Star formation rates in luminous quasars at 2 <z< 3

Harris, Kathryn, Farrah, Duncan, Schulz, Bernhard, Hatziminaoglou, Evanthia, Viero, Marco, Anderson, Nick, Béthermin, Matthieu, Chapman, Scott, Clements, David L, Cooray, Asantha, Efstathiou, Andreas, Feltre, Anne, Hurley, Peter, Ibar, Eduardo, Lacy, Mark, Oliver, Sebastian, Page, Mathew J, Pérez-Fournon, Ismael, Petty, Sara M., Pitchford, Lura K, Rigopoulou, Dimitra, Scott, Douglas, Symeonidis, Myrto, Vieira, Joaquin and Wang, Lingyu (2016) Star formation rates in luminous quasars at 2 <z< 3. Monthly Notices of the Royal Astronomical Society, 457 (4). pp. 4179-4194. ISSN 0035-8711

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Abstract

We investigate the relation between star formation rates (M ˙ s M˙s ) and AGN properties in optically selected type 1 quasars at 2 < z < 3 using data from Herschel and the SDSS. We find that M ˙ s M˙s remains approximately constant with redshift, at 300 ± 100 M⊙ yr−1. Conversely, M ˙ s M˙s increases with AGN luminosity, up to a maximum of ∼ 600 M⊙ yr−1, and with C IV FWHM. In context with previous results, this is consistent with a relation between M ˙ s M˙s and black hole accretion rate (M ˙ bh M˙bh ) existing in only parts of the z−M ˙ s −M ˙ bh z−M˙s−M˙bh plane, dependent on the free gas fraction, the trigger for activity, and the processes that may quench star formation. The relations between M ˙ s M˙s and both AGN luminosity and C IV FWHM are consistent with star formation rates in quasars scaling with black hole mass, though we cannot rule out a separate relation with black hole accretion rate. Star formation rates are observed to decline with increasing C IV equivalent width. This decline can be partially explained via the Baldwin effect, but may have an additional contribution from one or more of three factors; Mi is not a linear tracer of L2500, the Baldwin effect changes form at high AGN luminosities, and high C IV EW values signpost a change in the relation between M ˙ s M˙s and M ˙ bh M˙bh . Finally, there is no strong relation between M ˙ s M˙s and Eddington ratio, or the asymmetry of the C IV line. The former suggests that star formation rates do not scale with how efficiently the black hole is accreting, while the latter is consistent with C IV asymmetries arising from orientation effects.

Item Type: Article
Keywords: galaxies: evolution – quasars: general – galaxies: starburst – galaxies: star formation – infrared: galaxies.
Schools and Departments: School of Mathematical and Physical Sciences > Physics and Astronomy
Subjects: Q Science > QB Astronomy
Depositing User: Richard Chambers
Date Deposited: 20 May 2016 07:05
Last Modified: 15 Mar 2017 23:21
URI: http://sro.sussex.ac.uk/id/eprint/61093

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