An Observational Determination of the Bolometric Quasar Luminosity Function

Hopkins, Philip F.; Richards, Gordon T.; Hernquist, Lars

doi:10.1086/509629

Cited by 1,092 publications

(2,048 citation statements)

References 176 publications

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“…Cimatti et al 2006; Thomas et al 2010). In addition to these, both the integrated cosmic star formation rate and the black hole accretion rate increase rapidly from z ∼ 0 out to z ∼ 2 (Dickinson et al 2003;Babić et al 2007;Hopkins et al 2007;Wilkins et al 2008;Rigby et al 2011). All these relationships indicate that the formation and growth of the black holes and their host galaxies are fundamentally intertwined.…”

Section: Introductionmentioning

confidence: 92%

Herschel-ATLAS: the connection between star formation and AGN activity in radio-loud and radio-quiet active galaxies

Gürkan¹,

Hardcastle²,

Jarvis³

et al. 2015

Mon. Not. R. Astron. Soc.

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We examine the relationship between star formation and AGN activity by constructing matched samples of local (0 < z < 0.6) radio-loud and radio-quiet AGN in the Herschel-ATLAS fields. Radio-loud AGN are classified as high-excitation and low-excitation radio galaxies (HERGs, LERGs) using their emission lines and WISE 22-µm luminosity. AGN accretion and jet powers in these active galaxies are traced by [OIII] emission-line and radio luminosity, respectively. Star formation rates (SFRs) and specific star formation rates (SSFRs) were derived using Herschel 250-µm luminosity and stellar mass measurements from the SDSS−MPA-JHU catalogue. In the past, star formation studies of AGN have mostly focused on high-redshift sources to observe the thermal dust emission that peaks in the far-infrared, which limited the samples to powerful objects. However, with Herschel we can expand this to low redshifts. Our stacking analyses show that SFRs and SSFRs of both radio-loud and radioquiet AGN increase with increasing AGN power but that radio-loud AGN tend to have lower SFR. Additionally, radio-quiet AGN are found to have approximately an order of magnitude higher SSFRs than radio-loud AGN for a given level of AGN power. The difference between the star formation properties of radio-loud and -quiet AGN is also seen in samples matched in stellar mass.

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Section: Introductionmentioning

confidence: 92%

Herschel-ATLAS: the connection between star formation and AGN activity in radio-loud and radio-quiet active galaxies

Gürkan¹,

Hardcastle²,

Jarvis³

et al. 2015

Mon. Not. R. Astron. Soc.

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“…Connolly et al, 1997;Merloni, 2004;Hopkins et al, 2007). The classic evolutionary sequence−merger, to starburst, quasar, then elliptical−is not only a phase of some growth for stellar populations, but also has been shown to account for ∼30% of the Universe's integrated black hole growth through highly obscured accretion (Treister et al, 2009(Treister et al, , 2010.…”

Section: Agn Contentmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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“…An SED for an AGN of this bolometric luminosity is then computed using the model of Hopkins, Richards & Hernquist (2007). From this SED, a broad-band luminosity is computed in each X-ray band assuming a spectrum of the form f ν ∝ν α with α = −0.4 as in the observational analysis.…”

Section: S U M M a Ry A N D C O N C L U S I O Nmentioning

confidence: 99%

The dark matter haloes of moderate luminosity X-ray AGN as determined from weak gravitational lensing and host stellar masses

Leauthaud

Benson

Civano

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Understanding the relationship between galaxies hosting active galactic nuclei (AGN) and the dark matter halos in which they reside is key to constraining how black-hole fueling is triggered and regulated. Previous efforts have relied on simple halo mass estimates inferred from clustering, weak gravitational lensing, or halo occupation distribution modeling. In practice, these approaches remain uncertain because AGN, no matter how they are identified, potentially live a wide range of halo masses with an occupation function whose general shape and normalization are poorly known. In this work, we show that better constraints can be achieved through a rigorous comparison of the clustering, lensing, and cross-correlation signals of AGN hosts to the fiducial stellar-to-halo mass relation (SHMR) derived for all galaxies, irrespective of nuclear activity. Our technique exploits the fact that the global SHMR can be measured with much higher accuracy than any statistic derived from AGN samples alone. Using 382 moderate luminosity X-ray AGN at z < 1 from the COSMOS field, we report the first measurements of weak gravitational lensing from an X-ray selected sample. Comparing this signal to predictions from the global SHMR, we find that, contrary to previous results, most X-ray AGN do not live in medium size groups -nearly half reside in relatively low mass halos with M 200b ∼ 10 12.5 M ⊙ . The AGN occupation function is well described by the same form derived for all galaxies but with a lower normalization-the fraction of halos with AGN in our sample is a few percent. The number of AGN satellite galaxies scales as a power law with host halo mass with a power-law index α = 1. By highlighting the relatively "normal" way in which moderate luminosity X-ray AGN hosts occupy halos, our results suggest that the environmental signature of distinct fueling modes for luminous QSOs compared to moderate luminosity X-ray AGN is less obvious than previously claimed.

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An Observational Determination of the Bolometric Quasar Luminosity Function

Cited by 1,092 publications

References 176 publications

Herschel-ATLAS: the connection between star formation and AGN activity in radio-loud and radio-quiet active galaxies

Herschel-ATLAS: the connection between star formation and AGN activity in radio-loud and radio-quiet active galaxies

Dusty star-forming galaxies at high redshift

The dark matter haloes of moderate luminosity X-ray AGN as determined from weak gravitational lensing and host stellar masses

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