Star formation rates in luminous quasars at 2
Autor:
Mat Page, Matthieu Béthermin, Kathryn Harris, Scott Chapman, Sara Petty, Lura K. Pitchford, Edo Ibar, Anne Feltre, Peter Hurley, Bernhard Schulz, S. J. Oliver, Nick Anderson, Duncan Farrah, Marco Viero, Evanthia Hatziminaoglou, Mark Lacy, David L. Clements, M. Symeonidis, Ismael Perez-Fournon, Douglas Scott, Dimitra Rigopoulou, Lingyu Wang, Asantha Cooray, Joaquin Vieira, Andreas Efstathiou
Rok vydání:
2016
Předmět:
Physics
Active galactic nucleus
010308 nuclear & particles physics
Star formation
Astrophysics::High Energy Astrophysical Phenomena
Astronomy
Astronomy and Astrophysics
Context (language use)
Quasar
Astrophysics::Cosmology and Extragalactic Astrophysics
Astrophysics
01 natural sciences
Redshift
Luminosity
Black hole
Space and Planetary Science
0103 physical sciences
010303 astronomy & astrophysics
Equivalent width
Astrophysics::Galaxy Astrophysics
Zdroj:
Monthly Notices of the Royal Astronomical Society. 457:4179-4194
ISSN:
1365-2966
0035-8711
DOI:
10.1093/mnras/stw286
Popis:
We investigate the relation between star formation rates (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 remains approximately constant with redshift, at 300 ± 100 M⊙ yr^(−1). Conversely, 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 and black hole accretion rate (M_(bh)) existing in only parts of the 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 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; M_i is not a linear tracer of L_(2500), the Baldwin effect changes form at high AGN luminosities, and high C IV EW values signpost a change in the relation between M_s and M_(bh). Finally, there is no strong relation between 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.
Databáze:
OpenAIRE
Externí odkaz:
| Autor: | Mat Page, Matthieu Béthermin, Kathryn Harris, Scott Chapman, Sara Petty, Lura K. Pitchford, Edo Ibar, Anne Feltre, Peter Hurley, Bernhard Schulz, S. J. Oliver, Nick Anderson, Duncan Farrah, Marco Viero, Evanthia Hatziminaoglou, Mark Lacy, David L. Clements, M. Symeonidis, Ismael Perez-Fournon, Douglas Scott, Dimitra Rigopoulou, Lingyu Wang, Asantha Cooray, Joaquin Vieira, Andreas Efstathiou |
|---|---|
| Rok vydání: | 2016 |
| Předmět: |
Physics
Active galactic nucleus 010308 nuclear & particles physics Star formation Astrophysics::High Energy Astrophysical Phenomena Astronomy Astronomy and Astrophysics Context (language use) Quasar Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics 01 natural sciences Redshift Luminosity Black hole Space and Planetary Science 0103 physical sciences 010303 astronomy & astrophysics Equivalent width Astrophysics::Galaxy Astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 457:4179-4194 |
| ISSN: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/stw286 |
| Popis: | We investigate the relation between star formation rates (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 remains approximately constant with redshift, at 300 ± 100 M⊙ yr^(−1). Conversely, 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 and black hole accretion rate (M_(bh)) existing in only parts of the 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 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; M_i is not a linear tracer of L_(2500), the Baldwin effect changes form at high AGN luminosities, and high C IV EW values signpost a change in the relation between M_s and M_(bh). Finally, there is no strong relation between 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. |
| Databáze: | OpenAIRE |
| Externí odkaz: |
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