[ { "id": "authors:fap34-kq043", "collection": "authors", "collection_id": "fap34-kq043", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090817-112331560", "type": "article", "title": "SPACE: the spectroscopic all-sky cosmic explorer", "author": [ { "family_name": "Cimatti", "given_name": "A.", "clpid": "Cimatti-A" }, { "family_name": "Robberto", "given_name": "M.", "clpid": "Robberto-M" }, { "family_name": "Baugh", "given_name": "C.", "orcid": "0000-0002-9935-9755", "clpid": "Baugh-C-M" }, { "family_name": "Beckwith", "given_name": "S. V. W.", "clpid": "Beckwith-S-V-W" }, { "family_name": "Content", "given_name": "R.", "clpid": "Content-R" }, { "family_name": "Daddi", "given_name": "E.", "orcid": "0000-0002-3331-9590", "clpid": "Daddi-Emanuele" }, { "family_name": "De Lucia", "given_name": "G.", "clpid": "De-Lucia-G" }, { "family_name": "Garilli", "given_name": "B.", "clpid": "Garilli-B" }, { "family_name": "Guzzo", "given_name": "L.", "clpid": "Guzzo-L" }, { "family_name": "Kauffmann", "given_name": "G.", "clpid": "Kauffmann-G" }, { "family_name": "Lehnert", "given_name": "M.", "orcid": "0000-0003-1939-5885", "clpid": "Lehnert-Matthew-D" }, { "family_name": "Maccagni", "given_name": "D.", "clpid": "Maccagni-D" }, { "family_name": "Mart\u00ednez-Sansigre", "given_name": "Alejo", "clpid": "Mart\u00ednez-Sansigre-A" }, { "family_name": "Pasian", "given_name": "F.", "clpid": "Pasian-F" }, { "family_name": "Reid", "given_name": "I. N.", "clpid": "Reid-I-N" }, { "family_name": "Rosati", "given_name": "P.", "clpid": "Rosati-P" }, { "family_name": "Salvaterra", "given_name": "R.", "clpid": "Salvaterra-R" }, { "family_name": "Stiavelli", "given_name": "M.", "orcid": "0000-0001-9935-6047", "clpid": "Stiavelli-Massimo" }, { "family_name": "Wang", "given_name": "Y.", "clpid": "Wang-Y" }, { "family_name": "Zapatero Osorio", "given_name": "M.", "clpid": "Zapatero-Osorio-M-R" }, { "family_name": "Balcells", "given_name": "M.", "clpid": "Balcells-M" }, { "family_name": "Bersanelli", "given_name": "M.", "clpid": "Bersanelli-M" }, { "family_name": "Bertoldi", "given_name": "F.", "orcid": "0000-0002-1707-1775", "clpid": "Bertoldi-F" }, { "family_name": "Blaizot", "given_name": "J.", "clpid": "Blaizot-J" }, { "family_name": "Bottini", "given_name": "D.", "clpid": "Bottini-D" }, { "family_name": "Bower", "given_name": "R.", "clpid": "Bower-R-G" }, { "family_name": "Bulgarelli", "given_name": "A.", "clpid": "Bulgarelli-A" }, { "family_name": "Burgasser", "given_name": "A.", "orcid": "0000-0002-6523-9536", "clpid": "Burgasser-A-J" }, { "family_name": "Burigana", "given_name": "C", "clpid": "Burigana-C" }, { "family_name": "Butler", "given_name": "R. C.", "clpid": "Butler-R-C" }, { "family_name": "Casertano", "given_name": "S.", "clpid": "Casertano-S" }, { "family_name": "Ciardi", "given_name": "B.", "clpid": "Ciardi-B" }, { "family_name": "Cirasuolo", "given_name": "M.", "clpid": "Cirasuolo-M" }, { "family_name": "Clampin", "given_name": "M.", "clpid": "Clampin-M-C" }, { "family_name": "Cole", "given_name": "S.", "clpid": "Cole-S" }, { "family_name": "Comastri", "given_name": "A.", "orcid": "0000-0003-3451-9970", "clpid": "Comastri-A" }, { "family_name": "Cristiani", "given_name": "S.", "clpid": "Cristiani-S" }, { "family_name": "Cuby", "given_name": "J. G.", "clpid": "Cuby-J-G" }, { "family_name": "Cuttaia", "given_name": "F.", "clpid": "Cuttaia-F" }, { "family_name": "De Rosa", "given_name": "A.", "orcid": "0000-0001-5668-6863", "clpid": "De-Rosa-A" }, { "family_name": "Diaz Sanchez", "given_name": "A.", "clpid": "Diaz-Sanchez-A" }, { "family_name": "Di Capua", "given_name": "M.", "clpid": "Di-Capua-M" }, { "family_name": "Dunlop", "given_name": "J.", "clpid": "Dunlop-J-S" }, { "family_name": "Fan", "given_name": "X.", "orcid": "0000-0003-3310-0131", "clpid": "Fan-Xiaohui" }, { "family_name": "Ferrara", "given_name": "A.", "orcid": "0000-0002-9400-7312", "clpid": "Ferrara-A" }, { "family_name": "Finelli", "given_name": "F.", "clpid": "Finelli-F" }, { "family_name": "Franceschini", "given_name": "A.", "clpid": "Franceschini-A" }, { "family_name": "Franx", "given_name": "M.", "orcid": "0000-0002-8871-3026", "clpid": "Franx-M" }, { "family_name": "Franzetti", "given_name": "P.", "clpid": "Franzetti-P" }, { "family_name": "Frenk", "given_name": "C.", "clpid": "Frenk-C-S" }, { "family_name": "Gardner", "given_name": "Jonathan P.", "clpid": "Gardner-J-P" }, { "family_name": "Gianotti", "given_name": "F.", "clpid": "Gianotti-F" }, { "family_name": "Grange", "given_name": "R.", "clpid": "Grange-R" }, { "family_name": "Gruppioni", "given_name": "C.", "orcid": "0000-0002-5836-4056", "clpid": "Gruppioni-C" }, { "family_name": "Gruppuso", "given_name": "A.", "clpid": "Gruppuso-A" }, { "family_name": "Hammer", "given_name": "F.", "clpid": "Hammer-F" }, { "family_name": "Hillenbrand", "given_name": "L.