[ { "id": "authors:xqcv3-79f72", "collection": "authors", "collection_id": "xqcv3-79f72", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200908-091428952", "type": "monograph", "title": "Joint Survey Processing of Euclid, Rubin and Roman: Final Report", "author": [ { "family_name": "Chary", "given_name": "Ranga Ram", "orcid": "0000-0001-7583-0621", "clpid": "Chary-R-R" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Brammer", "given_name": "Gabriel", "orcid": "0000-0003-2680-005X", "clpid": "Brammer-G" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Faisst", "given_name": "Andreas", "orcid": "0000-0002-9382-9832", "clpid": "Faisst-A-L" }, { "family_name": "Flynn", "given_name": "Dave", "clpid": "Flynn-D" }, { "family_name": "Groom", "given_name": "Steven", "orcid": "0000-0001-5668-3507", "clpid": "Groom-S-L" }, { "family_name": "Ferguson", "given_name": "Henry C.", "orcid": "0000-0001-7113-2738", "clpid": "Ferguson-H-C" }, { "family_name": "Grillmair", "given_name": "Carl", "orcid": "0000-0003-4072-169X", "clpid": "Grillmair-C-J" }, { "family_name": "Hemmati", "given_name": "Shoubaneh", "orcid": "0000-0003-2226-5395", "clpid": "Hemmati-S" }, { "family_name": "Koekemoer", "given_name": "Anton", "orcid": "0000-0002-6610-2048", "clpid": "Koekemoer-A-M" }, { "family_name": "Lee", "given_name": "BoMee", "clpid": "Lee-BoMee" }, { "family_name": "Malhotra", "given_name": "Sangeeta", "orcid": "0000-0002-9226-5350", "clpid": "Malhotra-Sangeeta" }, { "family_name": "Miyatake", "given_name": "Hironao", "clpid": "Miyatake-H" }, { "family_name": "Melchior", "given_name": "Peter", "orcid": "0000-0002-8873-5065", "clpid": "Melchior-P" }, { "family_name": "Momcheva", "given_name": "Ivelina", "clpid": "Momcheva-I-G" }, { "family_name": "Newman", "given_name": "Jeffrey", "orcid": "0000-0001-8684-2222", "clpid": "Newman-J-A" }, { "family_name": "Masiero", "given_name": "Joseph", "orcid": "0000-0003-2638-720X", "clpid": "Masiero-J-R" }, { "family_name": "Paladini", "given_name": "Roberta", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Prakash", "given_name": "Abhishek", "orcid": "0000-0003-4451-4444", "clpid": "Prakash-Abhishek" }, { "family_name": "Rusholme", "given_name": "Benjamin", "orcid": "0000-0001-7648-4142", "clpid": "Rusholme-B" }, { "family_name": "Stickley", "given_name": "Nathaniel", "clpid": "Stickley-N-R" }, { "family_name": "Smith", "given_name": "Arfon", "clpid": "Smith-A-M" }, { "family_name": "Wood-Vasey", "given_name": "Michael", "clpid": "Wood-Vasey-W-M" }, { "family_name": "Teplitz", "given_name": "Harry I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" } ], "abstract": "The Euclid, Rubin/LSST and Roman (WFIRST) projects will undertake flagship optical/near-infrared surveys in the next decade. By mapping thousands of square degrees of sky and covering the electromagnetic spectrum between 0.3 and\n2 microns with sub-arcsec resolution, these projects will detect several tens\nof billions of sources, enable a wide range of astrophysical investigations by\nthe astronomical community and provide unprecedented constraints on the nature\nof dark energy and dark matter. The ultimate cosmological, astrophysical and\ntime-domain science yield from these missions will require joint survey\nprocessing (JSP) functionality at the pixel level that is outside the scope of\nthe individual survey projects. The JSP effort scoped here serves two\nhigh-level objectives: 1) provide precise concordance multi-wavelength images\nand catalogs over the entire sky area where these surveys overlap, which\naccounts for source confusion and mismatched isophotes, and 2) provide a\nscience platform to analyze concordance images and catalogs to enable a wide\nrange of astrophysical science goals to be formulated and addressed by the\nresearch community. For the cost of about 200WY, JSP will allow the U.S. (and\ninternational) astronomical community to manipulate the flagship data sets and\nundertake innovative science investigations ranging from solar system object\ncharacterization, exoplanet detections, nearby galaxy rotation rates and dark\nmatter properties, to epoch of reionization studies. It will also allow for the\nultimate constraints on cosmological parameters and the nature of dark energy,\nwith far smaller uncertainties and a better handle on systematics than by any one survey alone.", "doi": "10.48550/arXiv.2008.10663", "publisher": "arXiv", "publication_date": "2020-08-24" }, { "id": "authors:r383c-jrv08", "collection": "authors", "collection_id": "r383c-jrv08", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190812-161714076", "type": "monograph", "title": "Deep+Wide Lensing Surveys will Provide Exquisite Measurements of the Dark Matter Halos of Dwarf Galaxies", "author": [ { "family_name": "Leauthaud", "given_name": "Alexie", "orcid": "0000-0002-3677-3617", "clpid": "Leauthaud-A" }, { "family_name": "Singh", "given_name": "Sukhdeep", "clpid": "Singh-Sukhdeep" }, { "family_name": "Luo", "given_name": "Yifei", "clpid": "Luo-Yifei" }, { "family_name": "Ardila", "given_name": "Felipe", "orcid": "0000-0002-6100-4852", "clpid": "Ardila-F" }, { "family_name": "Greco", "given_name": "Johnny P.", "clpid": "Greco-J-P" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Greene", "given_name": "Jenny E.", "clpid": "Greene-J-E" }, { "family_name": "Mayer", "given_name": "Lucio", "clpid": "Mayer-Lucio" } ], "abstract": "The advent of new deep+wide photometric lensing surveys will open up the possibility of direct measurements of the dark matter halos of dwarf galaxies. The HSC wide survey will be the first with the statistical capability of measuring the lensing signal with high signal-to-noise at log(M*)=8. At this same mass scale, LSST will have the most overall constraining power with a predicted signal-to-noise for the galaxy-galaxy lensing signal around dwarfs of SN=200. WFIRST and LSST will have the greatest potential to push below the log(M*) = 7 mass scale thanks to the depth of their imaging data. Studies of the dark matter halos of dwarf galaxies at z=0.1 with gravitational lensing are soon within