Imaging Polarization of the Blue-excess Hot Dust-obscured Galaxy WISE J011601.41–050504.0

Assef, R. J.; Bauer, F. E.; Blain, A. W.; Brightman, M.; Díaz-Santos, T.; Eisenhardt, P. M.; Jun, H. D.; Stern, D.; Tsai, C. -W.; Walton, D. J.; Wu, J. W.

doi:10.3847/1538-4357/ac77fc

Imaging Polarization of the Blue-excess Hot Dust-obscured Galaxy WISE J011601.41–050504.0

Journal Article · Thu Jul 28 00:00:00 EDT 2022 · The Astrophysical Journal

DOI:https://doi.org/10.3847/1538-4357/ac77fc· OSTI ID:1983284

^[1]; ^[2]; ^[3]; ^[4]; ^[5]; Eisenhardt, P. M. ^[4]; ^[6]; ^[4]; ^[7]; ^[8]; ^[9]

Universidad Diego Portales, Santiago (Chile)
Pontificia Universidad Católica de Chile, Santiago (Chile); Millennium Institute of Astrophysics (MAS), Santiago (Chile); Space Science Institute, Boulder, CO (United States)
University of Leicester (United Kingdom)
California Institute of Technology (CalTech), Pasadena, CA (United States)
Foundation for Research and Technology–Hellas (FORTH), Heraklion (Greece); European University Cyprus, Nicosia (Cyprus)
Seoul National University (Korea, Republic of)
Chinese Academy of Sciences, Beijing (China)
University of Hertfordshire (United Kingdom)
Chinese Academy of Sciences, Beijing (China); University of Chinese Academy of Sciences, Beijing (China)

We report on VLT/FORS2 imaging polarimetry observations in the R_Special band of WISE J011601.41–050504.0 (W0116–0505), a heavily obscured hyperluminous quasar at z = 3.173 classified as a Hot Dust-obscured Galaxy (Hot DOG) based on its mid-IR colors. Recently, Assef et al. identified W0116–0505 as having excess rest-frame optical/UV emission and concluded that this excess emission is most likely scattered light from the heavily obscured AGN. We find that the broadband rest-frame UV flux is strongly linearly polarized (10.8% ± 1.9%, with a polarization angle of 74° ± 9°), confirming this conclusion. We analyze these observations in the context of a simple model based on scattering either by free electrons or by optically thin dust, assuming a classical dust torus with polar openings. Both can replicate the degree of polarization and the luminosity of the scattered component for a range of geometries and column densities, but we argue that optically thin dust in the ISM is the more likely scenario. We also explore the possibility that the scattering medium corresponds to an outflow recently identified for W0116–0505. This is a feasible option if the outflow component is biconical with most of the scattering occurring at the base of the receding outflow. In this scenario, the quasar would still be obscured even if viewed face-on but might appear as a reddened type 1 quasar once the outflow has expanded. We discuss a possible connection between blue-excess Hot DOGs, extremely red quasars, reddened type 1 quasars, and unreddened quasars that depends on a combination of evolution and viewing geometry.

View Accepted Manuscript (DOE)

Research Organization:: US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)

Sponsoring Organization:: USDOE

OSTI ID:: 1983284

Journal Information:: The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 2 Vol. 934; ISSN 0004-637X

Publisher:: IOP PublishingCopyright Statement

Country of Publication:: United States

Language:: English

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