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Jacobsen", "given_name": "A.", "clpid": "Jacobsen-A-J" }, { "family_name": "Jarvis", "given_name": "M.", "orcid": "0000-0001-7039-9078", "clpid": "Jarvis-M-J" }, { "family_name": "Kennicutt", "given_name": "R.", "orcid": "0000-0001-5448-1821", "clpid": "Kennicutt-R-C" }, { "family_name": "Kimble", "given_name": "R.", "clpid": "Kimble-Randy-A" }, { "family_name": "Kriek", "given_name": "M.", "orcid": "0000-0002-7613-9872", "clpid": "Kriek-M" }, { "family_name": "Kurk", "given_name": "J.", "clpid": "Kurk-J-D" }, { "family_name": "Kneib", "given_name": "J. P.", "orcid": "0000-0002-4616-4989", "clpid": "Kneib-J-P" }, { "family_name": "Le F\u00e8vre", "given_name": "O.", "orcid": "0000-0001-5891-2596", "clpid": "Le-F\u00e8vre-O" }, { "family_name": "Macchetto", "given_name": "D.", "clpid": "Macchetto-D" }, { "family_name": "MacKenty", "given_name": "J.", "clpid": "MacKenty-J" }, { "family_name": "Madau", "given_name": "P.", "clpid": "Madau-P" }, { "family_name": "Magliocchetti", "given_name": "M.", "clpid": "Magliocchetti-M" }, { "family_name": "Maino", "given_name": "D.", "clpid": "Maino-D" }, { "family_name": "Mandolesi", "given_name": "N.", "clpid": "Mandolesi-N" }, { "family_name": "Masetti", "given_name": "N.", "orcid": "0000-0001-9487-7740", "clpid": "Masetti-N" }, { "family_name": "McLure", "given_name": "R.", "clpid": "McLure-R-J" }, { "family_name": "Mennella", "given_name": "A.", "clpid": "Mennella-A" }, { "family_name": "Meyer", "given_name": "M.", "orcid": "0000-0003-1227-3084", "clpid": "Meyer-M-R" }, { "family_name": "Mignoli", "given_name": "M.", "clpid": "Mignoli-M" }, { "family_name": "Mobasher", "given_name": "B.", "clpid": "Mobasher-B" }, { "family_name": "Molinari", "given_name": "E.", "clpid": "Molinari-E" }, { "family_name": "Morgante", "given_name": "G.", "clpid": "Morgante-G" }, { "family_name": "Morris", "given_name": "S.", "clpid": "Morris-S" }, { "family_name": "Nicastro", "given_name": "L.", "clpid": "Nicastro-L" }, { "family_name": "Oliva", "given_name": "E.", "clpid": "Oliva-E" }, { "family_name": "Padovani", "given_name": "P.", "clpid": "Padovani-P" }, { "family_name": "Palazzi", "given_name": "E.", "clpid": "Palazzi-E" }, { "family_name": "Paresce", "given_name": "F.", "clpid": "Paresce-F" }, { "family_name": "Perez Garrido", "given_name": "A.", "clpid": "Perez-Garrido-A" }, { "family_name": "Pian", "given_name": "E.", "clpid": "Pian-E" }, { "family_name": "Popa", "given_name": "L.", "clpid": "Popa-L" }, { "family_name": "Postman", "given_name": "M.", "orcid": "0000-0002-9365-7989", "clpid": "Postman-Marc" }, { "family_name": "Pozzetti", "given_name": "L.", "clpid": "Pozzetti-L" }, { "family_name": "Rayner", "given_name": "J.", "clpid": "Rayner-J" }, { "family_name": "Rebolo", "given_name": "R.", "orcid": "0000-0003-3767-7085", "clpid": "Rebolo-R" }, { "family_name": "Renzini", "given_name": "A.", "orcid": "0000-0002-7093-7355", "clpid": "Renzini-A" }, { "family_name": "R\u00f6ttgering", "given_name": "H.", "clpid": "R\u00f6ttgering-H-J-A" }, { "family_name": "Schinnerer", "given_name": "E.", "orcid": "0000-0002-3933-7677", "clpid": "Schinnerer-E" }, { "family_name": "Scodeggio", "given_name": "M.", "clpid": "Scodeggio-M" }, { "family_name": "Saisse", "given_name": "M.", "clpid": "Saisse-M" }, { "family_name": "Shanks", "given_name": "T.", "clpid": "Shanks-T" }, { "family_name": "Shapley", "given_name": "A.", "orcid": "0000-0003-3509-4855", "clpid": "Shapley-A-E" }, { "family_name": "Sharples", "given_name": "R.", "clpid": "Sharples-R-M" }, { "family_name": "Shea", "given_name": "H.", "clpid": "Shea-H" }, { "family_name": "Silk", "given_name": "J.", "clpid": "Silk-J" }, { "family_name": "Smail", "given_name": "I.", "orcid": "0000-0003-3037-257X", "clpid": "Smail-Ian-R" }, { "family_name": "Span\u00f3", "given_name": "P.", "clpid": "Span\u00f3-P" }, { "family_name": "Steinacker", "given_name": "J.", "clpid": "Steinacker-J" }, { "family_name": "Stringhetti", "given_name": "L.", "clpid": "Stringhetti-L" }, { "family_name": "Szalay", "given_name": "A.", "clpid": "Szalay-A-S" }, { "family_name": "Tresse", "given_name": "L.", "clpid": "Tresse-L" }, { "family_name": "Trifoglio", "given_name": "M.", "clpid": "Trifoglio-M" }, { "family_name": "Urry", "given_name": "M.", "orcid": "0000-0002-0745-9792", "clpid": "Urry-C-M" }, { "family_name": "Valenziano", "given_name": "L.", "clpid": "Valenziano-L" }, { "family_name": "Villa", "given_name": "F.", "clpid": "Villa-F" }, { "family_name": "Villo Perez", "given_name": "I.", "clpid": "Villo-Perez-I" }, { "family_name": "Walter", "given_name": "F.", "orcid": "0000-0003-4793-7880", "clpid": "Walter-F" }, { "family_name": "Ward", "given_name": "M.", "clpid": "Ward-M-J" }, { "family_name": "White", "given_name": "R.", "clpid": "White-R" }, { "family_name": "White", "given_name": "S.", "clpid": "White-S" }, { "family_name": "Wright", "given_name": "E.", "orcid": "0000-0001-5058-1593", "clpid": "Wright-E-L" }, { "family_name": "Wyse", "given_name": "R.", "clpid": "Wyse-R" }, { "family_name": "Zamorani", "given_name": "G.", "clpid": "Zamorani-G" }, { "family_name": "Zacchei", "given_name": "A.", "clpid": "Zacchei-A" }, { "family_name": "Zeilinger", "given_name": "W. W.", "clpid": "Zeilinger-W-W" }, { "family_name": "Zerbi", "given_name": "F.", "clpid": "Zerbi-F" }, { "literal": "SPACE Team" } ], "abstract": "We describe the scientific motivations, the mission concept and the instrumentation of SPACE, a class-M mission proposed for concept study at the first call of the ESA Cosmic-Vision 2015\u20132025 planning cycle. SPACE aims to produce the largest three-dimensional evolutionary map of the Universe over the past 10 billion years by taking near-IR spectra and measuring redshifts for more than half a billion galaxies at 0\u2009<\u2009z\u2009<\u20092 down to AB~23 over 3\u03c0 sr of the sky. In addition, SPACE will also target a smaller sky field, performing a deep spectroscopic survey of millions of galaxies to AB~26 and at 2\u2009<\u2009z\u2009<\u200910\u2009+. These goals are unreachable with ground-based observations due to the \u2248500 times higher sky background (see e.g. Aldering, LBNL report