reach. However, further work will be required to develop optimized strategies for extracting dwarfs samples from these surveys, determining redshifts, and accurately measuring lensing on small radial scales. Dwarf lensing will be a new and powerful tool to constrain the halo masses and inner density slopes of dwarf galaxies and to distinguish between baryonic feedback and modified dark matter scenarios.", "doi": "10.48550/arXiv.1905.01433", "publisher": "arXiv", "publication_date": "2019-05-04" }, { "id": "authors:72kc4-p3855", "collection": "authors", "collection_id": "72kc4-p3855", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190813-091659412", "type": "monograph", "title": "Mini-survey of the northern sky to Dec < +30", "author": [ { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Sconlic", "given_name": "D.", "clpid": "Sconlic-D" }, { "family_name": "Cuillandre", "given_name": "J-C.", "clpid": "Cuillandre-J-C" }, { "family_name": "Castander", "given_name": "F.", "orcid": "0000-0001-7316-4573", "clpid": "Castander-F-J" }, { "family_name": "Bolton", "given_name": "A.", "clpid": "Bolton-A-S" }, { "family_name": "Bowler", "given_name": "R.", "clpid": "Bowler-R-A-A" }, { "family_name": "Chang", "given_name": "C.", "clpid": "Chang-C" }, { "family_name": "Dey", "given_name": "A.", "orcid": "0000-0002-4928-4003", "clpid": "Dey-A" }, { "family_name": "Eifler", "given_name": "T.", "orcid": "0000-0002-1894-3301", "clpid": "Eifler-T-F" }, { "family_name": "Eisenstein", "given_name": "D.", "clpid": "Eisenstein-D-J" }, { "family_name": "Grillmair", "given_name": "C.", "orcid": "0000-0003-4072-169X", "clpid": "Grillmair-C-J" }, { "family_name": "Gris", "given_name": "P.", "clpid": "Gris-P" }, { "family_name": "Hernitschek", "given_name": "N.", "orcid": "0000-0003-1681-0430", "clpid": "Hernitschek-N" }, { "family_name": "Hook", "given_name": "I.", "orcid": "0000-0002-2960-978X", "clpid": "Hook-I-M" }, { "family_name": "Hirata", "given_name": "C.", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Kuijken", "given_name": "B. Jain K.", "clpid": "Kuijken-B-J-K" }, { "family_name": "Lochner", "given_name": "M.", "orcid": "0000-0003-2221-8281", "clpid": "Lochner-M" }, { "family_name": "Newman", "given_name": "J.", "clpid": "Newman-J" }, { "family_name": "Oesch", "given_name": "P.", "orcid": "0000-0001-5851-6649", "clpid": "Oesch-P-A" }, { "family_name": "Olsen", "given_name": "K.", "orcid": "0000-0002-7134-8296", "clpid": "Olsen-Knut-A-G" }, { "family_name": "Rhodes", "given_name": "J.", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" }, { "family_name": "Robertson", "given_name": "B.", "orcid": "0000-0002-4271-0364", "clpid": "Robertson-B-E" }, { "family_name": "Rubin", "given_name": "D.", "clpid": "Rubin-D-M" }, { "family_name": "Scarlata", "given_name": "C.", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-C-M" }, { "family_name": "Silverman", "given_name": "J.", "orcid": "0000-0002-0000-6977", "clpid": "Silverman-J-D" }, { "family_name": "Wachter", "given_name": "S.", "clpid": "Wachter-S" }, { "family_name": "Wang", "given_name": "Y.", "clpid": "Wang-Yun" }, { "literal": "Tri-Agency Working Group" } ], "abstract": "We propose an extension of the LSST survey to cover the northern sky to DEC < +30 (accessible at airmass <1.8). This survey will increase the LSST sky coverage by ~9,600 square degrees from 18,900 to 28,500 square degrees (a 50% increase) but use only 0.6-2.5% of the time depending on the synergies with other surveys. This increased area addresses a wide range of science cases that enhance all of the primary LSST science goals by significant amounts. The science enabled includes: increasing the area of the sky accessible for follow-up of multi-messenger transients including gravitational waves, mapping the milky way halo and halo dwarfs including discovery of RR Lyrae stars in the outer galactic halo, discovery of z>7 quasars in combination Euclid, enabling a second generation DESI and other spectroscopic surveys, and enhancing all areas of science by improving synergies with Euclid, WFIRST, and unique northern survey facilities. This white paper is the result of the Tri-Agency Working Group (TAG) appointed to develop synergies between missions and presents a unified plan for northern coverage. The range of time estimates reflects synergies with other surveys. If the modified DESC WFD survey, the ecliptic plane mini survey, and the north galactic spur mini survey are executed this plan would only need 0.6% of the LSST time, however if none of these are included the overall request is 2.5% of the 10 year survey life. In other words, the majority of these observations are already suggested as part of these other surveys and the intent of this white paper is to propose a unified baseline plan to carry out a broad range of objectives to facilitate a combination of multiple science objectives. A companion white paper gives Euclid specific science goals, and we support the white papers for southern extensions of the LSST survey.", "doi": "10.48550/arXiv.1904.10438", "publisher": "arXiv", "publication_date": "2019-04-23" }, { "id": "authors:rpaxd-3ys70", "collection": "authors", "collection_id": "rpaxd-3ys70", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190813-093516063", "type": "monograph", "title": "Enhancing LSST Science with Euclid Synergy", "author": [ { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Cuillandre", "given_name": "J-C.", "clpid": "Cuillandre-J-C" }, { "family_name": "Bernardeau", "given_name": "F.", "clpid": "Bernardeau-F" }, { "family_name": "Castander", "given_name": "F.", "clpid": "Castander-F" }, { "family_name": "Bowler", "given_name": "R.", "clpid": "Bowler-R-A-A" }, { "family_name": "Chang", "given_name": "C.", "clpid": "Chang-C" }, { "family_name": "Grillmair", "given_name": "C.", "orcid": "0000-0003-4072-169X", "clpid": "Grillmair-C-J" }, { "family_name": "Gris", "given_name": "P.", "clpid": "Gris-P" }, { "family_name": "Eifler", "given_name": "T.", "orcid": "0000-0002-1894-3301", "clpid": "Eifler-T-F" }, { "family_name": "Hirata", "given_name": "C.", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Hook", "given_name": "I.", "orcid": "0000-0002-2960-978X", "clpid": "Hook-I-M" }, { "family_name": "Jain", "given_name": "B.", "clpid": "Jain-B" }, { "family_name": "Kuijken", "given_name": "K.", "clpid": "Kuijken-K" }, { "family_name": "Lochner", "given_name": "M.", "orcid": "0000-0003-2221-8281", "clpid": "Lochner-M" }, { "family_name": "Oesch", "given_name": "P.", "orcid": "0000-0001-5851-6649", "clpid": "Oesch-P-A" }, { "family_name": "Paltani", "given_name": "S.", "orcid": "0000-0002-8108-9179", "clpid": "Paltani-S" }, { "family_name": "Rhodes", "given_name": "J.", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" }, { "family_name": "Robertson", "given_name": "B.", "clpid": "Robertson-B" }, { "family_name": "Rubin", "given_name": "D.", "clpid": "Rubin-D" }, { "family_name": "Scaramella", "given_name": "R.", "clpid": "Scaramella-R" }, { "family_name": "Scarlata", "given_name": "C.", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-C-M" }, { "family_name": "Scolnic", "given_name": "D.", "orcid": "0000-0002-4934-5849", "clpid": "Scolnic-D" }, { "family_name": "Silverman", "given_name": "J.", "orcid": "0000-0002-0000-6977", "clpid": "Silverman-J-D" }, { "family_name": "Wachter", "given_name": "S.", "clpid": "Wachter-S" }, { "family_name": "Wang", "given_name": "Y.", "clpid": "Wang-Yun" }, { "literal": "Tri-Agency Working Group" } ], "abstract": "This white paper is the result of the Tri-Agency Working Group (TAG) appointed to develop synergies between missions and is intended to clarify what LSST observations are needed in order to maximally enhance the combined science output of LSST and Euclid. To facilitate LSST planning we provide a range of possible LSST surveys with clear metrics based on the improvement in the Dark Energy figure of merit (FOM). To provide a quantifiable metric we present five survey options using only between 0.3 and 3.8% of the LSST 10 year survey. We also provide information so that the LSST DDF cadence can possibly be matched to those of \\emph{Euclid} in common deep fields, SXDS, COSMOS, CDFS, and a proposed new LSST deep field (near the Akari Deep Field South). Co-coordination of observations from the Large Synoptic Survey Telescope (LSST) and Euclid will lead to a significant number of synergies. The combination of optical multi-band imaging from LSST with high resolution optical and near-infrared photometry and spectroscopy from \\emph{Euclid} will not only improve constraints on Dark Energy, but provide a wealth of science on the Milky Way, local group, local large scale structure, and even on first galaxies during the epoch of reionization. A detailed paper has been published on the Dark Energy science case (Rhodes et al.) by a joint LSST/Euclid working group as well as a white paper describing LSST/Euclid/WFIRST synergies (Jain et al.), and we will briefly describe other science cases here. A companion white paper argues the general science case for an extension of the LSST footprint to the north at airmass < 1.8, and we support the white papers for southern extensions of the LSST survey.", "doi": "10.48550/arXiv.1904.10439", "publisher": "arXiv", "publication_date": "2019-04-23" }, { "id": "authors:6f28t-ekq93", "collection": "authors", "collection_id": "6f28t-ekq93", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190813-094200294", "type": "monograph", "title": "An Ultra Deep Field survey with WFIRST", "author": [ { "family_name": "Koekemoer", "given_name": "Anton M.", "orcid": "0000-0002-6610-2048", "clpid": "Koekemoer-A-M" }, { "family_name": "Foley", "given_name": "R. J." }, { "family_name": "Spergel", "given_name": "D. N." }, { "family_name": "Bagley", "given_name": "M." }, { "family_name": "Bezanson", "given_name": "R." }, { "family_name": "Bianco", "given_name": "F. B." }, { "family_name": "Bouwens", "given_name": "R." }, { "family_name": "Bradley", "given_name": "L." }, { "family_name": "Brammer", "given_name": "G." }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Davidzon", "given_name": "I.", "orcid": "0000-0002-2951-7519", "clpid": "Davidzon-I" }, { "family_name": "De Rosa", "given_name": "G." }, { "family_name": "Dickinson", "given_name": "M. E." }, { "family_name": "Dor\u00e9", "given_name": "O." }, { "family_name": "Dunlop", "given_name": "J. S." }, { "family_name": "Ellis", "given_name": "R. S." }, { "family_name": "Fan", "given_name": "X." }, { "family_name": "Fazio", "given_name": "G. G." }, { "family_name": "Ferguson", "given_name": "H. C." }, { "family_name": "Filippenko", "given_name": "A. V." }, { "family_name": "Finkelstein", "given_name": "S." }, { "family_name": "Frye", "given_name": "B." }, { "family_name": "Gawiser", "given_name": "E." }, { "family_name": "Grogin", "given_name": "N. A." }, { "family_name": "Hathi", "given_name": "N. P." }, { "family_name": "Hirata", "given_name": "C. M." }, { "family_name": "Hounsell", "given_name": "R." }, { "family_name": "Illingworth", "given_name": "G. D." }, { "family_name": "Jansen", "given_name": "R. A." }, { "family_name": "Jauzac", "given_name": "M." }, { "family_name": "Jha", "given_name": "S. W." }, { "family_name": "Kartaltepe", "given_name": "J. S." }, { "family_name": "Kim", "given_name": "A. G." }, { "family_name": "Kelly", "given_name": "P." }, { "family_name": "Kruk", "given_name": "J. W." }, { "family_name": "Larson", "given_name": "R." }, { "family_name": "Lotz", "given_name": "J." }, { "family_name": "Lucas", "given_name": "R." }, { "family_name": "Malhotra", "given_name": "S." }, { "family_name": "Mandel", "given_name": "K." }, { "family_name": "Margutti", "given_name": "R." }, { "family_name": "Marrone", "given_name": "D." }, { "family_name": "McLure", "given_name": "R. J." }, { "family_name": "McQuinn", "given_name": "K." }, { "family_name": "Melchior", "given_name": "P." }, { "family_name": "Mobasher", "given_name": "B." }, { "family_name": "Mould", "given_name": "J. R." }, { "family_name": "Moustakas", "given_name": "L." }, { "family_name": "Newman", "given_name": "J. A." }, { "family_name": "Papovich", "given_name": "C." }, { "family_name": "Peeples", "given_name": "M. S." }, { "family_name": "Perlmutter", "given_name": "S." }, { "family_name": "Pirzkal", "given_name": "N." }, { "family_name": "Rhoads", "given_name": "J." }, { "family_name": "Rhodes", "given_name": "J." }, { "family_name": "Robertson", "given_name": "B." }, { "family_name": "Rubin", "given_name": "D." }, { "family_name": "Ryan", "given_name": "R." }, { "family_name": "Scolnic", "given_name": "D." }, { "family_name": "Shapley", "given_name": "A." }, { "family_name": "Somerville", "given_name": "R." }, { "family_name": "Steinhardt", "given_name": "C." }, { "family_name": "Stiavelli", "given_name": "M." }, { "family_name": "Street", "given_name": "R." }, { "family_name": "Trenti", "given_name": "M." }, { "family_name": "Treu", "given_name": "T." }, { "family_name": "Wang", "given_name": "L." }, { "family_name": "Wang", "given_name": "Y.", "clpid": "Wang-Yun" }, { "family_name": "Whalen", "given_name": "D." }, { "family_name": "Windhorst", "given_name": "R. A." }, { "family_name": "Wollack", "given_name": "E. J." }, { "family_name": "Yan", "given_name": "H." } ], "abstract": "Studying the formation and evolution of galaxies at the earliest cosmic times, and their role in reionization, requires the deepest imaging possible. Ultra-deep surveys like the HUDF and HFF have pushed to mag m_(AB)\u223c30, revealing galaxies at the faint end of the LF to z\u223c9\u221211 and constraining their role in reionization. However, a key limitation of these fields is their size, only a few arcminutes (less than a Mpc at these redshifts), too small to probe large-scale environments or clustering properties of these galaxies, crucial for advancing our understanding of reionization. Achieving HUDF-quality depth over areas \u223c100 times larger becomes possible with a mission like the Wide Field Infrared Survey Telescope (WFIRST), a 2.4-m telescope with similar optical properties to HST, with a field of view of \u223c1000 arcmin^2, \u223c100\u00d7 the area of the HST/ACS HUDF. \nThis whitepaper motivates an Ultra-Deep Field survey with WFIRST, covering \u223c100\u2212300\u00d7 the area of the HUDF, or up to \u223c1 deg^2, to m_(AB)\u223c30, potentially revealing thousands of galaxies and AGN at the faint end of the LF, at or beyond z\u223c9\u221210 in the epoch of reionization, and tracing their LSS environments, dramatically increasing the discovery potential at these redshifts. \n\n(Note: This paper is a somewhat expanded version of one that was submitted as input to the Astro2020 Decadal Survey, with this version including an Appendix (which exceeded the Astro2020 page limits), describing how the science drivers for a WFIRST Ultra Deep Field might map into a notional observing program, including the filters used and exposure times needed to achieve these depths.)", "doi": "10.48550/arXiv.1903.06154", "publisher": "arXiv", "publication_date": "2019-03-14" }, { "id": "authors:3m3f9-mrb52", "collection": "authors", "collection_id": "3m3f9-mrb52", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180904-154905435", "type": "monograph", "title": "Science Impacts of the SPHEREx All-Sky Optical to Near-Infrared Spectral Survey II: Report of a Community Workshop on the Scientific Synergies Between the SPHEREx Survey and Other Astronomy Observatories", "author": [ { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "de la Torre", "given_name": "Sylvain", "orcid": "0000-0002-0839-2884", "clpid": "de-la-Torre-S" }, { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" }, { "family_name": "Teplitz", "given_name": "Harry", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Werner", "given_name": "Michael", "clpid": "Werner-M-W" }, { "family_name": "Bock", "given_name": "Jamie", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Chang", "given_name": "Tzu-Ching", "clpid": "Chang-Tzu-Ching" }, { "family_name": "Crill", "given_name": "Brendan", "orcid": "0000-0002-4650-8518", "clpid": "Crill-B-P" }, { "family_name": "Korngut", "given_name": "Phil", "clpid": "Korngut-P-M" }, { "family_name": "Scoville", "given_name": "Nick Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" } ], "abstract": "SPHEREx is a proposed NASA MIDEX mission selected for Phase A study. SPHEREx would carry out the first all-sky spectral survey in the near infrared. At the end of its two-year mission, SPHEREx would obtain 0.75-to-5\u03bcm spectra of every 6.2 arcsec pixel on the sky, with spectral resolution R>35 and a 5-\u03c3 sensitivity AB>19 per spectral/spatial resolution element. More details concerning SPHEREx are available at http://spherex.caltech.edu. The SPHEREx team has proposed three specific science investigations to be carried out with this unique data set: cosmic inflation, interstellar and circumstellar ices, and the extra-galactic background light. Though these three themes are undoubtedly compelling, they are far from exhausting the scientific output of SPHEREx. Indeed, SPHEREx would create a unique all-sky spectral database including spectra of very large numbers of astronomical and solar system targets, including both extended and diffuse sources. These spectra would enable a wide variety of investigations, and the SPHEREx team is dedicated to making the data available to the community to enable these investigations, which we refer to as Legacy Science. To that end, we have sponsored two workshops for the general scientific community to identify the most interesting Legacy Science themes and to ensure that the SPHEREx data products are responsive to their needs. In February of 2016, some 50 scientists from all fields met in Pasadena to develop these themes and to understand their implications for the SPHEREx mission. The 2016 workshop highlighted many synergies between SPHEREx and other contemporaneous astronomical missions, facilities, and databases. Consequently, in January 2018 we convened a second workshop at the Center for Astrophysics in Cambridge to focus specifically on these synergies. This white paper reports on the results of the 2018 SPHEREx