[ { "id": "authors:qxv7g-1a092", "collection": "authors", "collection_id": "qxv7g-1a092", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190813-092455553", "type": "book_section", "title": "Panchromatic Study of the First Galaxies with Large ALMA Programs", "book_title": "Challenges in Panchromatic Modelling with Next Generation Facilities", "author": [ { "family_name": "Faisst", "given_name": "A.", "orcid": "0000-0002-9382-9832", "clpid": "Faisst-A-L" }, { "family_name": "B\u00e9thermin", "given_name": "M.", "orcid": "0000-0002-3915-2015", "clpid": "B\u00e9thermin-Matthieu" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Cassata", "given_name": "P.", "clpid": "Cassata-P" }, { "family_name": "LeFevre", "given_name": "O.", "orcid": "0000-0001-5891-2596", "clpid": "Le-F\u00e8vre-O" }, { "family_name": "Schaerer", "given_name": "D.", "orcid": "0000-0001-7144-7182", "clpid": "Schaerer-D" }, { "family_name": "Silverman", "given_name": "J.", "orcid": "0000-0002-0000-6977", "clpid": "Silverman-J-D" }, { "family_name": "Yan", "given_name": "L.", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" }, { "literal": "ALPINE Team" } ], "contributor": [ { "family_name": "Boquien", "given_name": "M.", "clpid": "Boquien-M" }, { "family_name": "Lusso", "given_name": "E.", "clpid": "Lusso-E" }, { "family_name": "Gruppioni", "given_name": "C.", "clpid": "Gruppioni-C" }, { "family_name": "Tisserand", "given_name": "P.", "clpid": "Tisserand-P" } ], "abstract": "Thanks to deep optical to near-IR imaging and spectroscopy, significant progress is made in characterizing the rest-frame UV to optical properties of galaxies in the early universe (z > 4. Surveys with Hubble, Spitzer, and ground-based facilities (Keck, Subaru, and VLT) provide spectroscopic and photometric redshifts, measurements of the spatial structure, stellar masses, and optical emission lines for large samples of galaxies. Recently, the Atacama Large (Sub) Millimeter Array (ALMA) has become a major player in pushing studies of high redshift galaxies to far-infrared wavelengths, hence making panchromatic surveys over many orders of frequencies possible. While past studies focused mostly on bright sub-millimeter galaxies, the sensitivity of ALMA now enables surveys like ALPINE, which focuses on measuring the gas and dust properties of a large sample of normal main-sequence galaxies at z > 4. Combining observations across different wavelengths into a single, panchromatic picture of galaxy formation and evolution is currently and in the future an important focus of the astronomical community.", "doi": "10.1017/S1743921319001881", "isbn": "9781108471473", "publisher": "Cambridge University Press", "place_of_publication": "Cambridge", "publication_date": "2019-11", "pages": "12-16" }, { "id": "authors:nkbed-qbs98", "collection": "authors", "collection_id": "nkbed-qbs98", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191202-081233387", "type": "book_section", "title": "Euclid Near-infrared Imaging Reduction Pipeline: Astrometric Calibration, Resampling and Stacking", "book_title": "Astronomical Data Analysis Software and Systems XXVI", "author": [ { "family_name": "Da Silva", "given_name": "R.", "clpid": "Da-Silva-R" }, { "family_name": "Radovich", "given_name": "M.", "clpid": "Radovich-M" }, { "family_name": "Bonchi", "given_name": "A.", "clpid": "Bonchi-A" }, { "family_name": "Faustini", "given_name": "F.", "clpid": "Faustini-F" }, { "family_name": "Frailis", "given_name": "M.", "clpid": "Frailis-M" }, { "family_name": "Polenta", "given_name": "G.", "clpid": "Polenta-G" }, { "family_name": "Bouwens", "given_name": "R.", "orcid": "0000-0002-4989-2471", "clpid": "Bouwens-R-J" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Jahnke", "given_name": "K.", "orcid": "0000-0003-3804-2137", "clpid": "Jahnke-K" }, { "family_name": "Kazandjian", "given_name": "M.", "clpid": "Kazandjian-M" }, { "family_name": "Liu", "given_name": "X. C.", "clpid": "Liu-X-C" }, { "family_name": "Maino", "given_name": "D.", "clpid": "Maino-D" }, { "family_name": "Teplitz", "given_name": "H.