number LBNL-51157, 2001). To achieve the main science objectives, SPACE will use a 1.5 m diameter Ritchey-Chretien telescope equipped with a set of arrays of Digital Micro-mirror Devices covering a total field of view of 0.4 deg^2, and will perform large-multiplexing multi-object spectroscopy (e.g. \u22486000 targets per pointing) at a spectral resolution of R~400 as well as diffraction-limited imaging with continuous coverage from 0.8 to 1.8 \u03bcm. Owing to the depth, redshift range, volume coverage and quality of its spectra, SPACE will reveal with unique sensitivity most of the fundamental cosmological signatures, including the power spectrum of density fluctuations and its turnover. SPACE will also place high accuracy constraints on the dark energy equation of state parameter and its evolution by measuring the baryonic acoustic oscillations imprinted when matter and radiation decoupled, the distance-luminosity relation of cosmological supernovae, the evolution of the cosmic expansion rate, the growth rate of cosmic large-scale structure, and high-z galaxy clusters. The datasets from the SPACE mission will represent a long lasting legacy for the whole astronomical community whose data will be mined for many years to come.", "doi": "10.1007/s10686-008-9096-7", "issn": "0922-6435", "publisher": "Springer", "publication": "Experimental Astronomy", "publication_date": "2009-03", "series_number": "1", "volume": "23", "issue": "1", "pages": "39-66" }, { "id": "authors:xmygf-z2868", "collection": "authors", "collection_id": "xmygf-z2868", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091117-151058276", "type": "article", "title": "The Formation and Evolution of Planetary Systems: Placing Our Solar System in Context with Spitzer", "author": [ { "family_name": "Meyer", "given_name": "Michael R.", "orcid": "0000-0003-1227-3084", "clpid": "Meyer-M-R" }, { "family_name": "Hillenbrand", "given_name": "Lynne A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Backman", "given_name": "Dana", "clpid": "Backman-D-E" }, { "family_name": "Beckwith", "given_name": "Steve", "clpid": "Beckwith-S-V-W" }, { "family_name": "Bouwman", "given_name": "Jeroen", "clpid": "Bouwman-J" }, { "family_name": "Brooke", "given_name": "Tim", "clpid": "Brooke-T-Y" }, { "family_name": "Carpenter", "given_name": "John", "orcid": "0000-0003-2251-0602", "clpid": "Carpenter-J-M" }, { "family_name": "Cohen", "given_name": "Martin", "clpid": "Cohen-Martin" }, { "family_name": "Cortes", "given_name": "Stephanie", "clpid": "Cortes-S-R" }, { "family_name": "Crockett", "given_name": "Nathan", "orcid": "0000-0002-6586-7591", "clpid": "Crockett-N-R" }, { "family_name": "Gorti", "given_name": "Uma", "clpid": "Gorti-U" }, { "family_name": "Henning", "given_name": "Thomas", "clpid": "Henning-T" }, { "family_name": "Hines", "given_name": "Dean", "orcid": "0000-0003-4653-6161", "clpid": "Hines-D-C" }, { "family_name": "Hollenbach", "given_name": "David", "clpid": "Hollenbach-D-J" }, { "family_name": "Kim", "given_name": "Jinyoung Serena", "clpid": "Kim-Jinyoung-Serena" }, { "family_name": "Lunine", "given_name": "Jonathan", "orcid": "0000-0003-2279-4131", "clpid": "Lunine-Jonathan-Irving" }, { "family_name": "Malhotra", "given_name": "Renu", "orcid": "0000-0002-1226-3305", "clpid": "Malhotra-Renu" }, { "family_name": "Mamajek", "given_name": "Eric", "orcid": "0000-0003-2008-1488", "clpid": "Mamajek-E-E" }, { "family_name": "Metchev", "given_name": "Stanimir", "orcid": "0000-0003-3050-8203", "clpid": "Metchev-S-A" }, { "family_name": "Moro-Mart\u00edn", "given_name": "Amaya", "orcid": "0000-0001-9504-8426", "clpid": "Moro-Mart\u00edn-A" }, { "family_name": "Morris", "given_name": "Pat", "orcid": "0000-0002-5186-4381", "clpid": "Morris-P-W" }, { "family_name": "Najita", "given_name": "Joan", "clpid": "Najita-Joan-R" }, { "family_name": "Padgett", "given_name": "Deborah", "orcid": "0000-0001-5334-5107", "clpid": "Padgett-D-L" }, { "family_name": "Pascucci", "given_name": "Ilaria", "orcid": "0000-0001-7962-1683", "clpid": "Pascucci-I" }, { "family_name": "Rodmann", "given_name": "Jens", "clpid": "Rodmann-J" }, { "family_name": "Schlingman", "given_name": "Wayne", "clpid": "Schlingman-W" }, { "family_name": "Silverstone", "given_name": "Murray", "clpid": "Silverstone-M-D" }, { "family_name": "Soderblom", "given_name": "David", "orcid": "0000-0002-0322-8161", "clpid": "Soderblom-D-R" }, { "family_name": "Stauffer", "given_name": "John", "orcid": "0000-0003-3595-7382", "clpid": "Stauffer-J-R" }, { "family_name": "Stobie", "given_name": "Elizabeth", "clpid": "Stobie-E-B" }, { "family_name": "Strom", "given_name": "Steve", "clpid": "Strom-S" }, { "family_name": "Watson", "given_name": "Dan", "clpid": "Watson-D-M" }, { "family_name": "Weidenschilling", "given_name": "Stuart", "clpid": "Weidenschilling-S" }, { "family_name": "Wolf", "given_name": "Sebastian", "clpid": "Wolf-S" }, { "family_name": "Young", "given_name": "Erick", "clpid": "Young-E-T" } ], "abstract": "We provide an overview of the Spitzer Legacy Program, Formation and Evolution of Planetary\nSystems, that was proposed in 2000, begun in 2001, and executed aboard the Spitzer Space Telescope between\n2003 and 2006. This program exploits the sensitivity of Spitzer to carry out mid-infrared spectrophotometric\nobservations of solar-type stars. With a sample of ~328 stars ranging in age from ~3 Myr to ~3 Gyr, we trace\nthe evolution of circumstellar gas and dust from primordial planet-building stages in young circumstellar disks\nthrough to older collisionally generated debris disks. When completed, our program will help define the timescales\nover which terrestrial and gas giant planets are built, constrain the frequency of planetesimal collisions as a\nfunction of time, and establish the diversity of mature planetary architectures. In addition to the observational\nprogram, we have coordinated a concomitant theoretical effort aimed at understanding the dynamics of\ncircumstellar dust with and without the effects of embedded planets, dust spectral energy distributions, and atomic\nand molecular gas line emission. Together with the observations, these efforts will provide an astronomical context\nfor understanding whether our solar system\u2014and its habitable planet\u2014is a common or a rare circumstance.