COSMIC EVOLUTION OF STAR FORMATION IN TYPE-1 QUASAR HOSTS SINCE<i>z</i>= 1

Shi, Yong; Rieke, G. H.; Ogle, Patrick; Jiang, Linhua; Diamond‐Stanic, Aleksandar M.

doi:10.1088/0004-637x/703/1/1107

Cited by 47 publications

(60 citation statements)

References 122 publications

(268 reference statements)

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“…We can see that our sample has L IR comparable to those of the other SMG samples (Pope et al 2008;Menéndez-Delmestre et al 2009), and the PAH-rich sources from Sajina et al (2007). The star-forming galaxies of Shi et al (2009) …”

Section: The Correlation Between Ir and Pah Luminositiessupporting

confidence: 62%

“…Remarkably, it has been verified among local starburst galaxies over two orders of magnitude in L IR , from 10 10 to 10 12 L , by Brandl et al (2006). The approximate proportionality between L 7.7 μm and L IR has been extended through the ULIRG range up to 10 13 L and z ≥ 2 by several studies (Shi et al 2009;Pope et al 2008;Menéndez-Delmestre et al 2009). Our sample gives us an opportunity to check how tight the relation is among the strongest starbursts at z ∼ 2.…”

Section: The Correlation Between Ir and Pah Luminositiesmentioning

confidence: 79%

“…We have computed ν L ν (1.4 GHz) for our sample and those of Sajina et al (2007), Pope et al (2008), Shi et al (2009), andBrandl et al (2006). For our sample, we have used α as computed in F09 and reported in Table 1.…”

Section: The Correlation Between 14 Ghz and Pah Luminositiesmentioning

confidence: 99%

“…As expected, we observe a correlation between L 1.4 GHz and L 7.7 μm . Considering our sample, but also the local star-forming galaxy sample (Brandl et al 2006), the sample of SMGs (Pope et al 2008), the PAH-rich sources from Sajina et al (2007), and the intermediate-redshift starbursts (Shi et al 2009), we obtain the following relation ( Fig. 10): log (L 7.7 μm ) = (0.91±0.06) log (νL ν (1.4 GHz))+(4.60±0.36) (10) The effect of the positive k-correction and the value of α are particularly important for the determination of L 1.4 GHz and may significantly affect the reliability of the relation stated in Eq.…”

Section: The Correlation Between 14 Ghz and Pah Luminositiesmentioning

confidence: 99%

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Mid-infrared spectroscopy ofSpitzer-selected ultra-luminous starbursts atz ~ 2

Fiolet

Omont

Lagache

et al. 2010

A&A

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Context. Spitzer's wide-field surveys and followup capabilities have allowed a new breakthrough in mid-IR spectroscopy up to redshifts ≥2, especially for 24 μm detected sources. Aims. We want to study the mid-infrared properties and the starburst and AGN contributions, of 24 μm sources at z ∼ 2, through analysis of mid-infrared spectra combined with millimeter, radio, and infrared photometry. Mid-infrared spectroscopy allows us to recover accurate redshifts. Methods. A complete sample of 16 Spitzer-selected sources (ULIRGs) believed to be starbursts at z ∼ 2 ("5.8 μm-peakers") was selected in the (0.5 deg 2 ) J1064+56 SWIRE Lockman Hole field ("Lockman-North"). These sources have S 24 μm > 0.5 mJy, a stellar emission peak redshifted to 5.8 μm, and r Vega > 23. The entire sample was observed with the low resolution units of the Spitzer/IRS infrared spectrograph. These sources have 1.2 mm observations with IRAM 30 m/MAMBO and very deep 20 cm observations from the VLA. Nine of our sources also benefit from 350 μm observation and detection from CSO/SHARC-II. All these data were jointly analyzed.Results. The entire sample shows good quality IRS spectra dominated by strong PAH features. The main PAH features at 6.2, 7.7, 8.6, and 11.3 μm have high S /N average luminosities of 2.90 ± 0.31, 10.38 ± 1.09, 3.62 ± 0.27, and 2.29 ± 0.26 × 10 10 L , respectively. Thanks to their PAH spectra, we derived accurate redshifts spanning from 1.750 to 2.284. The average of these redshifts is 2.017 ± 0.038. This result confirms that the selection criteria of "5.8 μm-peakers" associated with a strong detection at 24 μm are reliable to select sources at z ∼ 2. We have analyzed the different correlations between PAH emission and infrared, millimeter, and radio emissions. Practically all our sources are strongly dominated by starburst emission, with only one source showing an important AGN contribution. We have also defined two subsamples based on the equivalent width at 7.7 μm to investigate AGN contributions. Conclusions. Our sample contains strong starbursts and represents a particularly 24 μm-bright class of SMGs. The very good correlation between PAH and far-IR luminosities is now confirmed in high-z starburst ULIRGs. These sources show a small AGN contribution to the mid-IR, around ∼20% or less in most cases.

