The quasar relation through cosmic time - I. Data set and black hole masses

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

doi:10.1111/j.1365-2966.2009.16048.x

Cited by 35 publications

(48 citation statements)

References 63 publications

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“…BH mass estimates are computed from either the virial method (for broad-line sources; e.g., Woo et al 2008;Kim et al 2008;Decarli et al 2010b;Bennert et al 2010;Merloni et al 2010; see §4.1) or via some assumptions about the relationship between obscured and unobscured AGNs (as for SMGs; Alexander et al 2008a), each of which have significant uncertainty. The presence of an AGN also presents the additional challenge of separating the light from the host galaxy to that from the accreting BH, and difficulties in separating the mass or potential of the stellar bulge from the rest of the galaxy (e.g., Decarli et al, 2010a;Merloni et al, 2010).…”

Section: Correlations Between Bhs and Galaxy Spheroidsmentioning

confidence: 99%

What drives the growth of black holes?

Alexander

Hickox

2012

New Astronomy Reviews

581

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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Section: Correlations Between Bhs and Galaxy Spheroidsmentioning

confidence: 99%

What drives the growth of black holes?

Alexander

Hickox

2012

New Astronomy Reviews

581

501

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“…The difference can be attributed to the different continuum regions adopted by Vanden Berk et al (2001) We have also applied different continuum regions to gauge the dependence of the fit on the windows adopted. We considered the intervals listed by Decarli et al (2010) for a sample of 96 quasars at redshift lower than 3 with spectra collected from several instrument (e.g., SDSS, ESO/NTT, Nordic Optical Telescope, and HST). Specifically, the alternative windows adopted are 1351−1362, 1452−1480, 1680−1710, 1796−1834, 1970−2010, and 2188−2243Å.…”

Section: Spectral Fit and Emission Linesmentioning

confidence: 99%

The first ultraviolet quasar-stacked spectrum at z ≃ 2.4 from WFC3

Lusso

Worseck

Hennawi

et al. 2015

Monthly Notices of the Royal Astronomical Society

266

355

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The ionising continuum from active galactic nuclei (AGN) is fundamental for interpreting their broad emission lines and understanding their impact on the surrounding gas. Furthermore, it provides hints on how matter accretes onto supermassive black holes. Using HST's Wide Field Camera 3 we have constructed the first stacked ultraviolet (rest-frame wavelengths 600-2500Å) spectrum of 53 luminous quasars at z 2.4, with a state-of-the-art correction for the intervening Lyman forest and Lyman continuum absorption. The continuum slope (f ν ∝ ν αν ) of the full sample shows a break at ∼912Å with spectral index α ν = −0.61 ± 0.01 at λ > 912Å and a softening at shorter wavelengths (α ν = −1.70 ± 0.61 at λ 912Å). Our analysis proves that a proper intergalactic medium absorption correction is required to establish the intrinsic continuum emission of quasars. We interpret our average ultraviolet spectrum in the context of photoionisation, accretion disk models, and quasar contribution to the ultraviolet background. We find that observed broad line ratios are consistent with those predicted assuming an ionising slope of α ion =−2.0, similar to the observed ionising spectrum in the same wavelength range. The continuum break and softening are consistent with accretion disk plus X-ray corona models when black hole spin is taken into account. Our spectral energy distribution yields a 30% increase to previous estimates of the specific quasar emissivity, such that quasars may contribute significantly to the total specific Lyman limit emissivity estimated from the Lyα forest at z < 3.2.

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“…To determine the optimum selection criteria, we have taken the composite quasar spectrum from Decarli et al (2010), which consists of 96 bright quasars at 0 < z < 3. We chose this template because at red wavelengths it is less affected by host galaxy contamination than other composite spectra in the literature (e.g., Francis et al 1991;Vanden Berk et al 2001) and it samples the rest frame wavelengths of 5.7 < z < 7.2 quasars in the PS1 filters.…”

Section: Selection Of Quasar Candidatesmentioning

confidence: 99%

“…Left: the bottom panel shows the PS1 capture cross section in units of m 2 e −1 photon −1 for the i P1 , z P1 , and y P1 bands (Tonry et al 2012). The three upper panels show the composite quasar spectrum from Decarli et al (2010; with the intergalactic medium correction from Meiksin 2006) redshifted to z = 5.6, z = 6.0, and z = 6.3, from bottom to top. The gray dashed lines show the wavelength of the Lyα line at each redshift.…”

Section: Introductionmentioning

confidence: 99%

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The discovery of eight z ~ 6 quasars from Pan-STARRS1

Bañados¹,

Venemans²,

Morganson

et al. 2013

Proc. IAU

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High-redshift quasars are unique probes of the evolution of supermassive black holes and the intergalactic medium at the end of the epoch of reionization. We present the optical spectra of eight new z ~ 6 quasars selected from the Panoramic Survey Telescope & Rapid Response System 1 (Pan-STARRS1). Details of the selection strategy can be found in Bañados et al. (2014). With this work we increase the number of known quasars at z < 5.7 by more than 10%. The quasars discovered here span a large range of luminosities (19.6 ≤ zP1 ≤ 21.2) and are remarkably heterogeneous in their spectral features: half of them show bright emission lines whereas the other half show weak or no Lyα emission line. We find a larger fraction of weak–line emission quasars than in lower redshift studies, although still based on low number statistics, this may imply that the quasar population could be more diverse than previously thought.

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The quasar relation through cosmic time - I. Data set and black hole masses

Cited by 35 publications

References 63 publications

What drives the growth of black holes?

What drives the growth of black holes?

The first ultraviolet quasar-stacked spectrum at z ≃ 2.4 from WFC3

The discovery of eight z ~ 6 quasars from Pan-STARRS1

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