\nAdditional information about the FEPS project can be found on the team Web site.", "doi": "10.1086/510099", "issn": "0004-6280", "publisher": "Astronomical Society of the Pacific", "publication": "Publications of the Astronomical Society of the Pacific", "publication_date": "2006-12", "series_number": "850", "volume": "118", "issue": "850", "pages": "1690-1710" }, { "id": "authors:qzbw9-z4869", "collection": "authors", "collection_id": "qzbw9-z4869", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170209-103945183", "type": "article", "title": "Thermal response of Iapetus to an eclipse by Saturn's rings", "author": [ { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-Keith-Astronomy" }, { "family_name": "Nicholson", "given_name": "P. D.", "orcid": "0000-0003-2275-4463", "clpid": "Nicholson-P-D" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Gatley", "given_name": "I.", "clpid": "Gatley-I" }, { "family_name": "Beckwith", "given_name": "S. V. W.", "clpid": "Beckwith-S-V-W" } ], "abstract": "Measurements of Iapetus as seen at 20 and 2.2 \u03bcm in the shadow of Saturn's ring are given, providing the thermal response to a rapidly varying heat input. The 20 \u03bcm thermal emission follows the 2.2 \u03bcm flux input closely. The observations, plus a simple diffusion calculation, imply that the surface of Iapetus is made of material having a very small thermal inertia, probably / \u227e 10Jm^(-2)s^(-\u00bd)K^(-1).", "doi": "10.1016/j.icarus.2005.03.002", "issn": "0019-1035", "publisher": "Elsevier", "publication": "Icarus", "publication_date": "2005-09", "series_number": "1", "volume": "177", "issue": "1", "pages": "63-68" }, { "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:7bppe-dx662", "collection": "authors", "collection_id": "7bppe-dx662", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180228-083611806", "type": "article", "title": "The Calar Alto Deep Imaging Survey: K-band Galaxy number counts", "author": [ { "family_name": "Huang", "given_name": "J.-S.", "clpid": "Huang-J-S" }, { "family_name": "Thompson", "given_name": "D.", "clpid": "Thompson-D" }, { "family_name": "K\u00fcmmel", "given_name": "M. W.", "clpid": "K\u00fcmmel-M-W" }, { "family_name": "Meisenheimer", "given_name": "K.", "clpid": "Meisenheimer-K" }, { "family_name": "Wolf", "given_name": "C.", "orcid": "0000-0002-4569-016X", "clpid": "Wolf-C" }, { "family_name": "Beckwith", "given_name": "S. V. W.", "clpid": "Beckwith-S-V-W" }, { "family_name": "Fockenbrock", "given_name": "R.", "clpid": "Fockenbrock-R" }, { "family_name": "Fried", "given_name": "J. W.", "clpid": "Fried-J-W" }, { "family_name": "Hippelein", "given_name": "H.", "clpid": "Hippelein-H" }, { "family_name": "von Kuhlmann", "given_name": "B.", "clpid": "von-Kuhlmann-B" }, { "family_name": "Phleps", "given_name": "S.", "clpid": "Phleps-S" }, { "family_name": "R\u00f6ser", "given_name": "H.-J.", "clpid": "R\u00f6ser-H-J" }, { "family_name": "Thommes", "given_name": "E.", "clpid": "Thommes-E" } ], "abstract": "We present K-band number counts for the faint galaxies in the Calar Alto Deep Imaging Survey (CADIS). We covered 4 CADIS fields, a total area of 0.2 deg^2, in the broad band filters B, R and K. We detect about 4000 galaxies in the K-band images, with a completeness limit of K = 19.75 mag, and derive the K-band galaxy number counts in the range of 14.25 < K < 19.75 mag. This is the largest medium deep K-band survey to date in this magnitude range. The B- and R-band number counts are also derived, down to completeness limits of B = 24.75 mag and R = 23.25 mag. The K-selected galaxies in this magnitude range are of particular interest, since some medium deep near-infrared surveys have identified breaks of both the slope of the K-band number counts and the mean B - K color at K = 17 ~ 18 mag. There is, however, a significant disagreement in the K-band number counts among the existing surveys. Our large near-infrared selected galaxy sample allows us to establish the presence of a clear break in the slope at K = 17.0 mag from dlog N/dm = 0.64 at brighter magnitudes to dlog N/dm = 0.36 at the fainter end. We construct no-evolution and passive evolution models, and find that the passive evolution model can simultaneously fit the B-, R- and K-band number counts well. The B - K colors show a clear trend to bluer colors for K > 18 mag. We also find that most of the K = 18 \u2013 20 mag galaxies have a B - K color bluer than the prediction of a no-evolution model for an L\u22c6 Sbc galaxy, implying either significant evolution, even for massive galaxies, or the existence of an extra population of small galaxies.", "doi": "10.1051/0004-6361:20010057", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2001-03-04", "series_number": "3", "volume": "368", "issue": "3", "pages": "787-796" }, { "id": "authors:q2cc2-fq641", "collection": "authors", "collection_id": "q2cc2-fq641", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180306-111804723", "type": "article", "title": "Multi-color classification in the calar alto deep imaging survey", "author": [ { "family_name": "Wolf", "given_name": "C.", "orcid": "0000-0002-4569-016X", "clpid": "Wolf-C" }, { "family_name": "Meisenheimer", "given_name": "K.", "clpid": "Meisenheimer-K" }, { "family_name": "R\u00f6ser", "given_name": "H.