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Wachter", "given_name": "S.", "clpid": "Wachter-Stefanie" }, { "family_name": "Barbier", "given_name": "R.", "clpid": "Barbier-R" }, { "family_name": "Ealet", "given_name": "A.", "clpid": "Ealet-A" }, { "family_name": "Kubik", "given_name": "B.", "clpid": "Kubik-B" }, { "family_name": "Carretero", "given_name": "J.", "clpid": "Carretero-J" }, { "family_name": "Jullo", "given_name": "E.", "orcid": "0000-0002-9253-053X", "clpid": "Jullo-E" }, { "family_name": "Schultheis", "given_name": "M.", "clpid": "Schultheis-M" }, { "family_name": "Seidel", "given_name": "G.", "clpid": "Seidel-G-M" }, { "family_name": "Serrano", "given_name": "S.", "clpid": "Serrano-S" }, { "family_name": "Tallada", "given_name": "P.", "clpid": "Tallada-P" }, { "family_name": "Tonello", "given_name": "N.", "clpid": "Tonello-N" } ], "contributor": [ { "family_name": "Molinaro", "given_name": "Marco", "clpid": "Molinaro-M" }, { "family_name": "Shortridge", "given_name": "Keith", "clpid": "Shortridge-K" }, { "family_name": "Pasian", "given_name": "Fabio", "clpid": "Pasian-F" } ], "abstract": "Euclid is an ESA survey mission designed to understand the origin of the Universe's accelerating expansion using weak gravitational lensing and redshift clustering as main probes. Very high image quality is required for galaxy shape measurements, while accurate photometry at visible and near-infrared wavelengths and near-infrared spectroscopy are needed to measure photometric and spectroscopic galaxy redshifts. Within the Euclid Science Ground Segment, the near-infrared imaging (NIR) processing function has the task to reduce all the images produced by the near-infrared instrument (NISP) in photometric mode. Starting from Level 1 raw frames, the NIR pipeline shall produce individual images and stacked mosaics in Y, J, and H bands accounting for instrumental effects, subtracting the sky background, performing both astrometric and photometric calibrations, and providing all the information needed for catalogue production such as PSF, variance, weights, and quality flags. After an overview of the pipeline design, we present the current status of the NIR processing function development. We focus on preliminary results from the application of astrometric calibration, resampling, and stacking procedures to simulated images, and we discuss the different approaches that we tested in order to fulfill specific requirements.", "isbn": "978-1-58381-929-6", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "2019", "pages": "311-314" }, { "id": "authors:a7ndc-gmg80", "collection": "authors", "collection_id": "a7ndc-gmg80", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180814-144152671", "type": "book_section", "title": "SPHEREx: an all-sky NIR spectral survey", "book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave", "author": [ { "family_name": "Korngut", "given_name": "Phillip M.", "clpid": "Korngut-P-M" }, { "family_name": "Bock", "given_name": "James J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Akeson", "given_name": "Rachel", "orcid": "0000-0001-9674-1564", "clpid": "Akeson-R-L" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Hemmati", "given_name": "Shoubaneh", "orcid": "0000-0003-2226-5395", "clpid": "Hemmati-S" }, { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" }, { "family_name": "dePutter", "given_name": "Roland", "clpid": "de-Putter-R" }, { "family_name": "Smith", "given_name": "Roger", "clpid": "Smith-R-M" }, { "family_name": "Stickley", "given_name": "Nathaniel", "clpid": "Stickley-N" }, { "family_name": "Teplitz", "given_name": "Harry", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" } ], "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-E-C" } ], "abstract": "SPHEREx, a mission in NASA's Medium Explorer (MIDEX) program recently selected for Phase-A implementation, is an all-sky survey satellite that will produce a near-infrared spectrum for every 6 arcsecond pixel on the sky. SPHEREx has a simple, high-heritage design with large optical throughput to maximize spectral mapping speed. While the legacy data products will provide a rich archive of spectra for the entire astronomical community to mine, the instrument is optimized for three specific scientific goals: to probe inflation through the imprint primordial non-Gaussianity left on today's large-scale cosmological structure; to survey the Galactic plane for water and other biogenic ices through absorption line studies; and to constrain