TY - JOUR
T1 - Diagnosing DASH
T2 - A Catalog of Structural Properties for the COSMOS-DASH Survey
AU - Cutler, Sam E.
AU - Whitaker, Katherine E.
AU - Mowla, Lamiya A.
AU - Brammer, Gabriel B.
AU - Van Der Wel, Arjen
AU - Marchesini, Danilo
AU - Van Dokkum, Pieter G.
AU - Momcheva, Ivelina G.
AU - Song, Mimi
AU - Akhshik, Mohammad
AU - Nelson, Erica J.
AU - Bezanson, Rachel
AU - Franx, Marijn
AU - Kriek, Mariska
AU - Lange-Vagle, Daniel
AU - Leja, Joel
AU - Mackenty, John W.
AU - Muzzin, Adam
AU - Shipley, Heath
N1 - Funding Information:
This paper is based on observations made with the NASA/ESA HST, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program HST-GO-14114. Support for GO-14114 is gratefully acknowledged. S.C. and K.W. wish to acknowledge funding from the Alfred P. Sloan Foundation grant Nos. FG-2019-12514, HST-AR-15027, and HST-GO-16259. MA acknowledges support by NASA under award No 80NSSC19K1418. M.S. and K.W. acknowledge support under NASA grant No. 80NSSC20K0416. This research made use of Montage. It is funded by the National Science Foundation under grant No. ACI-1440620 and was previously funded by the National Aeronautics and Space Administrations Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement No. NCC5-626 between NASA and the California Institute of Technology. The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/1/1
Y1 - 2022/1/1
N2 - We present the H 160 morphological catalogs for the COSMOS-DASH survey, the largest area near-IR survey using HST-WFC3 to date. Utilizing the "Drift And SHift"observing technique for HST-WFC3 imaging, the COSMOS-DASH survey imaged approximately 0.5 deg2 of the UltraVISTA deep stripes (0.7 deg2, when combined with archival data). Global structural parameters are measured for 51,586 galaxies within COSMOS-DASH using GALFIT (excluding the CANDELS area) with detection using a deep multi-band HST image. We recover consistent results with those from the deeper 3D-HST morphological catalogs, finding that, in general, sizes and Sérsic indices of typical galaxies are accurate to limiting magnitudes of H 160 < 23 and H 160 < 22 ABmag, respectively. In size-mass parameter space, galaxies in COSMOS-DASH demonstrate robust morphological measurements out to z ∼2 and down to log(M∗/Mo˙)∼9 . With the advantage of the larger area of COSMOS-DASH, we measure a flattening of the quiescent size-mass relation below log(M∗/Mo˙)∼10.5 that persists out to z ∼2. We show that environment is not the primary driver of this flattening, at least out to z = 1.2, whereas internal physical processes may instead govern the structural evolution.
AB - We present the H 160 morphological catalogs for the COSMOS-DASH survey, the largest area near-IR survey using HST-WFC3 to date. Utilizing the "Drift And SHift"observing technique for HST-WFC3 imaging, the COSMOS-DASH survey imaged approximately 0.5 deg2 of the UltraVISTA deep stripes (0.7 deg2, when combined with archival data). Global structural parameters are measured for 51,586 galaxies within COSMOS-DASH using GALFIT (excluding the CANDELS area) with detection using a deep multi-band HST image. We recover consistent results with those from the deeper 3D-HST morphological catalogs, finding that, in general, sizes and Sérsic indices of typical galaxies are accurate to limiting magnitudes of H 160 < 23 and H 160 < 22 ABmag, respectively. In size-mass parameter space, galaxies in COSMOS-DASH demonstrate robust morphological measurements out to z ∼2 and down to log(M∗/Mo˙)∼9 . With the advantage of the larger area of COSMOS-DASH, we measure a flattening of the quiescent size-mass relation below log(M∗/Mo˙)∼10.5 that persists out to z ∼2. We show that environment is not the primary driver of this flattening, at least out to z = 1.2, whereas internal physical processes may instead govern the structural evolution.
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U2 - 10.3847/1538-4357/ac341c
DO - 10.3847/1538-4357/ac341c
M3 - Article
AN - SCOPUS:85125861148
SN - 0004-637X
VL - 925
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 34
ER -