3230-5055", "clpid": "Ghez-A-M" }, { "family_name": "Graham", "given_name": "J.", "clpid": "Graham-J" }, { "family_name": "Hillenbrand", "given_name": "L.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Millan-Gabet", "given_name": "R.", "orcid": "0000-0003-0447-5866", "clpid": "Millan-Gabet-R" }, { "family_name": "Monnier", "given_name": "J. D.", "orcid": "0000-0002-3380-3307", "clpid": "Monnier-J-D" }, { "family_name": "Pott", "given_name": "J. U.", "orcid": "0000-0003-4291-2078", "clpid": "Pott-J-U" }, { "family_name": "Ragland", "given_name": "S.", "clpid": "Ragland-S-D" }, { "family_name": "Wizinowich", "given_name": "P.", "orcid": "0000-0002-1646-442X", "clpid": "Wizinowich-P-L" }, { "family_name": "Woillez", "given_name": "J.", "clpid": "Woillez-J-M" } ], "contributor": [ { "family_name": "Danchi", "given_name": "William C.", "clpid": "Danchi-W-C" }, { "family_name": "Delplancke", "given_name": "Fran\u00e7oise", "clpid": "Delplancke-F" }, { "family_name": "Rajagopal", "given_name": "Jayadev K.", "clpid": "Rajagopal-J-K" } ], "abstract": "The ASTrometric and phase-Referenced Astronomy (ASTRA) project will provide phase referencing and astrometric observations at the Keck Interferometer, leading to enhanced sensitivity and the ability to monitor orbits at an accuracy level of 30-100 microarcseconds. Here we discuss recent scientific results from ASTRA, and describe new scientific programs that will begin in 2010-2011. We begin with results from the \"self phase referencing\" (SPR) mode of ASTRA, which uses continuum light to correct atmospheric phase variations and produce a phase-stabilized channel for spectroscopy. We have observed a number of protoplanetary disks using SPR and a grism providing a spectral dispersion of ~ 2000. In our data we spatially resolve emission from dust as well as gas. Hydrogen line emission is spectrally resolved, allowing differential phase measurements across the emission line that constrain the relative centroids of different velocity components at the 10 microarcsecond level. In the upcoming year, we will begin dual-field phase referencing (DFPR) measurements of the Galactic Center and a number of exoplanet systems. These observations will, in part, serve as precursors to astrometric monitoring of stellar orbits in the Galactic Center and stellar wobbles of exoplanet host stars. We describe the design of several scientific investigations capitalizing on the upcoming phase-referencing and astrometric capabilities of ASTRA.", "doi": "10.1117/12.856418", "isbn": "978-0-8194-8224-2", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_publication": "Bellingham, WA", "publication_date": "2010-07-21", "pages": "Art. No. 773411" }, { "id": "authors:t8pcz-bng42", "collection": "authors", "collection_id": "t8pcz-bng42", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161101-102709293", "type": "book_section", "title": "ASTRA: astrometry and phase-referencing astronomy on the Keck interferometer", "book_title": "Optical and Infrared Interferometry II", "author": [ { "family_name": "Woillez", "given_name": "J.", "clpid": "Woillez-J" }, { "family_name": "Akeson", "given_name": "R.", "orcid": "0000-0001-9674-1564", "clpid": "Akeson-R-L" }, { "family_name": "Hillenbrand", "given_name": "L.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Millan-Gabet", "given_name": "R.", "orcid": "0000-0003-0447-5866", "clpid": "Millan-Gabet-R" }, { "family_name": "Felizardo", "given_name": "C.", "clpid": "Felizardo-C" }, { "family_name": "Herstein", "given_name": "J.", "clpid": "Herstein-J" } ], "contributor": [ { "family_name": "Danchi", "given_name": "William C.", "clpid": "Danchi-W-C" }, { "family_name": "Delplanque", "given_name": "Fran\u00e7oise", "clpid": "Delplanque-F" }, { "family_name": "Rajagopal", "given_name": "Jayadev K.", "clpid": "Rajagopal-J-K" } ], "abstract": "ASTRA (ASTrometric and phase-Referencing Astronomy) is an upgrade to the existing Keck Interferometer which aims at providing new self-phase referencing (high spectral resolution observation of YSOs), dual-field phase referencing (sensitive AGN observations), and astrometric (known exoplanetary systems characterization and galactic center general relativity in strong field regime) capabilities. With the first high spectral resolution mode now offered to the community, this contribution focuses