workshop.", "doi": "10.48550/arXiv.1805.05489", "publication_date": "2018-05-14" }, { "id": "authors:2d6nt-2j991", "collection": "authors", "collection_id": "2d6nt-2j991", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180904-161455265", "type": "monograph", "title": "WFIRST Science Investigation Team \"Cosmology with the High Latitude Survey\" Annual Report 2017", "author": [ { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Hirata", "given_name": "Christopher", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Wang", "given_name": "Yun", "clpid": "Wang-Yun" }, { "family_name": "Weinberg", "given_name": "David", "clpid": "Weinberg-D" }, { "family_name": "Baronchelli", "given_name": "Ivano", "orcid": "0000-0003-0556-2929", "clpid": "Baronchelli-I" }, { "family_name": "Benson", "given_name": "Andrew", "orcid": "0000-0001-5501-6008", "clpid": "Benson-A-J" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Choi", "given_name": "Ami", "clpid": "Choi-Ami" }, { "family_name": "Eifler", "given_name": "Tim", "orcid": "0000-0002-1894-3301", "clpid": "Eifler-T-F" }, { "family_name": "Hemmati", "given_name": "Shoubaneh", "orcid": "0000-0003-2226-5395", "clpid": "Hemmati-S" }, { "family_name": "Ho", "given_name": "Shirley", "clpid": "Ho-Shirley" }, { "family_name": "Izard", "given_name": "Albert", "clpid": "Izard-A" }, { "family_name": "Jain", "given_name": "Bhuvnesh", "clpid": "Jain-B" }, { "family_name": "Jarvis", "given_name": "Mike", "clpid": "Jarvis-M" }, { "family_name": "Kiessling", "given_name": "Alina", "clpid": "Kiessling-A" }, { "family_name": "Krause", "given_name": "Elisabeth", "clpid": "Krause-E" }, { "family_name": "Massara", "given_name": "Elena", "clpid": "Massara-E" }, { "family_name": "Masters", "given_name": "Dan", "orcid": "0000-0001-5382-6138", "clpid": "Masters-D-C" }, { "family_name": "Merson", "given_name": "Alex", "clpid": "Merson-A-I" }, { "family_name": "Miyatake", "given_name": "Hironao", "clpid": "Miyatake-Hironao" }, { "family_name": "Malagon", "given_name": "Andres Plazas", "clpid": "Malagon-A-P" }, { "family_name": "Mandelbaum", "given_name": "Rachel", "orcid": "0000-0003-2271-1527", "clpid": "Mandelbaum-R" }, { "family_name": "Samushia", "given_name": "Lado", "clpid": "Samushia-L" }, { "family_name": "Shapiro", "given_name": "Chaz", "clpid": "Shapiro-C" }, { "family_name": "Simet", "given_name": "Melanie", "clpid": "Simet-M" }, { "family_name": "Spergel", "given_name": "David", "orcid": "0000-0002-5151-0006", "clpid": "Spergel-D-N" }, { "family_name": "Teplitz", "given_name": "Harry", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Troxel", "given_name": "Michael", "clpid": "Troxel-M" }, { "family_name": "Bean", "given_name": "Rachel", "clpid": "Bean-R" }, { "family_name": "Colbert", "given_name": "James", "clpid": "Colbert-J-W" }, { "family_name": "Heinrich", "given_name": "Chen He", "clpid": "Heinrich-Chen-He" }, { "family_name": "Heitmann", "given_name": "Katrin", "clpid": "Heitmann-K" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Hudson", "given_name": "Michael", "clpid": "Hudson-M-J" }, { "family_name": "Huff", "given_name": "Eric", "orcid": "0000-0002-9378-3424", "clpid": "Huff-E-M" }, { "family_name": "Leauthaud", "given_name": "Alexie", "orcid": "0000-0002-3677-3617", "clpid": "Leauthaud-A" }, { "family_name": "MacCrann", "given_name": "Niall", "clpid": "MacCrann-N" }, { "family_name": "Padmanabhan", "given_name": "Nikhil", "clpid": "Padmanabhan-N" }, { "family_name": "Pisani", "given_name": "Alice", "clpid": "Pisani-A" }, { "family_name": "Rhodes", "given_name": "Jason", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" }, { "family_name": "Rozo", "given_name": "Eduardo", "clpid": "Rozo-E" }, { "family_name": "Seiffert", "given_name": "Mike", "clpid": "Seiffert-M" }, { "family_name": "Smith", "given_name": "Kendrick", "clpid": "Smith-Kendrick" }, { "family_name": "Takada", "given_name": "Masahiro", "clpid": "Takada-Masahiro" }, { "family_name": "von der Linden", "given_name": "Anja", "clpid": "von-der-Linden-A" }, { "family_name": "Lupton", "given_name": "Robert", "orcid": "0000-0003-1666-0962", "clpid": "Lupton-R-H" }, { "family_name": "Yoshida", "given_name": "Naoki", "clpid": "Yoshida-Naoki" }, { "family_name": "Wu", "given_name": "Hao-Yi", "clpid": "Wu-Hao-Yi" }, { "family_name": "Zu", "given_name": "Ying", "clpid": "Zu-Ying" } ], "abstract": "Cosmic acceleration is the most surprising cosmological discovery in many decades. Testing and distinguishing among possible explanations requires cosmological measurements of extremely high precision probing the full history of cosmic expansion and structure growth and, ideally, compare and contrast matter and relativistic tracers of the gravity potential. This program is one of the defining objectives of the Wide-Field Infrared Survey Telescope (WFIRST), as set forth in the New Worlds, New Horizons report (NWNH) in 2010. The WFIRST mission has the ability to improve these measurements by 1-2 orders of magnitude compared to the current state of the art, while simultaneously extending their redshift grasp, greatly improving control of systematic effects, and taking a unified approach to multiple probes that provide complementary physical information and cross-checks of cosmological results. We describe in this annual report the activities of the Science Investigation Team (SIT) \"Cosmology with the High Latitude Survey (HLS)\" during the year 2017. This team was selected by NASA in December 2015 in order to address the stringent challenges of the WFIRST dark energy (DE) program through the Project's formulation phase. This SIT has elected to jointly address Galaxy Redshift Survey, Weak Lensing and Cluster Growth and thus fully embrace the fact that the imaging and spectroscopic elements of the HLS will be realized as an integrated observing program, and they jointly impose requirements on performance and operations. WFIRST is designed to be able to deliver a definitive result on the origin of cosmic acceleration. It is not optimized for Figure of Merit sensitivity but for control of systematic uncertainties and for having multiple techniques each with multiple cross-checks. Our SIT work focuses on