-J.", "clpid": "R\u00f6ser-H-J" }, { "family_name": "Beckwith", "given_name": "S. V. W.", "clpid": "Beckwith-S-V-W" }, { "family_name": "Chaffee", "given_name": "F. H.,Jr.", "clpid": "Chaffee-F-H-Jr" }, { "family_name": "Friedman", "given_name": "J.", "clpid": "Friedman-J" }, { "family_name": "Hippelein", "given_name": "H.", "clpid": "Hippelein-H" }, { "family_name": "Huang", "given_name": "J.-S.", "clpid": "Huang-J-S" }, { "family_name": "K\u00fcmmel", "given_name": "M.", "clpid": "K\u00fcmmel-M" }, { "family_name": "von Kuhlmann", "given_name": "B.", "clpid": "von-Kuhlmann-B" }, { "family_name": "Maier", "given_name": "C.", "clpid": "Maier-C" }, { "family_name": "Phleps", "given_name": "S.", "clpid": "Phleps-S" }, { "family_name": "Rix", "given_name": "H.-W.", "orcid": "0000-0003-4996-9069", "clpid": "Rix-H-W" }, { "family_name": "Thommes", "given_name": "E.", "clpid": "Thommes-E" }, { "family_name": "Thompson", "given_name": "D.", "clpid": "Thompson-D" } ], "abstract": "We use a multi-color classification method introduced by Wolf et al. ([CITE]) to reliably identify stars, galaxies and quasars in the up to 16-dimensional color space provided by the filter set of the Calar Alto Deep Imaging Survey (CADIS). The samples of stars, galaxies and quasars obtained this way have been used for dedicated studies which are published in separate papers. The classification is good enough to detect quasars rather completely and efficiently without confirmative spectroscopy. The multi-color redshifts are accurate enough for most statistical applications, e.g. evolutionary studies of the galaxy luminosity function. Also, the separation between stars and galaxies reaches deeper than with morphological criteria, so that studies of the stellar population can be extended to fainter levels. We characterize the dataset presently available on the CADIS 1 h-, 9 h- and 16 h-fields. Using Monte-Carlo simulations we model the classification performance expected for CADIS. We present a summary of the classification results on the CADIS database and discuss unclassified objects. More than 99% of the whole catalog sample at R < 22 (more than 95% at R < 23) are successfully classified matching the expectations derived from the simulations. A small number of peculiar objects challenging the classification is discussed in detail. Spectroscopic observations are used to check the reliability of the multi-color classification (6 mistakes among 151 objects with R < 24). From these, we also determine the accuracy of the multi-color redshifts which are rather good for galaxies (\u03c3_z \u2248 0.03) and useful for quasars. We find that the classification performance derived from the simulations compares well with results from the real survey. Finally, we locate areas for potential improvement of the classification.", "doi": "10.1051/0004-6361:20000064", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy & Astrophysics", "publication_date": "2001-01", "series_number": "3", "volume": "365", "issue": "3", "pages": "681-698" }, { "id": "authors:5554k-se596", "collection": "authors", "collection_id": "5554k-se596", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150605-095422672", "type": "article", "title": "Circumstellar disks and the search for neighbouring planetary systems", "author": [ { "family_name": "Beckwith", "given_name": "Steven V. W.", "clpid": "Beckwith-S-V-W" }, { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" } ], "abstract": "The recent discoveries of planets orbiting several 'mature' stars bring new life to the question of just how common other planetary systems might be. Observations of very young stars provide a way to address this question and suggest that a significant number of such stars harbour conditions appropriate for the formation of planetary systems like our own.", "doi": "10.1038/383139a0", "issn": "0028-0836", "publisher": "Nature Publishing Group", "publication": "Nature", "publication_date": "1996-09-12", "series_number": "6596", "volume": "383", "issue": "6596", "pages": "139-144" }, { "id": "authors:7gjgc-p5g68", "collection": "authors", "collection_id": "7gjgc-p5g68", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170227-154325068", "type": "book_section", "title": "Photodissociation Regions in Young PN", "book_title": "Infrared Astronomy with Arrays: The Next Generation", "author": [ { "family_name": "Graham", "given_name": "James R.", "clpid": "Graham-J-R" }, { "family_name": "Herbst", "given_name": "T. M.", "clpid": "Herbst-T-M" }, { "family_name": "Beckwith", "given_name": "S.", "clpid": "Beckwith-S-V-W" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Serabyn", "given_name": "E.", "clpid": "Serabyn-E" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" } ], "contributor": [ { "family_name": "McLean", "given_name": "Ian S.", "clpid": "McLean-I-S" } ], "abstract": "Infrared imaging of H2 and PAH emission in NGG 7027 and BD+30 3639 reveals the presence of photodissociation