The quasar relation through cosmic time - II. Evidence for evolution from<i>z = 3</i>to the present age

Decarli, Roberto; Falomo, R.; Treves, A.; Labita, M.; Kotilainen, J. K.; Scarpa, Riccardo

doi:10.1111/j.1365-2966.2009.16049.x

Cited by 172 publications

(235 citation statements)

References 81 publications

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“…There have been many studies focus on the evolution of the scaling relation. For instance, Decarli et al (2010) studied a sample of 96 quasars with redshift up to 3 and found that the M BH /M host,* ratio increases by a factor of seven from z = 0 to z = 3. Merloni et al (2010) used 89 broad-line AGNs detected in the zCOSMOS survey in the redshift range 1 < z < 2.2 and found that the average black hole to host galaxy mass ratio evolves positively with redshift.…”

Section: Discussionmentioning

confidence: 99%

Herschel Observed Stripe 82 Quasars and Their Host Galaxies: Connections Between Agn Activity and Host Galaxy Star Formation

2016

ApJ

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In this work, we present a study of 207 quasars selected from the Sloan Digital Sky Survey quasar catalogs and the Herschel Stripe 82 survey. Quasars within this sample are high-luminosity quasars with a mean bolometric luminosity of 10 46.4 erg s −1 . The redshift range of this sample is within z < 4, with a mean value of 1.5 ± 0.78. Because we only selected quasars that have been detected in all three Herschel-SPIRE bands, the quasar sample is complete yet highly biased. Based on the multi-wavelength photometric observation data, we conducted a spectral energy distribution (SED) fitting through UV to FIR. Parameters such as active galactic nucleus (AGN) luminosity, far-IR (FIR) luminosity, stellar mass, as well as many other AGN and galaxy properties are deduced from the SED fitting results. The mean star formation rate (SFR) of the sample is 419 M e yr −1 and the mean gas mass is ∼10 11.3 M e . All of these results point to an IR luminous quasar system. Compared with star formation main sequence (MS) galaxies, at least 80 out of 207 quasars are hosted by starburst galaxies. This supports the statement that luminous AGNs are more likely to be associated with major mergers. The SFR increases with the redshift up to z = 2. It is correlated with the AGN bolometric luminosity, where µ  L L FIR Bol 0.46 0.03 . The AGN bolometric luminosity is also correlated with the host galaxy mass and gas mass. Yet the correlation between L FIR and L Bol has higher significant level, implies that the link between AGN accretion and the SFR is more primal. The M BH /M * ratio of our sample is 0.02, higher than the value 0.005 in the local universe. It might indicate an evolutionary trend of the M BH -M * scaling relation.

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Section: Discussionmentioning

confidence: 99%

Herschel Observed Stripe 82 Quasars and Their Host Galaxies: Connections Between Agn Activity and Host Galaxy Star Formation

2016

ApJ

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“…We further assumed that the Mstellar -Mbh relationship does not evolve with cosmic time, which may or may not be the case (e.g. Decarli et al 2010) as selection effects and biases makes this relationship difficult to probe as redshift increases. However, such an evolution, if it exists, appears to be similar in strength to the scatter in the mass relationships at a given time.…”

Section: Dark Matter Halo Galaxy and Black Hole Growthmentioning

confidence: 99%

“…Peng et al 2006;Alexander et al 2008;Woo et al 2008;Decarli et al 2010;Kormendy & Ho 2013). To generate a starting point, we simply begin each BH at a random fraction (from 0.1 to 0.9) of its expected value (Figure 1).…”

Section: Dark Matter Halo Galaxy and Black Hole Growthmentioning

confidence: 99%

“…Hickox et al (2011), DiPompeo et al (2014b, and D16a attempted to explain the larger obscured halo masses with an evolutionary picture in which black hole growth lags behind dark matter halo growth (e.g. Peng et al 2006;Alexander et al 2008;Woo et al 2008;Decarli et al 2010;Kormendy & Ho 2013) and the obscured phase precedes the unobscured phase (e.g. Hopkins et al 2006;Booth & Schaye 2009), with the unobscured and obscured phases lasting roughly the same length of time (each on the order of 100 Myr, or 1% of the Hubble time).…”

Section: Introductionmentioning

confidence: 99%

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A unifying evolutionary framework for infrared-selected obscured and unobscured quasar host haloes

DiPompeo

Hickox

Myers

2016

Mon. Not. R. Astron. Soc.

