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Dust Emission in an Accretion-rate-limited Sample of z ≳ 6 Quasars

Venemans, Bram P. and Decarli, Roberto and Walter, Fabian and Bañados, Eduardo and Bertoldi, Frank and Fan, Xiaohui and Farina, Emanuele Paolo and Mazzucchelli, Chiara and Riechers, Dominik and Rix, Hans-Walter and Wang, Ran and Yang, Yujin (2018) Dust Emission in an Accretion-rate-limited Sample of z ≳ 6 Quasars. Astrophysical Journal, 866 (2). Art. No. 159. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20181024-140351642

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Abstract

We present Atacama Large Millimeter Array 1 mm observations of the rest-frame far-infrared (FIR) dust continuum in 27 quasars at redshifts 6.0 ≾ z < 6.7. We detect FIR emission at ≳3σ in all quasar host galaxies with flux densities at ~1900 GHz in the rest-frame of 0.12 < S_(rest,1900 GHz) < 5.9 mJy, with a median (mean) flux density of 0.88 mJy (1.59 mJy). The implied FIR luminosities range from L_(FIR) = (0.27–13) × 1012 L⊙, with 74% of our quasar hosts having L_(FIR) > 10^(12) L⊙. The estimated dust masses are M_(dust) = 10^7–10^9 M⊙. If the dust is heated only by star formation, then the star formation rates in the quasar host galaxies are between 50 and 2700 M⊙ yr^(-1). In the framework of the host galaxy–black hole coevolution model a correlation between ongoing black hole growth and star formation in the quasar host galaxy would be expected. However, combined with results from the literature to create a luminosity-limited quasar sample, we do not find a strong correlation between quasar UV luminosity (a proxy for ongoing black hole growth) and FIR luminosity (star formation in the host galaxy). The absence of such a correlation in our data does not necessarily rule out the coevolution model, and could be due to a variety of effects (including different timescales for black hole accretion and FIR emission).


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aadf35DOIArticle
https://arxiv.org/abs/1809.01662arXivDiscussion Paper
ORCID:
AuthorORCID
Venemans, Bram P.0000-0001-9024-8322
Decarli, Roberto0000-0002-2662-8803
Walter, Fabian0000-0003-4793-7880
Bañados, Eduardo0000-0002-2931-7824
Bertoldi, Frank0000-0002-1707-1775
Fan, Xiaohui0000-0003-3310-0131
Farina, Emanuele Paolo0000-0002-6822-2254
Mazzucchelli, Chiara0000-0002-5941-5214
Riechers, Dominik0000-0001-9585-1462
Rix, Hans-Walter0000-0003-4996-9069
Yang, Yujin0000-0003-3078-2763
Additional Information:© 2018 The American Astronomical Society. Received 2018 June 15; revised 2018 August 27; accepted 2018 September 2; published 2018 October 24. We thank the referee for providing valuable comments and suggestions. B.P.V., F.W., and E.P.F. acknowledge funding through the ERC grants "Cosmic Dawn" and "Cosmic Gas." Part of the support for R.D. was provided by the DFG priority program 1573 "The physics of the interstellar medium." D.R. acknowledges support from the National Science Foundation under grant number AST-1614213. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.01115.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.
Funders:
Funding AgencyGrant Number
European Research Council (ERC)Cosmic Dawn
European Research Council (ERC)Cosmic Gas
Deutsche Forschungsgemeinschaft (DFG)1573
NSFAST-1614213
Subject Keywords:galaxies: high-redshift – galaxies: star formation – galaxies: statistics – quasars: general
Record Number:CaltechAUTHORS:20181024-140351642
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20181024-140351642
Official Citation:Bram P. Venemans et al 2018 ApJ 866 159
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:90400
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:25 Oct 2018 17:06
Last Modified:25 Oct 2018 17:06

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