[ { "id": "authors:be6n1-ak678", "collection": "authors", "collection_id": "be6n1-ak678", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220504-215450097", "type": "monograph", "title": "Joint Survey Processing II: Stellar Proper Motions in the COSMOS Field, from Hubble Space Telescope ACS and Subaru Telescope HSC Observations", "author": [ { "family_name": "Fajardo-Acosta", "given_name": "Sergio B.", "orcid": "0000-0001-9309-0102", "clpid": "Fajardo-Acosta-Sergio-B" }, { "family_name": "Faisst", "given_name": "Andreas", "orcid": "0000-0002-9382-9832", "clpid": "Faisst-Andreas-L" }, { "family_name": "Grillmair", "given_name": "Carl J.", "orcid": "0000-0003-4072-169X", "clpid": "Grillmair-Carl-J" }, { "family_name": "Chary", "given_name": "Ranga-Ram", "orcid": "0000-0001-7583-0621", "clpid": "Chary-Ranga-Ram" }, { "family_name": "Paladini", "given_name": "Roberta", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Rusholme", "given_name": "Ben", "orcid": "0000-0001-7648-4142", "clpid": "Rusholme-Benjamin" }, { "family_name": "Stickley", "given_name": "Nathaniel", "orcid": "0000-0003-0987-5738", "clpid": "Stickley-Nathaniel-R" } ], "abstract": "We analyze stellar proper motions in the COSMOS field to assess the presence of bulk motions. At bright magnitudes (G-band 18.5-20.76 AB), we use the proper motions of 1,010 stars in the Gaia DR2 catalog. At the faint end, we computed proper motions of 11,519 point-like objects at i-band magnitudes 19-25 AB using Hubble ACS and Subaru HSC, which span two epochs about 11 years apart. In order to measure these proper motions with unprecedented accuracy at faint magnitudes, we developed a foundational set of astrometric tools which will be required for Joint Survey Processing (JSP) of data from the next generation of optical/infrared surveys. The astrometric grids of Hubble ACS and Subaru HSC mosaics were corrected at the catalog level, using proper motion-propagated and parallax-corrected Gaia DR2 sources. These astrometric corrections were verified using compact extragalactic sources. Upon comparison of our measured proper motions with Gaia DR2, we estimate the uncertainties in our measurements to be ~2--3 mas/yr per axis, down to 25.5 AB mag. We corrected proper motions for the mean motion of the Sun, and we find that late-type main-sequence stars predominantly in the thin disk in the COSMOS field have space velocities mainly towards the Galactic center. We detect candidate high-velocity (> 220 km/s) stars, 6 of them at ~0.4-6 kpc from the Gaia sample, and 5 of them at ~20 kpc from the faint star HSC and ACS sample. The sources from the faint star sample may be candidate halo members of the Sangarius stream.", "doi": "10.48550/arXiv.2203.05658", "publisher": "arXiv", "publication_date": "2022-03-10" }, { "id": "authors:t21jf-jyk53", "collection": "authors", "collection_id": "t21jf-jyk53", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220411-225157319", "type": "monograph", "title": "Illuminating Galaxy Evolution at Cosmic Noon with ISCEA: the Infrared Satellite for Cosmic Evolution Astrophysics", "author": [ { "family_name": "Wang", "given_name": "Yun", "orcid": "0000-0002-4749-2984", "clpid": "Wang-Yun" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-Lee" }, { "family_name": "Benson", "given_name": "Andrew", "orcid": "0000-0001-5501-6008", "clpid": "Benson-Andrew-J" }, { "family_name": "Daddi", "given_name": "Emanuele", "orcid": "0000-0002-3331-9590", "clpid": "Daddi-Emanuele" }, { "family_name": "Faisst", "given_name": "Andreas", "orcid": "0000-0002-9382-9832", "clpid": "Faisst-Andreas-L" }, { "family_name": "Gonzalez", "given_name": "Anthony", "orcid": "0000-0002-0933-8601", "clpid": "Gonzalez-Anthony-H" }, { "family_name": "Papovich", "given_name": "Casey", "orcid": "0000-0001-7503-8482", "clpid": "Papovich-Casey-J" }, { "family_name": "Ninkov", "given_name": "Zoran", "clpid": "Ninkov-Zoran" }, { "family_name": "Robberto", "given_name": "Massimo", "orcid": "0000-0002-9573-3199", "clpid": "Robberto-Massimo" }, { "family_name": "Rose", "given_name": "Randall J.", "clpid": "Rose-Randall-J" }, { "family_name": "Rose", "given_name": "Thomas", "clpid": "Rose-Thomas" }, { "family_name": "Scarlata", "given_name": "Claudia", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-Claudia-M" }, { "family_name": "Stanford", "given_name": "S. A.", "orcid": "0000-0003-0122-0841", "clpid": "Stanford-Specncer-A" }, { "family_name": "Veach", "given_name": "Todd", "clpid": "Veach-Todd" }, { "family_name": "Zhai", "given_name": "Zhongxu", "orcid": "0000-0001-7984-5476", "clpid": "Zhai-Zhongxu" }, { "family_name": "Benson", "given_name": "Bradford", "orcid": "0000-0002-5108-6823", "clpid": "Benson-Bradford-A" }, { "family_name": "Bleem", "given_name": "L. E.", "orcid": "0000-0001-7665-5079", "clpid": "Bleem-Lindsey-E" }, { "family_name": "Davis", "given_name": "Michael W.", "clpid": "Davis-Michael-W" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" } ], "abstract": "ISCEA (Infrared Satellite for Cosmic Evolution Astrophysics) is a small astrophysics mission whose Science Goal is to discover how galaxies evolved in the cosmic web of dark matter at cosmic noon. Its Science Objective is to determine the history of star formation and its quenching in galaxies as a function of local density and stellar mass when the Universe was 3-5 Gyrs old (1.2 < z < 2.1). ISCEA is designed to test the Science Hypothesis that during the period of cosmic noon, at 1.7 < z < 2.1, environmental quenching is the dominant quenching mechanism for typical galaxies not only in clusters and groups, but also in the extended cosmic web surrounding these structures. ISCEA meets its Science Objective by making a 10% shot noise measurement of star formation rate down to 6 M_\u2299\u2002 yr\u207b\u00b9 using H-\u03b1 out to a radius > 10 Mpc in each of 50 protocluster (cluster and cosmic web) fields at 1.2 < z < 2.1. ISCEA measures the star formation quenching factor in those fields, and galaxy kinematics with a precision < 50 km s\u207b\u00b9 to deduce the 3D spatial distribution in each field. ISCEA will transform our understanding of galaxy evolution at cosmic noon. \n\nISCEA is a small satellite observatory with a 30 cm equivalent diameter aperture telescope with a FoV of 0.32 deg\u00b2, and a multi-object spectrograph with a digital micro-mirror device (DMD) as its programmable slit mask. ISCEA will obtain spectra of 1000 galaxies simultaneously at an effective resolving power of R = 1000, with 2.8\" x 2.8\" slits, over the NIR wavelength range of 1.1 to 2.0 \u00b5m, a regime not accessible from the ground without large gaps in coverage. ISCEA will achieve a pointing accuracy of \u2264 2\" FWHM over 200s. ISCEA will be launched into a Low Earth Orbit, with a prime mission of 2.5 years. ISCEA's space-qualification of DMDs opens a new window for spectroscopy from space, enabling revolutionary advances in astrophysics.", "doi": "10.48550/arXiv.2112.02387", "publisher": "arXiv", "publication_date": "2021-12-04" } ]