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Recent measurements of the dark matter halo masses of infrared-selected obscured quasars are in tension -some indicate that obscured quasars have higher halo mass compared to their unobscured counterparts, while others find no difference. The former result is inconsistent with the simplest models of quasar unification that rely solely on viewing angle, while the latter may support such models. Here, using empirical relationships between dark matter halo and supermassive black hole masses, we provide a simple evolutionary picture that naturally explains these findings and is motivated by more sophisticated merger-driven quasar fueling models. The model tracks the growth rate of haloes, with the black hole growing in spurts of quasar activity in order to "catch-up" with the M bh -M stellar -M halo relationship. The first part of the quasar phase is obscured and is followed by an unobscured phase. Depending on the luminosity limit of the sample, driven by observational selection effects, a difference in halo masses may or may not be significant. For high luminosity samples, the difference can be large (a few to 10 times higher masses in obscured quasars), while for lower luminosity samples the halo mass difference is very small, much smaller than current observational constraints. Such a simple model provides a qualitative explanation for the higher mass haloes of obscured quasars, as well as rough quantitative agreement with seemingly disparate results.

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“…For a limited number of QSOs the use of 8-10m telescope under superb seeing conditions or with adaptive optics imaging has allowed the study of quasar host at high redshift (Kotilainen et al , 2009) and/or with adaptive optics These observations allowed to trace a a first view of the cosmic co-evolution of SMBH and their host galaxies (see e.g. Decarli et al 2010Decarli et al , 2012Sanghvi et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Low-redshift quasars in the SDSS Stripe 82. Host galaxy colours and close environment

Bettoni

Falomo

Kotilainen

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a photometrical and morphological multicolor study of the properties of low redshift (z<0.3) quasar hosts based on a large and homogeneous dataset of quasars derived from the Sloan Digital Sky Survey (DR7). We used quasars that were imaged in the SDSS Stripe82 that is up to 2 mag deeper than standard Sloan images. This sample is part of a larger dataset of ∼400 quasars at z < 0.5 for which both the host galaxies and their galaxy environments were studied Karhunen et al. 2014). For 52 quasars we undertake a study of the color of the host galaxies and of their close environments in u, g, r, i and z bands. We are able to resolve almost all the quasars in the sample in the filters g, r, i and z and also in u for about 50% of the targets. We found that the mean colors of the QSO host galaxy (g − i=0.82±0.26; r − i=0.26±0.16 and u − g=1.32±0.25) are very similar to the values of a sample of inactive galaxies matched in terms of redshift and galaxy luminosity with the quasar sample. There is a suggestion that the most massive QSO hosts have bluer colors. Both quasar hosts and the comparison sample of inactive galaxies have candidates of close (< 50 kpc) companion galaxies for ∼ 30% of the sources with no significant difference between active and inactive galaxies. We do not find significant correlation between the central black hole (BH) mass and the quasar host luminosity that appears to be extra luminous at a given BH mass with respect to the local relation (M BH -M host ) for inactive galaxies. This confirms previous suggestion that a substantial disc component, not correlated to the BH mass, is present in the galaxies hosting low z quasars. These results support a scenario where the activation of the nucleus has negligible effects on the global structural and photometrical properties of the hosting galaxies.

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The quasar relation through cosmic time - II. Evidence for evolution fromz = 3to the present age

Cited by 172 publications

References 81 publications

Herschel Observed Stripe 82 Quasars and Their Host Galaxies: Connections Between Agn Activity and Host Galaxy Star Formation

Herschel Observed Stripe 82 Quasars and Their Host Galaxies: Connections Between Agn Activity and Host Galaxy Star Formation

A unifying evolutionary framework for infrared-selected obscured and unobscured quasar host haloes

Low-redshift quasars in the SDSS Stripe 82. Host galaxy colours and close environment

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