the history of galaxy formation through power spectra of background fluctuations as measured in deep regions near the ecliptic poles. The aluminum telescope consists of a heavily baffled, wide-field off-axis reflective triplet design. The focal plane is imaged simultaneously by two mosaics of H2RG detector arrays separated by a dichroic beamsplitter. SPHEREx assembles spectra through the use of mass and volume efficient linear variable filters (LVFs) included in the focal plane assemblies, eliminating the need for any dispersive or moving elements. Instead, spectra are constructed through a series of small steps in the spacecraft attitude across the sky, modulating the location of an object within the FOV and varying the observation wavelength in each exposure. The spectra will cover the wavelength range between 0.75 and 5.0 \u00b5m at spectral resolutions ranging between R=35 and R=130. The entire telescope is cooled passively by a series of three V-groove radiators below 80K. An additional stage of radiative cooling is included to reduce the long wavelength focal plane temperature below 60K, controlling the dark current. As a whole, SPHEREx requires no new technologies and carries large technical and resource margins on every aspect of the design.", "doi": "10.1117/12.2312860", "isbn": "9781510619494", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_publication": "Bellingham, WA", "publication_date": "2018-07-06", "pages": "Art. No. 106981U" }, { "id": "authors:r6j1t-g6d38", "collection": "authors", "collection_id": "r6j1t-g6d38", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170109-144441145", "type": "book_section", "title": "High-Redshift Protoclusters Traced by Submillimeter Galaxies: Tracing Star Formation Activity out to z > 4", "book_title": "From Interstellar Clouds to Star-Forming Galaxies: Universal Processes?", "author": [ { "family_name": "Men\u00e9ndez-Delmestre", "given_name": "Kar\u00edn", "orcid": "0000-0003-3153-5123", "clpid": "Men\u00e9ndez-Delmestre-K" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Sheth", "given_name": "Kartik", "orcid": "0000-0002-5496-4118", "clpid": "Sheth-K" } ], "contributor": [ { "family_name": "Jablonka", "given_name": "Pascale", "clpid": "Jablonka-P" }, { "family_name": "Andr\u00e9", "given_name": "Philippe", "clpid": "Andr\u00e9-P" }, { "family_name": "van der Tak", "given_name": "Floris", "clpid": "van-der-Tak-F-F-S" } ], "abstract": "Clustering analysis indicate that at z ~ 2 submm-selected galaxies (SMGs) reside in very massive halos (M_(DM) > 5 \u00d7 10^(13)), suggesting that SMGs trace high-density environments that evolve into rich galaxy clusters. Conversely, recent work suggests that SMGs are tracers of a broader range of environments, including structures with more modest masses caught in highly active periods; since galaxies in these structures are likely caught during episodes of peak starbursts, SMGs may be tracers of a wider range of environments beyond the progenitors of todays very rich clusters, opening a window for a more complete exploration of the details underpinning the process of galaxy evolution in concert with the assembly of the large scale structure (LSS). We have undertaken a large observing program comprising deep narrow-band Ly-alpha imaging and multi-object spectroscopy using Palomar/Keck/Magellan/Gemini telescopes to probe for galaxy overdensities in SMG environments at z ~ 1 \u2212 5. With ~200 spectroscopically-confirmed Ly-alpha emitters, we are in a position to gauge the level of galaxy overdensity in these regions.", "doi": "10.1017/S1743921316008164", "isbn": "978-1-107-13520-8", "publisher": "Cambridge University Press", "place_of_publication": "Cambridge", "publication_date": "2016-09-12", "pages": "1-2" }, { "id": "authors:yt2nr-1yq19", "collection": "authors", "collection_id": "yt2nr-1yq19", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170227-100310208", "type": "book_section", "title": "Imaging of NGC 5907's stellar stream", "book_title": "The General Assembly of Galaxy Halos: Structure, Origin and Evolution", "author": [ { "family_name": "Laine", "given_name": "Seppo", "orcid": "0000-0003-1250-8314", "clpid": "Laine-S-J" }, { "family_name": "Grillmair", "given_name": "Carl J.", "orcid": "0000-0003-4072-169X", "clpid": "Grillmair-C-J" }, { "family_name": "Mart\u00ednez-Delgado", "given_name": "David", "orcid": "0000-0003-3835-2231", "clpid": "Mart\u00ednez-Delgado-D" }, { "family_name": "Romanowsky", "given_name": "Aaron J.", "orcid": "0000-0003-2473-0369", "clpid": "Romanowsky-A-J" }, { "family_name": "Capak", "given_name": "Peter L.