on the progress of the dual field and astrometric modes.", "doi": "10.1117/12.857740", "isbn": "978-0-8194-8224-2", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2010-07-21", "pages": "Art. No. 773412" }, { "id": "authors:pvz08-91b92", "collection": "authors", "collection_id": "pvz08-91b92", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110418-112715701", "type": "book_section", "title": "400 Years of Astronomical Discovery: The Accelerating Understanding of our Place in the Universe", "book_title": "Science Education and Outreach: Forging a Path to the Future", "author": [ { "family_name": "Hillenbrand", "given_name": "Lynne A.", "clpid": "Hillenbrand-L-A" } ], "contributor": [ { "family_name": "Barnes", "given_name": "Jonathan", "clpid": "Barnes-J-C" }, { "family_name": "Smith", "given_name": "Denise A.", "clpid": "Smith-D-A" }, { "family_name": "Gibbs", "given_name": "Michael G.", "clpid": "Gibbs-M-G" }, { "family_name": "Manning", "given_name": "James G.", "clpid": "Manning-J-G" } ], "abstract": "This plenary talk is a fast-paced review of the four hundred years of astronomical discovery since Galileo's first use of the telescope.", "isbn": "978-1-58381-742-1", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "2010", "pages": "8-16" }, { "id": "authors:6na3b-j3z79", "collection": "authors", "collection_id": "6na3b-j3z79", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100507-094556646", "type": "book_section", "title": "Measuring tiny mass accretion rates onto young brown dwarfs", "book_title": "COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun St. Andrews (Scotland), 21\u201325 July 2008", "author": [ { "family_name": "Herczeg", "given_name": "Gregory J.", "orcid": "0000-0002-7154-6065", "clpid": "Herczeg-G-J" }, { "family_name": "Cruz", "given_name": "Kelle", "orcid": "0000-0002-1821-0650", "clpid": "Cruz-K-L" }, { "family_name": "Hillenbrand", "given_name": "Lynne A.", "clpid": "Hillenbrand-L-A" } ], "contributor": [ { "family_name": "Stempels", "given_name": "Eric", "clpid": "Stempels-E" } ], "abstract": "We present low-resolution Keck I/LRIS-ADC spectra spanning from 3200\u20139000 \u00c5 of six young brown dwarfs in the TW Hya Association and in Upper Sco. The optical spectral types of the sample range from M7.25\u2013M8.75, though two have near-IR spectral types of early L-dwarfs. For four brown dwarfs in our sample, the accretion luminosity is measurable only when the image is binned over large wavelength intervals. This method extends our sensivity to accretion rate down to ~10^(\u221213) M_\u2609 yr^(\u22121) for brown dwarfs.", "doi": "10.1063/1.3099165", "isbn": "978-0-7354-0627-8", "publisher": "American Institute of Physics", "place_of_publication": "Melville, NY", "publication_date": "2009-02-16", "pages": "529-532" }, { "id": "authors:bhzks-n0935", "collection": "authors", "collection_id": "bhzks-n0935", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100510-100817359", "type": "book_section", "title": "Stellar Age Estimation from 3 Myr to 3 Gyr", "book_title": "Cool Stars, Stellar Systems And The Sun: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun St. Andrews (Scotland), 21\u201325 July 2008", "author": [ { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" }, { "family_name": "Mamajek", "given_name": "Eric", "orcid": "0000-0003-2008-1488", "clpid": "Mamajek-E-E" }, { "family_name": "Stauffer", "given_name": "John", "orcid": "0000-0003-3595-7382", "clpid": "Stauffer-J-R" }, { "family_name": "Soderblom", "given_name": "David", "orcid": "0000-0002-0322-8161", "clpid": "Soderblom-D-R" }, { "family_name": "Carpenter", "given_name": "John", "orcid": "0000-0003-2251-0602", "clpid": "Carpenter-J-M" }, { "family_name": "Meyer", "given_name": "Michael", "orcid": "0000-0003-1227-3084", "clpid": "Meyer-M-R" } ], "contributor": [ { "family_name": "Stempels", "given_name": "Eric", "clpid": "Stempels-E" } ], "abstract": "We present recent progress on quantitative estimation of stellar ages using indicators such as theoretical evolutionary tracks, rotation, rotation-driven chromospheric and coronal activity, and lithium depletion. Our focus is on roughly solar-mass and solar-metallicity stars younger than the Sun. We attempt to characterize the systematic and random error sources and then derive \"best\" ages along with the dispersion