Spectral Decomposition of Broad-Line AGNs and Host Galaxies

Berk, D. E. vanden; Shen, Jiajian; Yip, Ching-Wa; Schneider, Donald P.; Connolly, Andrew J.; Burton, R. E.; Jester, Sebastian; Hall, Patrick B.; Szalay, Alexander S.; Brinkmann, J.

doi:10.1086/497973

Cited by 131 publications

(148 citation statements)

References 84 publications

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“…All of these predictions appear to be opposite the observations, with quasar spectra dominated by poststarburst activity (Vanden Berk et al 2006), typically early-type, bulge-dominated hosts (especially in the brightest quasars; Dunlop et al 2003;Floyd et al 2004), and observed starbursts usually showing high accretion rate BHs, which are at that moment undermassive relative to their hosts (e.g., Borys et al 2005). Moreover, if star formation is ongoing in these objects to grow their bulges, it implies a lower mass-to-light ratio and suggests that the discrepancy between their M BH -host relations is even larger than that in Figure 2, amplifying these difficulties.…”

Section: Discussionmentioning

confidence: 60%

An Upper Limit to the Degree of Evolution between Supermassive Black Holes and Their Host Galaxies

Hopkins

Robertson

Krause

et al. 2006

ApJ

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We describe a model-independent integral constraint that defines an upper limit to the allowed degree of evolution in the ratio of black hole (BH) mass to host galaxy luminosity or mass, as a function of redshift. Essentially, if the BH/host ratio is excessive at redshift z, then it would imply that the total mass density in BHs above some M min BH is larger at that redshift than at z ¼ 0, which is impossible. This argument requires no knowledge of host or BH properties, only a lower limit to the observed luminosity density in the brightest galaxies at some z. We calculate this upper limit from a variety of luminosity and mass functions in different bands from redshifts z ¼ 0Y2. We show that it is consistent with passive evolution of spheroid populations (with a fixed M BH /M host relation) in all cases, and provides tighter constraints than have generally been obtained previously, ruling out at k6 observational and theoretical estimates suggesting that M BH /M host was significantly larger at high redshifts than locally. We discuss a variety of possible ''loopholes'' or changes in the BH/host populations and correlations, and show that they typically lower the upper limits and strengthen our conclusions.

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Section: Discussionmentioning

confidence: 60%

An Upper Limit to the Degree of Evolution between Supermassive Black Holes and Their Host Galaxies

Hopkins

Robertson

Krause

et al. 2006

ApJ

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“…Lacking the data to measure the host galaxies of our sources, we must estimate their contribution. Such estimates of the contribution of host galaxy light to the SEDs can be made by applying simple scaling relationships among host bulge luminosity, bulge mass, black hole mass, and Eddington luminosity (e.g., Dunlop et al 2003;Vanden Berk et al 2006). The well-known correlation between central black hole mass and both bulge mass and luminosity (e.g., Ferrarese 2002) implies that quasars accreting at near their Eddington limits must have host bulge masses, and therefore luminosities, large enough to harbor the inferred black hole.…”

Section: Mean Sedsmentioning

confidence: 99%

“…The well-known correlation between central black hole mass and both bulge mass and luminosity (e.g., Ferrarese 2002) implies that quasars accreting at near their Eddington limits must have host bulge masses, and therefore luminosities, large enough to harbor the inferred black hole. We have used the quasar luminosity versus host luminosity relationship at optical frequencies, described by Vanden Berk et al (2006), to estimate the relative host galaxy contribution, assuming that the quasars are emitting at their Eddington limits.…”