understanding the potential systematics in the WFIRST DE measurements.", "doi": "10.48550/arXiv.1804.03628", "publisher": "arXiv", "publication_date": "2018-04-10" }, { "id": "authors:2j5cr-vhm22", "collection": "authors", "collection_id": "2j5cr-vhm22", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180907-095533038", "type": "monograph", "title": "The Science Case for an Extended Spitzer Mission", "author": [ { "family_name": "Yee", "given_name": "Jennifer C.", "orcid": "0000-0001-9481-7123", "clpid": "Yee-Jennifer-C" }, { "family_name": "Ciardi", "given_name": "David R.", "orcid": "0000-0002-5741-3047", "clpid": "Ciardi-D-R" }, { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Teplitz", "given_name": "H. I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "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": "Krick", "given_name": "Jessica E.", "clpid": "Krick-Jessica-E" }, { "family_name": "Lowrance", "given_name": "Patrick J.", "orcid": "0000-0001-8014-0270", "clpid": "Lowrance-P-J" }, { "family_name": "Grillmair", "given_name": "Carl J.", "orcid": "0000-0003-4072-169X", "clpid": "Grillmair-C-J" }, { "family_name": "Mahoney", "given_name": "William A.", "clpid": "Mahoney-W-A" } ], "abstract": "Although the final observations of the Spitzer Warm Mission are currently scheduled for March 2019, it can continue operations through the end of the decade with no loss of photometric precision. As we will show, there is a strong science case for extending the current Warm Mission to December 2020. Spitzer has already made major impacts in the fields of exoplanets (including microlensing events), characterizing near Earth objects, enhancing our knowledge of nearby stars and brown dwarfs, understanding the properties and structure of our Milky Way galaxy, and deep wide-field extragalactic surveys to study galaxy birth and evolution. By extending Spitzer through 2020, it can continue to make ground-breaking discoveries in those fields, and provide crucial support to the NASA flagship missions JWST and WFIRST, as well as the upcoming TESS mission, and it will complement ground-based observations by LSST and the new large telescopes of the next decade. This scientific program addresses NASA's Science Mission Directive's objectives in astrophysics, which include discovering how the universe works, exploring how it began and evolved, and searching for life on planets around other stars.", "doi": "10.48550/arXiv.1710.04194", "publication_date": "2017-10-11" }, { "id": "authors:ts3gk-d8y56", "collection": "authors", "collection_id": "ts3gk-d8y56", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180914-101943065", "type": "monograph", "title": "Science Impacts of the SPHEREx All-Sky Optical to Near-Infrared Spectral Survey: Report of a Community Workshop Examining Extragalactic, Galactic, Stellar and Planetary Science", "author": [ { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" }, { "family_name": "Werner", "given_name": "Michael", "clpid": "Werner-M-W" }, { "family_name": "Bock", "given_name": "Jamie", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bull", "given_name": "Philip", "clpid": "Bull-P" }, { "family_name": "Crill", "given_name": "Brendan", "orcid": "0000-0002-4650-8518", "clpid": "Crill-B-P" }, { "family_name": "de Putter", "given_name": "Roland", "clpid": "de-Putter-R" }, { "family_name": "Eifler", "given_name": "Tim", "orcid": "0000-0002-1894-3301", "clpid": "Eifler-T-F" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" }, { "family_name": "Korngut", "given_name": "Phillip", "clpid": "Korngut-P-M" }, { "family_name": "Nguyen", "given_name": "Hien", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Rhodes", "given_name": "Jason", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" } ], "abstract": "SPHEREx is a proposed SMEX mission selected for Phase A. SPHEREx will carry out the first all-sky spectral survey and provide for every 6.2\" pixel a spectra between 0.75 and 4.18 \u03bcm [with R\u223c41.4] and 4.18 and 5.00 \u03bcm [with R\u223c135]. The SPHEREx team has proposed three specific science investigations to be carried out with this unique data set: cosmic inflation, interstellar and circumstellar ices, and the extra-galactic background light. It is readily apparent, however, that many other questions in astrophysics and planetary sciences could be addressed with the SPHEREx data. The SPHEREx team convened a community workshop in February 2016, with the intent of enlisting the aid of a larger group of scientists in defining these questions. This paper summarizes the rich and varied menu of investigations that was laid out. It includes studies of the composition of main belt and Trojan/Greek asteroids; mapping the zodiacal light with unprecedented spatial and spectral resolution; identifying and studying very low-metallicity stars; improving stellar parameters in order to better characterize transiting exoplanets; studying aliphatic and aromatic carbon-bearing molecules in the interstellar medium; mapping star formation rates in nearby galaxies; determining the redshift of clusters of galaxies; identifying high redshift quasars over the full sky; and providing a NIR spectrum for most eROSITA X-ray sources. All of these investigations, and others not listed here, can be carried out with the nominal all-sky spectra to be produced by SPHEREx. In addition, the workshop defined enhanced data products and user tools which would facilitate some of these scientific studies. Finally, the workshop noted the high degrees of synergy between SPHEREx and a number of other current or forthcoming programs, including JWST, WFIRST, Euclid, GAIA, K2/Kepler, TESS, eROSITA and LSST.", "doi": "10.48550/arXiv.1606.07039", "publication_date": "2016-06-22" }, { "id": "authors:vjtnf-xxt92", "collection": "authors", "collection_id": "vjtnf-xxt92", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180911-163142346", "type": "monograph", "title": "An Empirical Approach to Cosmological Galaxy Survey Simulation: Application to SPHEREx Low-Resolution Spectroscopy", "author": [ { "family_name": "Stickley", "given_name": "Nathaniel