in age arising among the various age estimation methods. Our main application of these techniques is to the evolution of debris disks.", "doi": "10.1063/1.3099237", "isbn": "978-0-7354-0627-8", "publisher": "American Institute of Physics", "place_of_publication": "New York, NY", "publication_date": "2009-02-16", "pages": "800-803" }, { "id": "authors:1066d-jde47", "collection": "authors", "collection_id": "1066d-jde47", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100506-142952555", "type": "book_section", "title": "Age-related observations of low mass pre-main and young main sequence stars", "book_title": "The Ages of Stars", "author": [ { "family_name": "Hillenbrand", "given_name": "Lynne A.", "clpid": "Hillenbrand-L-A" } ], "abstract": "This overview summarizes the age dating methods available for young sub-solar mass stars. Pre-main sequence age diagnostics include the Hertzsprung-Russell (HR) diagram, spectroscopic surface gravity indicators, and lithium depletion; asteroseismology is also showing recent promise. Near and beyond the zero-age main sequence, rotation period or vsini and activity (coronal and chromospheric) diagnostics along with lithium depletion serve as age proxies. Other authors in this volume present more detail in each of the aforementioned areas. Herein, I focus on pre-main sequence HR diagrams and address the questions: Do empirical young cluster isochrones match theoretical isochrones? Do isochrones predict stellar ages consistent with those derived via other independent techniques? Do the observed apparent luminosity spreads at constant effective temperature correspond to true age spreads? While definitive answers to these questions are not provided, some methods of progression are outlined.", "doi": "10.1017/S1743921309031731", "isbn": "9780521889896", "publisher": "Cambridge University Press", "publication_date": "2008-10", "pages": "81-94" }, { "id": "authors:etf6a-0mw93", "collection": "authors", "collection_id": "etf6a-0mw93", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:HILstsiss08", "type": "book_section", "title": "Observational constraints on dust disk lifetimes : implications for planet formation", "book_title": "A Decade of extrasolar planets around normal stars : proceedings of the Space Telescope Science Institute Symposium, held in Baltimore, Maryland May 2-5, 2005", "author": [ { "family_name": "Hillenbrand", "given_name": "L.A.", "clpid": "Hillenbrand-L-A" } ], "contributor": [ { "family_name": "Livio", "given_name": "Mario", "clpid": "Livio-M" }, { "family_name": "Sahu", "given_name": "Kailash", "clpid": "Sahu-K" }, { "family_name": "Valenti", "given_name": "Jeff", "clpid": "Valenti-J" } ], "abstract": "Thus far our impressions regarding the evolutionary time scales for young circumstellar disks\nhave been based on small number statistics. Over the past decade, however, in addition to preci-\nsion study of individual star/disk systems, substantial observational effort has been invested in\nobtaining less detailed data on large numbers of objects in young star clusters. This has resulted\nin a plethora of information now enabling statistical studies of disk evolutionary diagnostics.\nAlong an ordinate one can measure disk presence or strength through indicators such as ul-\ntraviolet/blue excess or spectroscopic emission lines tracing accretion, infrared excess tracing\ndust, or millimeter flux measuring mass. Along an abscissa one can track stellar age. While\nbulk trends in disk indicators versus age are evident, observational errors affecting both axes,\ncombined with systematic errors in our understanding of stellar ages, both cloud and bias any\nsuch trends. Thus detailed understanding of the physical processes involved in disk dissipation\nand of the relevant time scales remains elusive. Nevertheless, a clear effect in current data that\nis unlikely to be altered by data analysis improvements is the dispersion in disk lifetimes. Inner\naccretion disks are traced by near-infrared emission. Moderating a generally declining trend in\nnear-infared continuum excess and excess frequency with age over <1 to 8\u00b14 Myr, is the fact\nthat a substantial fraction of rather young (<1 Myr old) stars apparently have already lost their\ninner accretion disks while a significant number of rather old (8-16 Myr) stars apparently