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Arendt", "given_name": "Richard G.", "orcid": "0000-0001-8403-8548", "clpid": "Arendt-R-G" }, { "family_name": "Ashby", "given_name": "Matthew L. N.", "orcid": "0000-0002-3993-0745", "clpid": "Ashby-M-L-N" }, { "family_name": "Davies", "given_name": "James E.", "clpid": "Davies-J-E" }, { "family_name": "Majewski", "given_name": "Steven R.", "orcid": "0000-0003-2025-3147", "clpid": "Majewski-Steven-R" }, { "family_name": "GaBany", "given_name": "R. Jay", "clpid": "GaBany-R-J" } ], "contributor": [ { "family_name": "Bragaglia", "given_name": "Angela", "clpid": "Bragaglia-A" }, { "family_name": "Arnaboldi", "given_name": "Magda", "clpid": "Arnaboldi-M" }, { "family_name": "Rejkuba", "given_name": "Marina", "clpid": "Rejkuba-M" }, { "family_name": "Romano", "given_name": "Donatella", "clpid": "Romano-D" } ], "abstract": "We have obtained deep g, r, and i-band Subaru and ultra-deep 3.6 \u03bcm IRAC images of parts of the multiply-wrapped stellar stream around the nearby edge-on galaxy NGC 5907. We have fitted the surface brightness measurements of the stream with FSPS stellar population synthesis models to derive the metallicity and age of the brightest parts of the stream. The resulting relatively high metallicity ([Fe/H] = \u22120.3) is consistent with a major merger scenario but a satellite accretion event cannot be ruled out.", "doi": "10.1017/S1743921315006663", "isbn": "9781107138193", "publisher": "Cambridge University Press", "place_of_publication": "Cambridge", "publication_date": "2016-05-09", "pages": "324-325" }, { "id": "authors:ye26d-r1w23", "collection": "authors", "collection_id": "ye26d-r1w23", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180824-100034119", "type": "book_section", "title": "Star-forming galaxies versus low- and high-excitation radio AGN in the VLA-COSMOS 3GHz Large Project", "author": [ { "family_name": "Baran", "given_name": "N.", "clpid": "Baran-Nikola" }, { "family_name": "Smol\u010di\u0107", "given_name": "V.", "orcid": "0000-0002-3893-8614", "clpid": "Smol\u010di\u0107-V" }, { "family_name": "Novak", "given_name": "M.", "orcid": "0000-0001-8695-825X", "clpid": "Novak-Mladen" }, { "family_name": "Delhaize", "given_name": "J.", "orcid": "0000-0002-6149-0846", "clpid": "Delhaize-J" }, { "family_name": "Delvecchio", "given_name": "I.", "orcid": "0000-0001-8706-2252", "clpid": "Delvecchio-I" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Civano", "given_name": "F.", "orcid": "0000-0002-2115-1137", "clpid": "Civano-Francesca" }, { "family_name": "Herrera Ruiz", "given_name": "N.", "clpid": "Herrera-Ruiz-N" }, { "family_name": "Ilbert", "given_name": "O.", "orcid": "0000-0002-7303-4397", "clpid": "Ilbert-Olivier" }, { "family_name": "Laigle", "given_name": "C.", "clpid": "Laigle-C" }, { "family_name": "Marchesi", "given_name": "S.", "orcid": "0000-0001-5544-0749", "clpid": "Marchesi-S" }, { "family_name": "McCracken", "given_name": "H. J.", "orcid": "0000-0002-9489-7765", "clpid": "McCracken-H-J" }, { "family_name": "Middelberg", "given_name": "E.", "clpid": "Middelberg-E" }, { "family_name": "Salvato", "given_name": "M.", "orcid": "0000-0001-7116-9303", "clpid": "Salvato-Mara" }, { "family_name": "Schinnerer", "given_name": "E.", "orcid": "0000-0002-3933-7677", "clpid": "Schinnerer-E" } ], "abstract": "We study the composition of the faint radio population selected from the VLA-COSMOS 3GHz Large Project, a radio continuum survey performed at 10 cm wavelength. The survey covers the\nfull 2 square degree COSMOS field with mean rms \u223c 2.3 \u00b5Jy/beam, cataloging 10,899 source components above 5 \u00d7 rms. By combining these radio data with UltraVISTA, optical, near-infrared,\nand Spitzer/IRAC mid-infrared data, as well as X-ray data from the Chandra Legacy, Chandra COSMOS surveys, we gain insight into the emission mechanisms within our radio sources out to redshifts of z \u223c 5. From these emission