R.", "clpid": "Stickley-N-R" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Masters", "given_name": "Daniel", "orcid": "0000-0001-5382-6138", "clpid": "Masters-D-C" }, { "family_name": "de Putter", "given_name": "Roland", "clpid": "de-Putter-R" }, { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Bock", "given_name": "Jamie", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" } ], "abstract": "Highly accurate models of the galaxy population over cosmological volumes are necessary in order to predict the performance of upcoming cosmological missions. We present a data-driven model of the galaxy population constrained by deep 0.1-8 \u03bcm imaging and spectroscopic data in the COSMOS survey, with the immediate goal of simulating the spectroscopic redshift performance of the proposed SPHEREx mission. SPHEREx will obtain over the full-sky R\u223c41 spectrophotometry at moderate spatial resolution (\u223c6\") over the wavelength range 0.75-4.18 \u03bcm and R\u223c135 over the wavelength range 4.18-5 \u03bcm. We show that our simulation accurately reproduces a range of known galaxy properties, encapsulating the full complexity of the galaxy population and enables realistic, full end-to-end simulations to predict mission performance. Finally, we discuss potential applications of the simulation framework to future cosmology missions and give a description of released data products.", "doi": "10.48550/arXiv.1606.06374", "publication_date": "2016-06-21" }, { "id": "authors:hnsv3-9d647", "collection": "authors", "collection_id": "hnsv3-9d647", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170629-130428473", "type": "monograph", "title": "Wide-Field InfrarRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA 2015 Report", "author": [ { "family_name": "Spergel", "given_name": "D.", "orcid": "0000-0002-5151-0006", "clpid": "Spergel-D-N" }, { "family_name": "Gehrels", "given_name": "N.", "clpid": "Gehrels-N" }, { "family_name": "Baltay", "given_name": "C.", "clpid": "Baltay-C" }, { "family_name": "Bennett", "given_name": "D.", "orcid": "0000-0001-8043-8413", "clpid": "Bennett-D-P" }, { "family_name": "Breckinridge", "given_name": "J.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Donahue", "given_name": "M.", "orcid": "0000-0002-2808-0853", "clpid": "Donahue-Megan" }, { "family_name": "Dressler", "given_name": "A.", "clpid": "Dressler-A" }, { "family_name": "Gaudi", "given_name": "B. S.", "orcid": "0000-0003-0395-9869", "clpid": "Gaudi-B-S" }, { "family_name": "Greene", "given_name": "T.", "orcid": "0000-0002-8963-8056", "clpid": "Greene-T-P" }, { "family_name": "Guyon", "given_name": "O.", "orcid": "0000-0002-1097-9908", "clpid": "Guyon-O" }, { "family_name": "Hirata", "given_name": "C.", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Kalirai", "given_name": "J.", "orcid": "0000-0001-9690-4159", "clpid": "Kalirai-J-S" }, { "family_name": "Kasdin", "given_name": "N. J.", "clpid": "Kasdin-N-J" }, { "family_name": "Macintosh", "given_name": "B.", "orcid": "0000-0003-1212-7538", "clpid": "Macintosh-B-A" }, { "family_name": "Moos", "given_name": "W.", "clpid": "Moos-W" }, { "family_name": "Perlmutter", "given_name": "S.", "clpid": "Perlmutter-S" }, { "family_name": "Postman", "given_name": "M.", "orcid": "0000-0002-9365-7989", "clpid": "Postman-Marc" }, { "family_name": "Rauscher", "given_name": "B.", "clpid": "Rauscher-B-J" }, { "family_name": "Rhodes", "given_name": "J.", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" }, { "family_name": "Wang", "given_name": "Y.", "clpid": "Wang-Y" }, { "family_name": "Weinberg", "given_name": "D.", "clpid": "Weinberg-D" }, { "family_name": "Benford", "given_name": "D.", "orcid": "0000-0002-9884-4206", "clpid": "Benford-D-J" }, { "family_name": "Hudson", "given_name": "M.", "clpid": "Hudson-M" }, { "family_name": "Jeong", "given_name": "W.-S.", "clpid": "Jeong-Woong-Seob" }, { "family_name": "Mellier", "given_name": "Y.", "clpid": "Mellier-Y" }, { "family_name": "Traub", "given_name": "W.", "clpid": "Traub-W-A" }, { "family_name": "Yamada", "given_name": "T.", "clpid": "Yamada-Toru" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Colbert", "given_name": "J.", "clpid": "Colbert-J-W" }, { "family_name": "Masters", "given_name": "D.", "orcid": "0000-0001-5382-6138", "clpid": "Masters-D-C" }, { "family_name": "Penny", "given_name": "M.", "orcid": "0000-0001-7506-5640", "clpid": "Penny-M-T" }, { "family_name": "Savransky", "given_name": "D.", "clpid": "Savransky-D" }, { "family_name": "Stern", "given_name": "D.", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Zimmerman", "given_name": "N.", "orcid": "0000-0001-5484-1516", "clpid": "Zimmerman-N" }, { "family_name": "Barry", "given_name": "R.", "clpid": "Barry-R-K" }, { "family_name": "Bartusek", "given_name": "L.", "clpid": "Bartusek-L" }, { "family_name": "Carpenter", "given_name": "K.", "orcid": "0000-0002-1085-9949", "clpid": "Carpenter-K-C" }, { "family_name": "Cheng", "given_name": "E.", "clpid": "Cheng-E" }, { "family_name": "Content", "given_name": "D.", "clpid": "Content-D" }, { "family_name": "Dekens", "given_name": "F.", "clpid": "Dekens-F-G" }, { "family_name": "Demers", "given_name": "R.", "clpid": "Demers-R" }, { "family_name": "Grady", "given_name": "K.", "clpid": "Grady-K" }, { "family_name": "Jackson", "given_name": "C.", "clpid": "Jackson-C" }, { "family_name": "Kuan", "given_name": "G.", "clpid": "Kuan-Gary" }, { "family_name": "Kruk", "given_name": "J.", "orcid": "0000-0002-5861-7236", "clpid": "Kruk-J-W" }, { "family_name": "Melton", "given_name": "M.", "clpid": "Melton-M" }, { "family_name": "Nemati", "given_name": "B.", "clpid": "Nemati-B" }, { "family_name": "Parvin", "given_name": "B.", "clpid": "Parvin-B" }, { "family_name": "Poberezhskiy", "given_name": "I.", "clpid": "Poberezhskiy-I" }, { "family_name": "Peddie", "given_name": "C.", "clpid": "Peddie-C" }, { "family_name": "Ruffa", "given_name": "J.", "clpid": "Ruffa-J" }, { "family_name": "Wallace", "given_name": "J. K.", "clpid": "Wallace-J-K" }, { "family_name": "Whipple", "given_name": "A.", "clpid": "Whipple-A" }, { "family_name": "Wollack", "given_name": "E.", "orcid": "0000-0002-7567-4451", "clpid": "Wollack-E-J" }, { "family_name": "Zhao", "given_name": "F.", "clpid": "Zhao-F" }, { "literal": "WFIRST