regions in the neutral gas surrounding these young planetary nebulae.", "doi": "10.1007/978-94-011-1070-9_15", "isbn": "978-94-010-4466-0", "publisher": "Springer", "place_of_publication": "Dordrecht", "publication_date": "1994", "pages": "69-72" }, { "id": "authors:qzwqt-3kp62", "collection": "authors", "collection_id": "qzwqt-3kp62", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-070004355", "type": "article", "title": "H_2 morphology of young planetary nebulae", "author": [ { "family_name": "Graham", "given_name": "James R.", "clpid": "Graham-J-R" }, { "family_name": "Herbst", "given_name": "T. M.", "clpid": "Herbst-T-M" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Serabyn", "given_name": "E.", "clpid": "Serabyn-E" }, { "family_name": "Beckwith", "given_name": "S.", "clpid": "Beckwith-S-V-W" } ], "abstract": "The distributions of H_2 1-0 S(l) emission in the young planetary nebulae BD +30\u00b03639 and NGC 7027 show striking similarities: both have limb-brightened arcs of H_2 emission with radii that are about twice those of their H II regions. The extended H_2 emission in both nebulae is attributed to a photodissociation region. This implies that the neutral envelopes of these young planetaries extend well beyond the edge of the H II region, in contrast to older nebulae where the ionized and molecular gas are more nearly coextensive. The contrast between young and old planetaries can only be explained if the molecular envelope is inhomogeneous. We endorse a scenario for the evolution of a planetary nebula in which a photodissociation front propagates through the clumpy molecular envelope, leaving the ionized core embedded in an envelope of partially ionized atomic gas and dense molecular knots. In an evolved planetary, the H II region has expanded to engulf some of the dense molecular knots, which can be identified with bright [O I] and H_2 1-0 S(l) condensations, while the remnant of the photodissociated envelope may be detected as a faint optical halo.", "doi": "10.1086/186842", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1993-05-10", "series_number": "2", "volume": "408", "issue": "2", "pages": "L105-L107" }, { "id": "authors:d3vkb-hdb04", "collection": "authors", "collection_id": "d3vkb-hdb04", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170228-145632241", "type": "article", "title": "A spatially resolved photodissociation region in the planetary nebula NGC 7027", "author": [ { "family_name": "Graham", "given_name": "James R.", "clpid": "Graham-J-R" }, { "family_name": "Serabyn", "given_name": "E.", "clpid": "Serabyn-E" }, { "family_name": "Herbst", "given_name": "T. M.", "clpid": "Herbst-T-M" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Wilson", "given_name": "T. D.", "clpid": "Wilson-T-D" }, { "family_name": "Beckwith", "given_name": "S.", "clpid": "Beckwith-S-V-W" } ], "abstract": "High spatial resolution, narrow band, infrared line images and CO (1\u20140) mm interferometer data are presented for NGC 7027. These data trace emission from the central H II region (Br\u0251), the intermediate photodissociation region [H_2 1\u20140S(1) and 3.3 \u00b5m dust feature], and the molecular circumstellar envelope [CO (1\u20140)]. The H II region lies in a cavity in the CO envelope, and consists of a smooth elliptical shell. A striking change of morphology is seen in the H_2 emission and the dust feature. The H_2 1\u20140 S(l) emission is composed of two components: (1) an incomplete elliptical ring of knots which bounds the ionized gas; (2) a remarkable thin shell which loops around the H II region with fourfold symmetry. The dust emission is similar to that from the ionized gas, but is displaced further from the center, and extends at low surface brightness into four \"ears\" which fill in the bays delineated by the outermost loops of H_2 emission. No 3.3 \u00b5m emission is detectable beyond the outer H_2 shell. The outer loops of H_2 emission and the 3.3 \u00b5m emission occupy the region between the edge of the H II region and the inner edge of the molecular gas. It is natural to ascribe the morphology of NGC 7027 to a photodissociation region which separates the ionized and molecular gas. If this is correct then the exterior H_2 loops are due to molecular gas heated by the far-UV emission escaping from the H II region, and delineate a photodissociation front. The H_2 and CO kinematics rule out shock excitation of the H_2 emission and favor UV excitation.", "doi": "10.1086/116423", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "1993-01", "series_number": "1", "volume": "105", "issue": "1", "pages": "250-257" }, { "id": "authors:qhatd-n6534", "collection": "authors", "collection_id": "qhatd-n6534", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-075023575", "type": "article", "title": "Diffraction limited infrared images of the binary star T Tauri", "author": [ { "family_name": "Ghez", "given_name": "A. M.", "orcid": "0000-0003-3230-5055", "clpid": "Ghez-A-M" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Gorham", "given_name": "P. W.", "clpid": "Gorham-P-W" }, { "family_name": "Haniff", "given_name": "C. A.", "clpid": "Haniff-C-A" }, { "family_name": "Kulkarni", "given_name": "S. R.", "orcid": "0000-0001-5390-8563", "clpid": "Kulkarni-S-R" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-Keith-Astronomy" }, { "family_name": "Koresko", "given_name": "C.", "clpid": "Koresko-C-D" }, { "family_name": "Beckwith", "given_name": "S.", "clpid": "Beckwith-S-V-W" } ], "abstract": "High-resolution