characteristics we classify our souces\nas star forming galaxies or AGN. Using their multi-wavelength properties we further separate the AGN into sub-samples dominated by radiatively efficient and inefficient AGN, often referred to as high- and low-excitation emission line AGN. We compare our method with other results based on fitting of the sources' spectral energy distributions using both galaxy and AGN spectral models, and those based on the infrared-radio correlation. We study the fractional contributions of these sub-populations down to radio flux levels of \u223c10 \u00b5Jy. We find that at 3 GHz flux densities above \u223c400 \u00b5Jy quiescent, red galaxies, consistent with the low-excitation radio AGN class constitute the dominant fraction. Below densities of \u223c200 \u00b5Jy star-forming galaxies begin to constitute the largest fraction, followed by the low-excitation, and X-ray- and IR-identified high-excitation radio AGN.", "doi": "10.22323/1.267.0055", "publisher": "SISSA", "publication_date": "2015-10" }, { "id": "authors:4eb2a-e7q91", "collection": "authors", "collection_id": "4eb2a-e7q91", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180713-114823898", "type": "book_section", "title": "Enhancement of the Spitzer Infrared Array Camera (IRAC) distortion correction for parallax measurements", "book_title": "Space Telescopes and Instrumentation 2014: Optical, Infrared, and Millimeter Wave", "author": [ { "family_name": "Lowrance", "given_name": "Patrick J.", "orcid": "0000-0001-8014-0270", "clpid": "Lowrance-P-J" }, { "family_name": "Carey", "given_name": "Sean J.", "orcid": "0000-0002-0221-6871", "clpid": "Carey-S-J" }, { "family_name": "Ingalls", "given_name": "James G.", "orcid": "0000-0003-4714-1364", "clpid": "Ingalls-J-G" }, { "family_name": "Surace", "given_name": "Jason A.", "orcid": "0000-0001-7291-0087", "clpid": "Surace-J-A" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Stauffer", "given_name": "John", "orcid": "0000-0003-3595-7382", "clpid": "Stauffer-J-R" }, { "family_name": "Beichman", "given_name": "Chas", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Shupe", "given_name": "David", "orcid": "0000-0003-4401-0430", "clpid": "Shupe-David-L" }, { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" } ], "contributor": [ { "family_name": "Oschmann", "given_name": "Jacobus M.", "clpid": "Oschmann-J-M" }, { "family_name": "Clampin", "given_name": "Mark", "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" } ], "abstract": "The Spitzer Space Telescope Infrared Array (IRAC) offers a rare opportunity to measure distances and determine physical properties of the faintest and coldest brown dwarfs. The current distortion correction is a 3rd order polynomial represented by TAN-SIP parameters within the headers. The current correction, good to 100 mas, was derived from deep imaging, using marginally resolved galaxies in some cases, and has remained stable throughout both the cryogenic and warm mission. Using recent Spitzer calibration observations mapped to HST/ACS calibration observations of 47 Tuc with an absolute accuracy good to 1 mas, we are working towards a possible 5th order polynomial correction that theoretically could allow measurements to within 20 mas. Extensive testing, using observations of 47 Tuc, NGC 6791 and NGC 2264, are underway, after which the new parameters will be used to update all the 3.6 and 4.5um data taken within warm and cryogenic missions. We anticipate if achievable, this new accuracy could be combined with other ongoing enhancements (Ingalls et al, 9143-52) that will permit measurements of parallaxes out to about 50 pc, increasing the volume surveyed by a factor of 100, and enabling new capabilities such as luminosity measurements of the population of young brown dwarfs in the beta Pictoris moving group.", "doi": "10.1117/12.2057195", "isbn": "9780819496119", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2014-08-28", "pages": "Art. No. 914358" }, { "id": "authors:wcmyx-1st86", "collection": "authors", "collection_id": "wcmyx-1st86", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110713-095334730", "type": "book_section", "title": "Science Validation of the Spitzer Source List", "book_title": "Astronomical Data Analysis Software and Systems XX", "author": [ { "family_name": "Teplitz", "given_name": "H. I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Brooke", "given_name": "T.", "clpid": "Brooke-T-Y" }, { "family_name": "Hoard", "given_name": "D. W.", "orcid": "0000-0002-6800-6519", "clpid": "Hoard-D-W" }, { "family_name": "Hanish", "given_name": "D.", "clpid": "Hanish-D-J" }, { "family_name": "Desai", "given_name": "V.", "orcid": "0000-0002-1340-0543", "clpid": "Desai-V" }, { "family_name": "Khan", "given_name": "I.", "clpid": "Khan-I-R" }, { "family_name": "Laher", "given_name": "R.", "orcid": "0000-0003-2451-5482", "clpid": "Laher-R-R" } ], "contributor": [ { "family_name": "Evans", "given_name": "Ian N.", "clpid": "Evans-I-N" }, { "family_name": "Accomazzi", "given_name": "Alberto", "clpid": "Accomazzi-A" }, { "family_name": "Mink", "given_name": "Douglas J.", "clpid": "Mink-D-J" }, { "family_name": "Rots", "given_name": "Arnold H.", "clpid": "Rots-A-H" } ], "abstract": "The Spitzer Science Center will produce a source list (SL) of photometry for a large subset of imaging data in the Spitzer Heritage Archive (SHA). The list will enable a large range of science projects. The primary requirement on the SL is very high reliability \u2014 with areal coverage, completeness and limiting depth being secondary considerations. The SHA at the NASA Infrared Science Archive (IRSA) will serve the SL as an enhanced data product. The SL will include data from the four channels of\nIRAC (3\u20138 microns) and the 24 micron channel of MIPS. The Source List will include image products (mosaics) and photometric data for Spitzer observations of about 1500\nsquare degrees and include around 30 million sources. We describe ongoing science validation of the Spitzer Source List, and discuss the range of use cases which will be\nsupported.", "isbn": "978-1-58381-764-3", "publisher": "Astronomical Society of the Pacific", "publication_date": "2011", "pages": "363-366" }, { "id": "authors:8prpx-ksj77", "collection": "authors", "collection_id": "8prpx-ksj77", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110520-135007765", "type": "book_section", "title": "The Spitzer Source List", "book_title": "Astronomical data analysis software and systems XIX", "author": [ { "family_name": "Teplitz", "given_name": "Harry I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Brooke", "given_name": "Timothy", "clpid": "Brooke-T-Y" }, { "family_name": "Shenoy", "given_name": "Sachin", "clpid": "Shenoy-S-S" }, { "family_name": "Brinkworth", "given_name": "Carolyn", "clpid": "Brinkworth-C-S" }, { "family_name": "Desai", "given_name": "Vandana", "orcid": "0000-0002-1340-0543", "clpid": "Desai-V" }, { "family_name": "Khan", "given_name": "Iffat", "clpid": "Khan-I-R" }, { "family_name": "Laher", "given_name": "Russ", "orcid": "0000-0003-2451-5482", "clpid": "Laher-R-R" } ], "contributor": [ { "family_name": "Mizumoto", "given_name": "Yoshihiko", "clpid": "Mizumoto-Yoshihiko" }, { "family_name": "Morita", "given_name": "Koh-Ichiro", "clpid": "Morita-Koh-Ichiro" }, { "family_name": "Ohishi", "given_name": "Masatoshi", "clpid": "Ohishi-Masatoshi" } ], "abstract": "The Spitzer Science Center will produce a source list (SL) of photometry for a large subset of imaging data in the Spitzer Heritage Archive (SHA). The list will enable a large range of science projects. The primary requirement on the SL is very high reliability, with areal coverage, completeness and limiting depth being secondary considerations. The SHA at the NASA Infrared Science Archive (IRSA) will serve the SL as an enhanced data product. The SL will include data from the four channels of IRAC (3\u20138 microns) and the 24 micron channel of MIPS. The Source List will include image products (mosaics) and photometric data for Spitzer observations of about 1500 square degrees and include around 30 million sources. We describe the plans and timeline for development of the Spitzer Source List. We demonstrate the verification of the Source List pipeline using Spitzer Legacy catalogs at \"truth tables\". Finally, we discuss the range of use cases which will be supported.", "isbn": "978-1-58381-748-3", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "2010", "pages": "437-440" }, { "id": "authors:qw28a-kcf38", "collection": "authors", "collection_id": "qw28a-kcf38", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100913-150853446", "type": "book_section", "title": "Design