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|Title:||The Role of Quenching Time in the Evolution of the Mass-size Relation of Passive Galaxies from the Wisp Survey||Authors:||ZANELLA, ANITA
Corsini, E. M.
Bedregal, A. G.
Dalla Bontà, E.
Bunker, A. J.
. Colbert, J.
Dai, Y. S.
Rutkowski, M. J.
|Issue Date:||2016||Journal:||THE ASTROPHYSICAL JOURNAL||Number:||824||Issue:||2||First Page:||68||Abstract:||We analyze how passive galaxies at z ∼ 1.5 populate the mass-size plane as a function of their stellar age, to understand if the observed size growth with time can be explained with the appearance of larger quenched galaxies at lower redshift. We use a sample of 32 passive galaxies extracted from the Wide Field Camera 3 Infrared Spectroscopic Parallel (WISP) survey with spectroscopic redshift 1.3 ≲ z ≲ 2.05, specific star formation rates lower than 0.01 Gyr<SUP>-1</SUP>, and stellar masses above 4.5 × 10<SUP>10</SUP> M <SUB>☉</SUB>. All galaxies have spectrally determined stellar ages from fitting of their rest-frame optical spectra and photometry with stellar population models. When dividing our sample into young (age ≤2.1 Gyr) and old (age >2.1 Gyr) galaxies we do not find a significant trend in the distributions of the difference between the observed radius and that predicted by the mass-size relation. This result indicates that the relation between the galaxy age and its distance from the mass-size relation, if it exists, is rather shallow, with a slope α ≳ -0.6. At face value, this finding suggests that multiple dry and/or wet minor mergers, rather than the appearance of newly quenched galaxies, are mainly responsible for the observed time evolution of the mass-size relation in passive galaxies. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555.||URI:||http://hdl.handle.net/20.500.12386/24593||URL:||https://iopscience.iop.org/article/10.3847/0004-637X/824/2/68||ISSN:||0004-637X||DOI:||10.3847/0004-637X/824/2/68||Bibcode ADS:||2016ApJ...824...68Z||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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