images of T Tau and its infrared companion have been reconstructed from near- and mid-infrared data collected at the Hale 5 m telescope. The near-infrared ( 1-5 \u00b5m) results were obtained by two dimensional speckle imaging and the mid-infrared (10-20 \u00b5m) results were derived from shift and add procedures applied to slit scans. The spectral energy distributions of the separated components were constructed from 1 to 20 \u00b5m data collected in less than half a year (1990 September to 1991 January). The spectral energy distribution of the optical component (T Tau N) is interpreted as containing two distinct constituents, a photosphere and a surrounding disk of circumstellar material. Measurements at a number of infrared wavelengths over the period 1985 December to 1991 January show a 2 mag color-independent change in the brightness of the infrared component (T Tau S). We propose that this may have been caused by an increase in accretion onto T Tau S and model the spectral energy distribution of T Tau S as being dominated by an accretion disk.", "doi": "10.1086/116030", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "1991-12", "series_number": "12", "volume": "102", "issue": "12", "pages": "2066-2072" }, { "id": "authors:th7f6-qmp59", "collection": "authors", "collection_id": "th7f6-qmp59", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181121-090050084", "type": "book_section", "title": "Molecular Disks Around Young Stars", "book_title": "Structure and Dynamics of the Interstellar Medium", "author": [ { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Beckwith", "given_name": "Steven V. W.", "clpid": "Beckwith-S-V-W" } ], "contributor": [ { "family_name": "Moles", "given_name": "Mariano", "clpid": "Moles-M" }, { "family_name": "Tenorio-Tagle", "given_name": "Guillermo", "clpid": "Tenorio-Tagle-G" }, { "family_name": "Melnick", "given_name": "Jorge", "clpid": "Melnick-J" } ], "abstract": "There is now a substantial body of evidence that disk-like structures of gas and dust surround many protostars and young stellar objects (e.g. Rodriguez, these proceedings). We are currently studying a number of these disks to establish whether they have properties compatible with those attributed to the proto-solar nebula, in the early stages of evolution of our solar system. The frequency with which such proto-planetary disks are associated with young stars is also being investigated.", "doi": "10.1017/S0252921100023769", "isbn": "9783540519560", "publisher": "Springer", "place_of_publication": "Berlin", "publication_date": "1989", "pages": "215-220" }, { "id": "authors:p0ppk-x0n26", "collection": "authors", "collection_id": "p0ppk-x0n26", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200318-082248223", "type": "book_section", "title": "Moderate Resolution Spectroscopy For The Space Infrared Telescope Facility (SIRTF)", "book_title": "Cryogenic Optical Systems and Instruments II", "author": [ { "family_name": "Houck", "given_name": "J. R.", "clpid": "Houck-J-R" }, { "family_name": "Beckwith", "given_name": "S. V. W.", "clpid": "Beckwith-S-V-W" }, { "family_name": "Herter", "given_name": "T.", "orcid": "0000-0002-3856-8385", "clpid": "Herter-T-L" }, { "family_name": "Salpeter", "given_name": "E. E.", "clpid": "Salpeter-E-E" }, { "family_name": "Forrest", "given_name": "W. J.", "clpid": "Forrest-W-J" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-Keith-Astronomy" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Watson", "given_name": "D.", "clpid": "Watson-D" }, { "family_name": "Roellig", "given_name": "T.", "clpid": "Roellig-T-L" }, { "family_name": "Weedman", "given_name": "D.", "clpid": "Weedman-D-W" }, { "family_name": "Bauman", "given_name": "L. R.", "clpid": "Bauman-L-R" }, { "family_name": "Downey", "given_name": "C. H.", "clpid": "Downey-C-H" }, { "family_name": "Reitsema", "given_name": "H. J.", "clpid": "Reitsema-H-J" }, { "family_name": "Strecker", "given_name": "D. W.", "clpid": "Strecker-D-W" } ], "contributor": [ { "family_name": "Melugin", "given_name": "Ramsey K.", "clpid": "Melugin-R-K" } ], "abstract": "A conceptual design for an infrared spectrometer capable of both low resolution (\u03bb/\u0394-\u03bb = 50; 2.5-200 microns) and moderate resolution (1000; 4-200 microns) and moderate resolution (1000; 4-200 microns) has been developed. This facility instrument will permit the spectroscopic study in the infrared of objects ranging from within the solar system to distant galaxies. The spectroscopic capability provided by this instrument for SIRTF will give astronomers orders of magnitude greater sensitivity for the study of faint objects than had been previously available. The low resolution mode will enable detailed studies of the continuum radiation. The moderate resolution mode of the instrument will permit studies of a wide range of problems, from the infrared spectral signatures of small outer solar system bodies such as Pluto and the satellites of the giant planets, to investigations of more luminous active galaxies and QS0s at substantially greater distances. A simple design concept has been developed for the spectrometer which supports the science investigation with practical cryogenic engineering. Operational flexibility is preserved with a minimum number of mechanisms. The five modules share a common aperture, and all gratings share a single scan mechanism. High reliability is achieved through use of flight-proven hardware concepts and redundancy. The design controls the heat load into