still\nretain inner accretion disks. The age at which evidence for inner accretion disks ceases to be\napparent for the vast majority (~90%) of stars is in the range 3-8 Myr. More distant, terrestrial\nzone dust is traced by mid-infrared emission where sufficient sensitivity and uniform data collec-\ntion are only now being realized with data return from the Spitzer Space Telescope. Constraints\non mid-disk dissipation and disk clearing trends with radius are forthcoming.", "isbn": "9780521897846", "publisher": "Cambridge University Press", "place_of_publication": "New York", "publication_date": "2008-06", "pages": "84-105" }, { "id": "authors:6y93f-e8241", "collection": "authors", "collection_id": "6y93f-e8241", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100715-134358160", "type": "book_section", "title": "An assessment of HR diagram constraints on ages and age spreads in star-forming regions and young clusters", "book_title": "14th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun", "author": [ { "family_name": "Hillenbrand", "given_name": "Lynne A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Bauermeister", "given_name": "Amber", "clpid": "Bauermeister-A" }, { "family_name": "White", "given_name": "Russel J.", "orcid": "0000-0001-5313-7498", "clpid": "White-R-J" } ], "abstract": "Pre-main sequence evolutionary theory is not well-calibrated to\nobservations. With care, the observed quantities can be converted into effective\ntemperature and luminosity (i.e. the Hertzsprung-Russell diagram) which the\ntheoretical calculations also predict as a function of stellar mass and age. For a\nsample of nearby young stellar clusters and associations ranging in age from <1\nMyr to >100 Myr, we have tested the loci of luminosity as a function of effective\ntemperature against various sets of predicted pre-main sequence isochrones. As\nwe found in Hillenbrand & White (2004) which tested stellar masses, here for\nthe stellar ages there are two conclusions: some evolutionary calculations fare\nbetter than others in reproducing the empirical sequences, and systematic differences\nbetween all pre-main sequence evolutionary calculations and the data\nare apparent. We also simulate hypothetical clusters of varying star formation\nhistory and compare the resulting HR diagram predictions to observed clusters.\nOur efforts are directed towards quantitative assessment of apparent luminosity\nspreads in star forming regions and young clusters, which are often erroneously\ninterpreted as true luminosity spreads indicative of true age spreads.", "isbn": "978-1-58381-331-7", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco", "publication_date": "2008", "pages": "200-213" }, { "id": "authors:ah7h5-ktk07", "collection": "authors", "collection_id": "ah7h5-ktk07", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191127-100958634", "type": "book_section", "title": "Formation and Evolution of Planetary Systems: SIRTF Legacy Science in the VLT Era", "book_title": "The Origin of Stars and Planets: The VLT View", "author": [ { "family_name": "Meyer", "given_name": "M. R.", "orcid": "0000-0003-1227-3084", "clpid": "Meyer-M-R" }, { "family_name": "Backman", "given_name": "D.", "clpid": "Backman-D-E" }, { "family_name": "Beckwith", "given_name": "S. V. W.", "clpid": "Beckwith-S-V-W" }, { "family_name": "Brooke", "given_name": "T. Y.", "clpid": "Brooke-T-Y" }, { "family_name": "Carpenter", "given_name": "J. M.", "orcid": "0000-0003-2251-0602", "clpid": "Carpenter-J-M" }, { "family_name": "Cohen", "given_name": "M.", "orcid": "0000-0002-8033-5972", "clpid": "Cohen-M-H" }, { "family_name": "Gorti", "given_name": "U.", "clpid": "Gorti-U" }, { "family_name": "Henning", "given_name": "T.", "clpid": "Henning-Thomas" }, { "family_name": "Hillenbrand", "given_name": "L. A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Hines", "given_name": "D.", "orcid": "0000-0003-4653-6161", "clpid": "Hines-D-C" }, { "family_name": "Hollenbach", "given_name": "D.", "clpid": "Hollenbach-D-J" }, { "family_name": "Lunine", "given_name": "J.", "orcid": "0000-0003-2279-4131", "clpid": "Lunine-Jonathan-Irving" }, { "family_name": "Malhotra", "given_name": "R.", "orcid": "0000-0002-1226-3305", "clpid": "Malhotra-Renu" }, { "family_name": "Mamajek", "given_name": "E.", "orcid": "0000-0003-2008-1488", "clpid": "Mamajek-E-E" }, { "family_name": "Morris", "given_name": "P.", "orcid": "0000-0002-5186-4381", "clpid": "Morris-P-W" }, { "family_name": "Najita", "given_name": "J.", "clpid": "Najita-Joan-R" }, { "family_name": "Padgett", "given_name": "D. L.", "orcid": "0000-0001-5334-5107", "clpid": "Padgett-D-L" }, { "family_name": "Soderblom", "given_name": "D.", "orcid": "0000-0002-0322-8161", "clpid": "Soderblom-D-R" }, { "family_name": "Stauffer", "given_name": "J.", "orcid": "0000-0003-3595-7382", "clpid": "Stauffer-J-R" }, { "family_name": "Strom", "given_name": "S. E.", "clpid": "Strom-S-E" }, { "family_name": "Watson", "given_name": "D.", "clpid": "Watson-D" }, { "family_name": "Weidenschilling", "given_name": "S.", "clpid": "Weidenschilling-S" }, { "family_name": "Young", "given_name": "E.", "clpid": "Young-E-T" } ], "contributor": [ { "family_name": "Alves", "given_name": "Jo\u00e3o F.", "clpid": "Alves-J-F" }, { "family_name": "McCaughrean", "given_name": "Mark J.", "clpid": "McCaughrean-M-J" } ], "abstract": "We will utilize the sensitivity of SIRTF through the Legacy Science Program to carry out spectrophotometric observations of solar-type stars aimed at (1) defining the timescales over which terrestrial and gas giant planets are built, from measurements diagnostic of dust/gas masses and radial distributions; and (2) establishing the diversity of planetary architectures and the frequency of planetesimal collisions as a function of time through observations of circumstellar debris disks. Together, these observations will provide an astronomical context for understanding whether our solar system - and its habitable planet - is a common or a rare circumstance.\n\nAchieving our science goals requires measuring precise spectral energy distributions for a statistically robust sample capable of revealing evolutionary trends and the diversity of system outcomes. Our targets have been selected from two carefully assembled databases of solar-like stars: (1) a sample located within 50 pc of the Sun spanning an age range from 100-3000 Myr for which a rich set of ancillary measurements (e.g. metallicity, stellar activity, kinematics) are available; and (2) a selection located between 15 and 180 pc and spanning ages from 3 to 100 Myr. For stars at these distances SIRTF is capable of detecting stellar photospheres with SNR >30 at \u03bb\u226424\u03bc m for our entire sample, as well as achieving SNR >5 at the photospheric limit for over 50% of our sample at \u03bb=70\u03bc m. Thus we will provide a complete census of stars with excess emission down to the level produced by the dust in our present-day solar system.\n\nSIRTF observations obtained as part of this program will provide a rich Legacy for follow-up observations utilizing a variety of facilities including the VLT. More information concerning our program can be found at http://gould.as.arizona.edu/feps.", "doi": "10.1007/10856518_60", "isbn": "978-3-540-43541-9", "publisher": "Springer", "place_of_publication": "Berlin", "publication_date": "2003-10-15", "pages": "463-472" }, { "id": "authors:3279e-p2j26", "collection": "authors", "collection_id": "3279e-p2j26", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200610-082408943", "type": "book_section", "title": "Mass Function of Newly Formed Stars", "book_title": "The Dense Interstellar Medium in Galaxies", "author": [ { "family_name": "Hillenbrand", "given_name": "L. A.", "clpid": "Hillenbrand-L-A" } ], "contributor": [ { "family_name": "Pfalzner", "given_name": "Susanne", "clpid": "Pfalzner-S" }, { "family_name": "Kramer", "given_name": "Carsten", "clpid": "Kramer-C" }, { "family_name": "Straubmeier", "given_name": "Christian", "clpid": "Straubmeier-C" }, { "family_name": "Heithausen", "given_name": "Andreas", "clpid": "Heithausen-A" } ], "abstract": "The topic of the stellar \"original mass function\" has a nearly 50 year history, dating to the publication in 1955 of Salpeter's seminal paper. In this review I discuss the many more recent results that have emerged on the initial mass function (IMF), as it is now called, from studies over the last decade of resolved populations in star forming regions and young open clusters.", "doi": "10.1007/978-3-642-18902-9_105", "isbn": "978-3-642-62348-6", "publisher": "Springer", "place_of_publication": "Berlin", "publication_date": "1997", "pages": "601-609" } ]