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Section: The Correlation Between Ir and Pah Luminositiessupporting

confidence: 62%

Section: The Correlation Between Ir and Pah Luminositiesmentioning

confidence: 79%

Section: The Correlation Between 14 Ghz and Pah Luminositiesmentioning

confidence: 99%

Section: The Correlation Between 14 Ghz and Pah Luminositiesmentioning

confidence: 99%

See 2 more Smart Citations

Mid-infrared spectroscopy ofSpitzer-selected ultra-luminous starbursts atz ~ 2

Fiolet

Omont

Lagache

et al. 2010

A&A

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“…However, a close correspondence between QSOs and recent starburst events is predicted even in co-evolutionary models that do not explicitly rely on major galaxy mergers to fuel QSOs (e.g., Ciotti & Ostriker 2007). Star formation (SF) in QSO host galaxies has been extensively studied using high-resolution imaging in the optical (e.g., Bahcall et al 1997;Dunlop et al 2003;Jahnke et al 2004) and near-infared (e.g., Kukula et al 2001;Guyon et al 2006;Veilleux et al 2009); emission line tracers such as the [O II] line (Hes et al 1993;Ho 2005;Silverman et al 2009;Kalfountzou et al 2012); mid-infrared emission lines and PAH features (Netzer et al 2007;Lutz et al 2008;Shi et al 2009); and farinfrared (FIR) and sub-mm photometry (e.g., Priddey et al 2003;Omont et al 2003;Lutz et al 2010;Serjeant & Hatziminaoglou 2009;Serjeant et al 2010;Bonfield et al 2011). In general, QSO hosts are in massive, spheroidally-dominated galaxies, which frequently show signs of on-going star-formation (e.g., Jahnke et al 2004;Trump et al 2013), though signatures of early stage mergers or strong disturbances are not particularly frequent (Dunlop et al 2003;Guyon et al 2006;Bennert et al 2008;Veilleux et al 2009).…”

Section: Introductionmentioning

confidence: 99%

The mean star-forming properties of QSO host galaxies

Rosario

Trakhtenbrot

Lutz

et al. 2013

A&A

128

112

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Quasi-stellar objects (QSOs) occur in galaxies in which supermassive black holes (SMBHs) are growing substantially through rapid accretion of gas. Many popular models of the co-evolutionary growth of galaxies and black holes predict that QSOs are also sites of substantial recent star formation (SF), mediated by important processes, such as major mergers, which rapidly transform the nature of galaxies. A detailed study of the star-forming properties of QSOs is a critical test of these models. We present a far-infrared Herschel/PACS study of the mean star formation rate (SFR) of a sample of spectroscopically observed QSOs to z ∼ 2 from the COSMOS extragalactic survey. This is the largest sample to date of moderately luminous QSOs (with nuclear luminosities that lie around the knee of the luminosity function) studied using uniform, deep far-infrared photometry. We study trends of the mean SFR with redshift, black hole mass, nuclear bolometric luminosity, and specific accretion rate (Eddington ratio). To minimize systematics, we have undertaken a uniform determination of SMBH properties, as well as an analysis of important selection effects of spectroscopic QSO samples that influence the interpretation of SFR trends. We find that the mean SFRs of these QSOs are consistent with those of normal massive star-forming galaxies with a fixed scaling between SMBH and galaxy mass at all redshifts. No strong enhancement in SFR is found even among the most rapidly accreting systems, at odds with several co-evolutionary models. Finally, we consider the qualitative effects on mean SFR trends from different assumptions about the SF properties of QSO hosts and from redshift evolution of the SMBH-galaxy relationship. While currently limited by uncertainties, valuable constraints on AGN-galaxy co-evolution can emerge from our approach.

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What drives the growth of black holes?

Alexander

Hickox

2012

New Astronomy Reviews

595

501

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Massive black holes (BHs) are at once exotic and yet ubiquitous, residing in the centers of massive galaxies in the local Universe. Recent years have seen remarkable advances in our understanding of how these BHs form and grow over cosmic time, during which they are revealed as active galactic nuclei (AGN). However, despite decades of research, we still lack a coherent picture of the physical drivers of BH growth, the connection between the growth of BHs and their host galaxies, the role of large-scale environment on the fueling of BHs, and the impact of BH-driven outflows on the growth of galaxies. In this paper we review our progress in addressing these key issues, motivated by the science presented at the "What Drives the Growth of Black Holes?" workshop held at Durham on 26 th -29 th July 2010, and discuss how these questions may be tackled with current and future facilities.

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COSMIC EVOLUTION OF STAR FORMATION IN TYPE-1 QUASAR HOSTS SINCEz= 1

Cited by 47 publications

References 122 publications

Mid-infrared spectroscopy ofSpitzer-selected ultra-luminous starbursts atz ~ 2

Mid-infrared spectroscopy ofSpitzer-selected ultra-luminous starbursts atz ~ 2

The mean star-forming properties of QSO host galaxies

What drives the growth of black holes?

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