Study Office" }, { "literal": "Science Definition Team" } ], "abstract": "This report describes the 2014 study by the Science Definition Team (SDT) of the Wide-Field Infrared Survey Telescope (WFIRST) mission. It is a space observatory that will address the most compelling scientific problems in dark energy, exoplanets and general astrophysics using a 2.4-m telescope with a wide-field infrared instrument and an optical coronagraph. The Astro2010 Decadal Survey recommended a Wide Field Infrared Survey Telescope as its top priority for a new large space mission. As conceived by the decadal survey,\nWFIRST would carry out a dark energy science program, a microlensing program to\ndetermine the demographics of exoplanets, and a general observing program\nutilizing its ultra wide field. In October 2012, NASA chartered a Science\nDefinition Team (SDT) to produce, in collaboration with the WFIRST Study Office\nat GSFC and the Program Office at JPL, a Design Reference Mission (DRM) for an\nimplementation of WFIRST using one of the 2.4-m, Hubble-quality telescope\nassemblies recently made available to NASA. This DRM builds on the work of the\nearlier WFIRST SDT, reported by Green et al. (2012) and the previous WFIRST-2.4\nDRM, reported by Spergel et. (2013). The 2.4-m primary mirror enables a mission\nwith greater sensitivity and higher angular resolution than the 1.3-m and 1.1-m\ndesigns considered previously, increasing both the science return of the\nprimary surveys and the capabilities of WFIRST as a Guest Observer facility.\nThe addition of an on-axis coronagraphic instrument to the baseline design\nenables imaging and spectroscopic studies of planets around nearby stars.", "doi": "10.48550/arXiv.1503.03757", "publisher": "arXiv", "publication_date": "2015-03-12" }, { "id": "authors:pfysr-16j58", "collection": "authors", "collection_id": "pfysr-16j58", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180925-102425921", "type": "monograph", "title": "Inter-comparison of Radio-Loudness Criteria for Type 1 AGNs in the XMM-COSMOS Survey", "author": [ { "family_name": "Hao", "given_name": "Heng", "clpid": "Hao-Heng" }, { "family_name": "Sargent", "given_name": "Mark T.", "orcid": "0000-0003-1033-9684", "clpid": "Sargent-M-T" }, { "family_name": "Elvis", "given_name": "Martin", "clpid": "Elvis-M" }, { "family_name": "Schinnerer", "given_name": "Eva", "orcid": "0000-0002-3933-7677", "clpid": "Schinnerer-E" }, { "family_name": "Zamorani", "given_name": "Gianni", "clpid": "Zamorani-G" }, { "family_name": "Ho", "given_name": "Luis C.", "orcid": "0000-0001-6947-5846", "clpid": "Ho-Luis-C" }, { "family_name": "Donley", "given_name": "Jennifer L.", "clpid": "Donley-J-L" }, { "family_name": "Civano", "given_name": "Francesca", "orcid": "0000-0002-2115-1137", "clpid": "Civano-Francesca" }, { "family_name": "Smol\u010di\u0107", "given_name": "Vernesa", "orcid": "0000-0002-3893-8614", "clpid": "Smol\u010di\u0107-V" }, { "family_name": "Celotti", "given_name": "Annalisa", "clpid": "Celotti-A" }, { "family_name": "Kuraszkiewicz", "given_name": "Joanna", "clpid": "Kuraszkiewicz-J" }, { "family_name": "Salvato", "given_name": "Mara", "orcid": "0000-0001-7116-9303", "clpid": "Salvato-Mara" }, { "family_name": "Brusa", "given_name": "Marcella", "orcid": "0000-0002-5059-6848", "clpid": "Brusa-Marcella" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Carilli", "given_name": "Chris L.", "orcid": "0000-0001-6647-3861", "clpid": "Carilli-C-L" }, { "family_name": "Comastri", "given_name": "Andrea", "orcid": "0000-0003-3451-9970", "clpid": "Comastri-A" }, { "family_name": "Impey", "given_name": "Chris D.", "clpid": "Impey-C-D" }, { "family_name": "Jahnke", "given_name": "Knud", "orcid": "0000-0003-3804-2137", "clpid": "Jahnke-K" }, { "family_name": "Koekemoer", "given_name": "Anton M.", "orcid": "0000-0002-6610-2048", "clpid": "Koekemoer-A-M" }, { "family_name": "Schawinski", "given_name": "Kevin", "orcid": "0000-0001-5464-0888", "clpid": "Schawinski-K" }, { "family_name": "Trump", "given_name": "Jonathan R.", "clpid": "Trump-J-R" }, { "family_name": "Urry", "given_name": "C. Megan", "orcid": "0000-0002-0745-9792", "clpid": "Urry-C-M" }, { "family_name": "Vignali", "given_name": "Cristian", "orcid": "0000-0002-8853-9611", "clpid": "Vignali-C" }, { "family_name": "Yun", "given_name": "Min", "orcid": "0000-0001-7095-7543", "clpid": "Yun-Min-S" } ], "abstract": "Limited studies have been performed on the radio-loud fraction in X-ray selected type 1 AGN samples. The consistency between various radio-loudness definitions also needs to be checked. We measure the radio-loudness of the 407 type 1 AGNs in the XMM-COSMOS quasar sample using nine criteria from the literature (six defined in the rest-frame and three defined in the observed frame): R_L = log(L_(5GHz)/L_B), q_(24) = log(L_(24\u03bcm)/L_(1.4GHz)), R_(uv) = log(L_(5GHz)/L _(2500\u00b0A)), R_i = log(L_(1.4GHz)/L_i), R_X = log(\u03bdL_\u03bd (5GHz)/L_X), P_(5GHz) = log(P_(5GHz)(W/Hz/Sr)), R_(L,obs) = log(f_(1.4GHz)/f_B) (observed frame), R_(i,obs) = log(f_(1.4GHz)/f_i) (observed\nframe), and q_(24,obs) = log(f_(24\u03bcm)/f_(1.4GHz)) (observed frame). Using any single criterion\ndefined in the rest-frame, we find a low radio-loud fraction of \u22725% in the XMM-COSMOS type 1 AGN sample, except for R_(uv). Requiring that any two criteria agree\nreduces the radio-loud fraction to \u22722% for about 3/4 of the cases. The low radio-loud fraction cannot be simply explained by the contribution of the host galaxy luminos\nity and reddening. The P_(5GHz) = log(P_(5GHz)(W/Hz/Sr)) gives the smallest radio-loud fraction. Two of the three radio-loud fractions from the criteria defined in the observed frame without k-correction (R_(L,obs) and R_(i,obs)) are much larger than the radio-loud fractions from other criteria.", "doi": "10.48550/arXiv.1408.1090", "publisher": "arXiv", "publication_date": "2014-08-05" } ]