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Hubble Space Telescope Morphologies of z ~ 2 Dust-obscured Galaxies. II. Bump Sources

Bussmann, R. S. and Dey, Arjun and Lotz, J. and Armus, L. and Brown, M. J. I. and Desai, V. and Eisenhardt, P. and Higdon, J. and Higdon, S. and Jannuzi, B. T. and Le Floc'h, E. and Melbourne, J. and Soifer, B. T. and Weedman, D. (2011) Hubble Space Telescope Morphologies of z ~ 2 Dust-obscured Galaxies. II. Bump Sources. Astrophysical Journal, 733 (1). Art. No. 21. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20110527-111102694

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Abstract

We present Hubble Space Telescope imaging of 22 ultra-luminous infrared galaxies (ULIRGs) at z ≈ 2 with extremely red R – [24] colors (called dust-obscured galaxies, or DOGs) which have a local maximum in their spectral energy distribution (SED) at rest-frame 1.6 μm associated with stellar emission. These sources, which we call "bump DOGs," have star formation rates (SFRs) of 400-4000 M_⊙ yr^(–1) and have redshifts derived from mid-IR spectra which show strong polycyclic aromatic hydrocarbon emission—a sign of vigorous ongoing star formation. Using a uniform morphological analysis, we look for quantifiable differences between bump DOGs, power-law DOGs (Spitzer-selected ULIRGs with mid-IR SEDs dominated by a power law and spectral features that are more typical of obscured active galactic nuclei than starbursts), submillimeter-selected galaxies, and other less-reddened ULIRGs from the Spitzer Extragalactic First Look Survey. Bump DOGs are larger than power-law DOGs (median Petrosian radius of 8.4 ± 2.7 kpc versus 5.5 ± 2.3 kpc) and exhibit more diffuse and irregular morphologies (median M _(20) of –1.08 ± 0.05 versus –1.48 ± 0.05). These trends are qualitatively consistent with expectations from simulations of major mergers in which merging systems during the peak SFR period evolve from M _(20) = –1.0 to M _(20) = –1.7. Less-obscured ULIRGs (i.e., non-DOGs) tend to have more regular, centrally peaked, single-object morphologies rather than diffuse and irregular morphologies. This distinction in morphologies may imply that less-obscured ULIRGs sample the merger near the end of the peak SFR period. Alternatively, it may indicate that the intense star formation in these less-obscured ULIRGs is not the result of a recent major merger.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/733/1/21DOIArticle
http://iopscience.iop.org/0004-637X/733/1/21PublisherArticle
ORCID:
AuthorORCID
Dey, Arjun0000-0002-4928-4003
Armus, L.0000-0003-3498-2973
Brown, M. J. I.0000-0002-1207-9137
Desai, V.0000-0002-1340-0543
Additional Information:© 2011 American Astronomical Society. Received 2010 June 25; accepted 2011 March 11; published 2011 April 29. The work is based primarily on observations made with the Hubble Space Telescope. This work also relies in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. We are grateful to the expert assistance of the staff Kitt Peak National Observatory where the Boötes field observations of the NDWFS were obtained. The authors thank NOAO for supporting the NOAO Deep Wide-Field Survey. In particular, we thank Jenna Claver, Lindsey Davis, Alyson Ford, Emma Hogan, Tod Lauer, Lissa Miller, Erin Ryan, Glenn Tiede, and Frank Valdes for their able assistance with the NDWFS data. We also thank the staff of the W. M. Keck Observatory, where some of the galaxy redshifts were obtained. We gratefully acknowledge the anonymous referee whose helpful suggestions have resulted in an improved manuscript. R.S.B. gratefully acknowledges financial assistance from HST grants GO10890 and GO11195, without which this research would not have been possible. Support for program numbers HST-GO10890 and HST-GO11195 were provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The research activities of A.D. and B.T.J. are supported by NOAO, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. Support for E. Le Floc’h was provided by NASA through the Spitzer Space Telescope Fellowship Program.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA1407
National Optical Astronomy Observatory (NOAO)UNSPECIFIED
NASAGO10890
NASAGO11195
NASAHST-GO10890
NASAHST-GO11195
NASANAS5-26555
NASA Spitzer FellowshipUNSPECIFIED
Subject Keywords:galaxies: evolution, galaxies: fundamental parameters, galaxies: high-redshift
Issue or Number:1
Classification Code:PACS: 98.54.Ep; 98.65.Fz; 98.62.Ai; 95.30.Ky; 98.62.Qz; 98.62.Py
Record Number:CaltechAUTHORS:20110527-111102694
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20110527-111102694
Official Citation:Hubble Space Telescope Morphologies of z ~ 2 Dust-obscured Galaxies. II. Bump Sources R. S. Bussmann, Arjun Dey, J. Lotz, L. Armus, M. J. I. Brown, V. Desai, P. Eisenhardt, J. Higdon, S. Higdon, B. T. Jannuzi, E. Le Floc'h, J. Melbourne, B. T. Soifer and D. Weedman doi: 10.1088/0004-637X/733/1/21
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:23823
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:27 May 2011 20:15
Last Modified:03 Oct 2019 02:50

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