of the Spitzer Space Telescope Heritage Archive", "book_title": "Astronomical Data Analysis Software and Systems XVIII", "author": [ { "family_name": "Levine", "given_name": "Deborah", "clpid": "Levine-D-A" }, { "family_name": "Wu", "given_name": "X.", "clpid": "Wu-X" }, { "family_name": "Good", "given_name": "J.", "clpid": "Good-J-C" }, { "family_name": "Alexov", "given_name": "A.", "clpid": "Alexov-A" }, { "family_name": "Berriman", "given_name": "G. B.", "orcid": "0000-0001-8388-534X", "clpid": "Berriman-G-B" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Groom", "given_name": "S.", "orcid": "0000-0001-5668-3507", "clpid": "Groom-S-L" }, { "family_name": "Handley", "given_name": "T.", "clpid": "Handley-T" }, { "family_name": "Kirkpatrick", "given_name": "J. D.", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" }, { "family_name": "Lacy", "given_name": "M.", "orcid": "0000-0002-3032-1783", "clpid": "Lacy-M" }, { "family_name": "Legassie", "given_name": "M.", "clpid": "Legassie-M" }, { "family_name": "Laine", "given_name": "S.", "orcid": "0000-0003-1250-8314", "clpid": "Laine-S-J" }, { "family_name": "Ly", "given_name": "L.", "clpid": "Ly-Loi" }, { "family_name": "Roby", "given_name": "T.", "clpid": "Roby-T" }, { "family_name": "Laher", "given_name": "Russ R.", "orcid": "0000-0003-2451-5482", "clpid": "Laher-R-R" } ], "contributor": [ { "family_name": "Bohlender", "given_name": "David A.", "clpid": "Bohlender-D-A" }, { "family_name": "Durand", "given_name": "Daniel", "clpid": "Durand-D" }, { "family_name": "Dowler", "given_name": "Patrick", "clpid": "Dowler-P" } ], "abstract": "It is predicted that Spitzer Space Telescope's cryogen will run out in April 2009, and the final reprocessing for the cryogenic mission is scheduled to end in April 2011, at which time the Spitzer archive will be transferred to the NASA/IPAC Infrared Science Archive (IRSA) for long-term curation. The Spitzer Science Center (SSC) and IRSA are collaborating to design and deploy the Spitzer Heritage Archive (SHA), which will supersede the current Spitzer archive. It will initially contain the raw and final reprocessed cryogenic science products, and will eventually incorporate the final products from the Warm mission. The SHA will be accompanied by tools deemed necessary to extract the full science content of the archive and by comprehensive documentation.", "isbn": "978-1-58381-702-5", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "2009", "pages": "29-32" }, { "id": "authors:yh41e-p9k47", "collection": "authors", "collection_id": "yh41e-p9k47", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100222-095358778", "type": "book_section", "title": "IRAC Deep Survey of COSMOS", "book_title": "The Science Opportunities of the Warm Spitzer Mission Workshop", "author": [ { "family_name": "Scoville", "given_name": "Nick", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Giavalisco", "given_name": "Mauro", "orcid": "0000-0002-7831-8751", "clpid": "Giavalisco-M" }, { "family_name": "Sanders", "given_name": "Dave", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" } ], "abstract": "Over the last four years, we have developed the COSMOS survey field with complete multi-wavelength coverage from radio to X-ray, including a total of 600 hours of Spitzer Legacy time (166 hours IRAC, 460 hours MIPS). Here we propose to deepen the IRAC 3.6 \u00b5m and 4.5 \u00b5m coverage with 3000 hours over 2.3 deg^2 area included in deep Subaru imaging. This extended mission deep survey will increase the sensitivity by a factor of 3\u20135. The most important impact will be that the COSMOS survey will then provide extremely sensitive photometric redshifts and stellar mass estimates for approximately a million galaxies out to z~6. We expect these data to detect approximately 1000 objects at z = 6 to 10. The data will also provide excellent temporal coverage for variability studies on timescales from days to the length of the extended mission.", "doi": "10.1063/1.2806781", "isbn": "978-0-7354-0457-1", "publisher": "American Institute of Physics", "place_of_publication": "Melville, NY", "publication_date": "2007-10-18", "pages": "221-228" } ]