Section: Mean Sedsmentioning

confidence: 99%

Spectral Energy Distributions and Multiwavelength Selection of Type 1 Quasars

Richards

Lacy

Storrie-Lombardi

et al. 2006

ASTROPHYS J SUPPL S

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1,120

1,194

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We present an analysis of the mid-infrared (MIR) and optical properties of type 1 (broad-line) quasars detected by the Spitzer Space Telescope. The MIR color-redshift relation is characterized to z $ 3, with predictions to z ¼ 7. We demonstrate how combining MIR and optical colors can yield even more efficient selection of active galactic nuclei (AGNs) than MIR or optical colors alone. Composite spectral energy distributions (SEDs) are constructed for 259 quasars with both Sloan Digital Sky Survey and Spitzer photometry, supplemented by near-IR, GALEX, VLA, and ROSAT data, where available. We discuss how the spectral diversity of quasars influences the determination of bolometric luminosities and accretion rates; assuming the mean SED can lead to errors as large as 50% for individual quasars when inferring a bolometric luminosity from an optical luminosity. Finally, we show that careful consideration of the shape of the mean quasar SED and its redshift dependence leads to a lower estimate of the fraction of reddened /obscured AGNs missed by optical surveys as compared to estimates derived from a single mean MIR to optical flux ratio.

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“…Studies of stellar populations through broadband SEDs and optical spectra have discovered intermediate-age stars or bluer colors in AGN hosts compared to their inactive galaxy counterparts at both low redshift (Ronnback et al 1996;Brotherton et al 1999;Kauffmann et al 2003a;Jahnke & Wisotzki 2003;Jahnke et al 2004;Canalizo et al 2006;Vanden Berk et al 2006;Jahnke et al 2007;Schawinski et al 2009) and high redshift (Ammons et al 2009). In the following, we show that the spectral features employed by current studies of stellar populations are not sensitive to ongoing (<0.1 Gyr) starburst activity.…”

Section: Comparisons With the Study Of Stellar Populationsmentioning

confidence: 99%

“…More importantly, obscuration can hide blue host-galaxy light if star formation occurs in the circumnuclear region as discussed above. Therefore, results based on spectra extending shorter than < 4000 Å may still underestimate significantly the level of ongoing star formation activity (Jahnke et al 2007;Vanden Berk et al 2006;Chen et al 2009). Kauffmann et al (2003a) employed the 4000 Å break and Hδ absorption to study stellar populations and found intermediateage stars in hosts with early-type morphologies.…”

Section: Comparisons With the Study Of Stellar Populationsmentioning

confidence: 99%

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

Shi

Rieke

Ogle

et al. 2009

ApJ

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We present Spitzer Infrared Spectrograph observations of a complete sample of 57 Sloan Digital Sky Survey type-1 quasars at z ∼ 1. Aromatic features at 6.2 and/or 7.7 μm are detected in about half of the sample and show profiles similar to those seen in normal galaxies at both low and high redshift, indicating a star formation origin for the features. Based on the ratio of aromatic to star formation infrared (SFIR) luminosities for normal star-forming galaxies at z ∼ 1, we have constructed the SFIR luminosity function (LF) of z ∼ 1 quasars. As we found earlier for low-redshift Palomar-Green (PG) quasars, these z ∼ 1 quasars show a flatter SFIR LF than do z ∼ 1 field galaxies, implying the quasar host galaxy population has on average a higher star formation rate (SFR) than the field galaxies do. As measured from their SFIR LF, individual quasar hosts have on average LIRG-level SFRs, which mainly arise in the circumnuclear regions. By comparing with similar measurements of low-redshift PG quasars, we find that the comoving SFIR luminosity density in quasar hosts shows a much larger increase with redshift than that in field galaxies. The behavior is consistent with pure density evolution since the average SFR and the average SFR/BH accretion rate in quasar hosts show little evolution with redshift. For individual quasars, we have found a correlation between the aromatic-based SFR and the luminosity of the nuclear radiation, consistent with predictions of some theoretical models. We propose that type-1 quasars reside in a distinct galaxy population that shows elliptical morphology but that harbors a significant fraction of intermediate-age stars and is experiencing intense circumnuclear star formation.

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Spectral Decomposition of Broad-Line AGNs and Host Galaxies

Cited by 131 publications

References 84 publications

An Upper Limit to the Degree of Evolution between Supermassive Black Holes and Their Host Galaxies

An Upper Limit to the Degree of Evolution between Supermassive Black Holes and Their Host Galaxies

Spectral Energy Distributions and Multiwavelength Selection of Type 1 Quasars

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

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