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Hot Dust-Obscured Galaxies with Excess Blue Light

Assef, R. J. and Brightman, M. and Walton, D. J. and Stern, D. and Bauer, F. E. and Blain, A. W. and Díaz-Santos, T. and Eisenhardt, P. R. M. and Hickox, R. C. and Jun, H. D. and Psychogyios, A. and Tsai, C.-W. and Wu, J. W. (2019) Hot Dust-Obscured Galaxies with Excess Blue Light. . (Unpublished) https://resolver.caltech.edu/CaltechAUTHORS:20190809-153952098

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Abstract

Hot Dust-Obscured Galaxies (Hot DOGs) are among the most luminous galaxies in the Universe. Powered by highly obscured, possibly Compton-thick, active galactic nuclei (AGNs), Hot DOGs are characterized by SEDs that are very red in the mid-IR yet dominated by the host galaxy stellar emission in the UV and optical. An earlier study identified a sub-sample of Hot DOGs with significantly enhanced UV emission. One target, W0204-0506, was studied in detail and, based on Chandra observations, it was concluded that the enhanced emission was most likely due to either extreme unobscured star-formation (SFR > 1000 M⊙ yr^(−1)) or to light from the highly obscured AGN scattered by gas or dust into our line of sight. Here, we present a follow-up study of W0204-0506 as well as two more Hot DOGs with excess UV emission. For the two new objects we obtained Chandra/ACIS-S observations, and for all three targets we obtained HST/WFC3 F555W and F160W imaging. We conclude that the excess UV emission is primarily dominated by light from the central highly obscured, hyper-luminous AGN that has been scattered into our line of sight. We cannot rule out, however, that star-formation may significantly contribute to the UV excess of W0204-0506.


Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1905.04320arXivDiscussion Paper
ORCID:
AuthorORCID
Assef, R. J.0000-0002-9508-3667
Brightman, M.0000-0002-8147-2602
Walton, D. J.0000-0001-5819-3552
Stern, D.0000-0003-2686-9241
Bauer, F. E.0000-0002-8686-8737
Blain, A. W.0000-0001-7489-5167
Díaz-Santos, T.0000-0003-0699-6083
Hickox, R. C.0000-0003-1468-9526
Jun, H. D.0000-0003-1470-5901
Tsai, C.-W.0000-0002-9390-9672
Additional Information:We thank J. Comerford and B. Weiner for carrying out observations presented in this article. RJA was supported by FONDECYT grants number 1151408 and 1191124. DJW acknowledges financial support from STFC Ernest Rutherford fellowships. HDJ was supported by Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education (NRF-2017R1A6A3A04005158). FEB acknowledges support from CONICYT-Chile (Basal AFB-170002) and the Ministry of Economy, Development and Tourism’s Millenium Science Initiative through grant IC120009, awarded to The Millenium Institute of Astrophysics, MAS. JW is supported by the NSFC Grant 11690024 and SPRP CAS grant XDB23000000. Based on observations made with the NASA/ESA Hubble Space Telescope, 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 #14358. Support for program#14358 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The scientific results reported in this article are based to a significant degree on data obtained from the Chandra X-ray Observatory and observations made by the Chandra X-ray Observatory and published previously in cited articles. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number 17700696 issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE) and the Los Alamos National Laboratory. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Some of the observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona.
Funders:
Funding AgencyGrant Number
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1151408
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1191124
Science and Technology Facilities Council (STFC)UNSPECIFIED
National Research Foundation of KoreaNRF-2017R1A6A3A04005158
Basal-CATAAFB-170002
Iniciativa Científica Milenio del Ministerio de Economía, Fomento y TurismoIC120009
National Natural Science Foundation of China11690024
Chinese Academy of SciencesXDB23000000
NASANAS 5-26555
NASA17700696
NASANAS8-03060
NASA/JPL/CaltechUNSPECIFIED
NASANNX08AR22G
NSFAST-1238877
Alfred P. Sloan FoundationUNSPECIFIED
Participating InstitutionsUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
Subject Keywords:galaxies: active — galaxies: evolution — galaxies: high-redshift — quasars: general — infrared: galaxies
Record Number:CaltechAUTHORS:20190809-153952098
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190809-153952098
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:97735
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:09 Aug 2019 22:55
Last Modified:05 Nov 2019 00:18

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