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THE ROLE of QUENCHING TIME in the EVOLUTION of the MASS-SIZE RELATION of PASSIVE GALAXIES from the WISP SURVEY

  • Author(s): Zanella, A
  • Scarlata, C
  • Corsini, EM
  • Bedregal, AG
  • Dalla Bontà, E
  • Atek, H
  • Bunker, AJ
  • Colbert, J
  • Dai, YS
  • Henry, A
  • Malkan, M
  • Martin, C
  • Rafelski, M
  • Rutkowski, MJ
  • Siana, B
  • Teplitz, H
  • et al.

Published Web Location

https://arxiv.org/abs/1604.00034
No data is associated with this publication.
Abstract

© 2016. The American Astronomical Society. All rights reserved. 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-1, and stellar masses above 4.5 × 1010 M Ȯ. 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.

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