CaltechAUTHORS
  A Caltech Library Service

Evolution of the Fraction of Clumpy Galaxies at 0.2 < z < 1.0 in the COSMOS Field

Murata, K. L. and Kajisawa, M. and Taniguchi, Y. and Kobayashi, M. A. R. and Shioya, Y. and Capak, P. and Ilbert, O. and Koekemoer, A. M. and Salvato, M. and Scoville, N. Z. (2014) Evolution of the Fraction of Clumpy Galaxies at 0.2 < z < 1.0 in the COSMOS Field. Astrophysical Journal, 786 (1). Art. No. 15. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20140616-111641778

[img]
Preview
PDF - Published Version
See Usage Policy.

5Mb
[img]
Preview
PDF - Submitted Version
See Usage Policy.

4Mb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20140616-111641778

Abstract

Using the Hubble Space Telescope/Advanced Camera for Surveys data in the COSMOS field, we systematically searched clumpy galaxies at 0.2 < z < 1.0 and investigated the fraction of clumpy galaxies and its evolution as a function of stellar mass, star formation rate (SFR), and specific SFR (SSFR). The fraction of clumpy galaxies in star-forming galaxies with M_(star) > 10^(9.5) M☉ decreases with time from ~0.35 at 0.8 < z < 1.0 to ~0.05 at 0.2 < z < 0.4, irrespective of the stellar mass, although the fraction tends to be slightly lower for massive galaxies with M_(star) > 10^(10.5) M☉ at each redshift. On the other hand, the fraction of clumpy galaxies increases with increasing both SFR and SSFR in all the redshift ranges we investigated. In particular, we found that the SSFR dependences of the fractions are similar among galaxies with different stellar masses, and the fraction at a given SSFR does not depend on the stellar mass in each redshift bin. The evolution of the fraction of clumpy galaxies from z ~ 0.9 to z ~ 0.3 seems to be explained by such SSFR dependence of the fraction and the evolution of SSFRs of star-forming galaxies. The fraction at a given SSFR also appears to decrease with time, but this can be due to the effect of the morphological k correction. We suggest that these results are understood by the gravitational fragmentation model for the formation of giant clumps in disk galaxies, where the gas mass fraction is a crucial parameter.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1403.1496arXivArticle
http://dx.doi.org/10.1088/0004-637X/786/1/15 DOIArticle
http://iopscience.iop.org/0004-637X/786/1/15/PublisherArticle
Additional Information:© 2014 The American Astronomical Society. Received 2013 December 12; accepted 2014 March 6; published 2014 April 10. 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. Also based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory under Large Program 175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation; and the Canada–France–Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the NRC and CADC of Canada, the CNRS of France, TERAPIX, and the University of Hawaii. We thank the anonymous referee for valuable comments and suggestions. We also thank Tsutomu T. Takeuchi at Nagoya University for his generous support to K.L.M. and for useful discussions. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We greatly acknowledge the contributions of the entire COSMOS collaboration, consisting of more than 70 scientists. This work was financially supported in part by the Japan Society for the Promotion of Science (Nos. 17253001, 19340046, 23244031, and 23740152).
Group:COSMOS
Funders:
Funding AgencyGrant Number
NASAHST-GO-09822
Japan Society for the Promotion of Science (JSPS)17253001
Japan Society for the Promotion of Science (JSPS)19340046
Japan Society for the Promotion of Science (JSPS)23244031
Japan Society for the Promotion of Science (JSPS)23740152
Subject Keywords:galaxies: evolution; galaxies: irregular; galaxies: star formation
Record Number:CaltechAUTHORS:20140616-111641778
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140616-111641778
Official Citation:Evolution of the Fraction of Clumpy Galaxies at 0.2 < z < 1.0 in the COSMOS Field K. L. Murata et al. 2014 ApJ 786 15
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:46279
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:16 Jun 2014 20:01
Last Modified:06 Jul 2015 17:30

Repository Staff Only: item control page