the SIRTF cryogen, with all heat sources other than the detectors operating at 7K and isolated from the 4K cold station. Two-dimensional area detector arrays are used in the 2.5-120\u03bcm bands to simultaneously monitor adjacent regions in extended objects and to measure the background near point sources.", "doi": "10.1117/12.966640", "isbn": "9780892526543", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "1986-07-18", "pages": "69-72" }, { "id": "authors:zzqdd-d7j94", "collection": "authors", "collection_id": "zzqdd-d7j94", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200318-083716382", "type": "book_section", "title": "Moderate Resolution Spectroscopy For The Space Infrared Telescope Facility (SIRTF)", "book_title": "Instrumentation for Optical Remote Sensing from Space", "author": [ { "family_name": "Houck", "given_name": "J. R.", "clpid": "Houck-J-R" }, { "family_name": "Beckwith", "given_name": "S. V. W.", "clpid": "Beckwith-S-V-W" }, { "family_name": "Herter", "given_name": "T.", "orcid": "0000-0002-3856-8385", "clpid": "Herter-T-L" }, { "family_name": "Salpeter", "given_name": "E. E.", "clpid": "Salpeter-E-E" }, { "family_name": "Forrest", "given_name": "W. J.", "clpid": "Forrest-W-J" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-Keith-Astronomy" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Watson", "given_name": "D.", "clpid": "Watson-D" }, { "family_name": "Roellig", "given_name": "T.", "clpid": "Roellig-T-L" }, { "family_name": "Weedman", "given_name": "D.", "clpid": "Weedman-D-W" }, { "family_name": "Bauman", "given_name": "L. R.", "clpid": "Bauman-L-R" }, { "family_name": "Downey", "given_name": "C. H.", "clpid": "Downey-C-H" }, { "family_name": "Reitsema", "given_name": "H. J.", "clpid": "Reitsema-H-J" }, { "family_name": "Strecker", "given_name": "D. W.", "clpid": "Strecker-D-W" } ], "contributor": [ { "family_name": "Lear", "given_name": "John W.", "clpid": "Lear-J-W" }, { "family_name": "Monfils", "given_name": "Andre", "clpid": "Monfils-A" }, { "family_name": "Russak", "given_name": "Sidney L.", "clpid": "Russak-S-L" }, { "family_name": "Seeley", "given_name": "John S.", "clpid": "Seeley-J-S" } ], "abstract": "A conceptual design for an infrared spectrometer capable of both low resolution (\u03bb/\u0394-\u03bb = 50; 2.5-200 microns) and moderate resolution (1000; 4-200 microns) and moderate resolution (1000; 4-200 microns) has been developed. This facility instrument will permit the spectroscopic study in the infrared of objects ranging from within the solar system to distant galaxies. The spectroscopic capability provided by this instrument for SIRTF will give astronomers orders of magnitude greater sensitivity for the study of faint objects than had been previously available. The low resolution mode will enable detailed studies of the continuum radiation. The moderate resolution mode of the instrument will permit studies of a wide range of problems, from the infrared spectral signatures of small outer solar system bodies such as Pluto and the satellites of the giant planets, to investigations of more luminous active galaxies and QS0s at substantially greater distances. A simple design concept has been developed for the spectrometer which supports the science investigation with practical cryogenic engineering. Operational flexibility is preserved with a minimum number of mechanisms. The five modules share a common aperture, and all gratings share a single scan mechanism. High reliability is achieved through use of flight-proven hardware concepts and redundancy. The design controls the heat load into the SIRTF cryogen, with all heat sources other than the detectors operating at 7K and isolated from the 4K cold station. Two-dimensional area detector arrays are used in the 2.5-120\u03bcm bands to simultaneously monitor adjacent regions in extended objects and to measure the background near point sources.", "doi": "10.1117/12.951938", "isbn": "9780892526246", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "1986-05-01", "pages": "238-241" }, { "id": "authors:q021r-jmt46", "collection": "authors", "collection_id": "q021r-jmt46", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170322-162615695", "type": "article", "title": "Molecular hydrogen emission in NGC 7027", "author": [ { "family_name": "Beckwith", "given_name": "S.", "clpid": "Beckwith-S-V-W" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Becklin", "given_name": "E. E.", "clpid": "Becklin-E-E" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Persson", "given_name": "S. E.", "clpid": "Persson-S-E" } ], "abstract": "The spatial distribution of the emission in the v = 1-0 S(1) line of H2 in the planetary nebula NGC 7027 is presented. The excited H2 molecules do not fill the same volume as the ionized gas and most likely reside near the outer edge of the nebula. The spatial resolution of the data, 5 arcsec, is insufficient to define the location of the molecules precisely. An upper limit to the strength of the v = 2-1 S(1) line is given; it is low enough to preclude simple ultraviolet fluorescence as the source of excitation. A simple shock model can fit the line ratio data, however, and there is enough energy in the expanding nebula to sustain such a shock. A rough estimate of 1 M_\u2299 to 4 M_\u2299 for the mass in the molecular cloud surrounding NGC 7027 is derived.", "doi": "10.1086/112753", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "1980-07", "series_number": "7", "volume": "85", "issue": "7", "pages": "886-890" } ]