The Host Galaxies of Luminous Radio-Quiet Quasars

Percival, Will J.; Miller, L.; McLure, R. J.; Dunlop, James

doi:10.1007/978-1-4615-0695-9_3

Cited by 6 publications

(8 citation statements)

References 41 publications

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“…Although the universal validity of this boundary has recently been questioned by Percival et al (2000;also these proceedings), it is clearly present in our data. We therefore decided to incorporate it by multiplying the above expression by a factor H(L gal − xL nuc ) where H(t 1 − t 2 ) = 1 for t 1 > t 2 and 0 elsewhere is the Heavyside step function, and x is an adjustable parameter.…”

Section: Bivariate Luminosity Functionmentioning

confidence: 43%

The Luminosity Function of QSO Host Galaxies

Wisotzki

Kuhlbrodt

Jahnke

2001

QSO Hosts and Their Environments

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We report on results from H band imaging observations of a complete sample of high-luminosity low-redshift QSOs. The luminosity function of QSO hosts is similar in shape to that of normal galaxies, although offset in normalisation by a factor of 10 −4 . This supports the hypothesis that the parent population of quasars is identical to the general population of early-type field galaxies. IntroductionIdentifying the parent population of QSO host galaxies is one of the fundamental problems linking the QSO phenomenon to galaxy evolution in general. While the most widely adopted approach is to compare morphological (and increasingly also spectral) properties of normal and active galaxies, we investigate here the statistical distribution of galaxy luminosities. This short report highlights some results which will be elaborated in more detail in a series of forthcoming papers. We adopt h = 0.5 and q 0 = 0.5 throughout. 2.H band imaging of a complete QSO sampleIn order to constrain the overall luminosity distribution of QSO hosts, the investigated targets must represent a fair sample of the QSO population. To obtain also the normalisation, the sample has furthermore to be complete (in the sense of comprising all QSOs within a given area that are brighter than a well-defined flux limit). Our sample has been selected from the Hamburg/ESO bright quasar survey , with the following additional criteria: Right ascension between 9 h and 16 h ; nuclear absolute magnitudes M B J < −23; and redshifts z < 0.3. The resulting sample consisted of 30 targets distributed over 2200 deg 2 , all of which were subsequently observed. Because of the op-1

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Section: Bivariate Luminosity Functionmentioning

confidence: 43%

The Luminosity Function of QSO Host Galaxies

Wisotzki

Kuhlbrodt

Jahnke

2001

QSO Hosts and Their Environments

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“…A summary of these observations is given in Table 1. For completeness, we have also included the photometry obtained by other groups as well (Giles et al 1999;Percival et al 1998;Homer et al 2001).…”

Section: Observations and Resultsmentioning

confidence: 99%

The Optical Counterpart of the Accreting Millisecond Pulsar SAX J1808.4−3658 in Outburst: Constraints on the Binary Inclination

Wang

Chakrabarty

Roche

et al. 2001

The Astrophysical Journal

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We present multiband optical/IR photometry of V4580 Sgr, the optical counterpart of the accretion-powered millisecond pulsar SAX J1808.4Ϫ3658, taken during the 1998 X-ray outburst of the system. The optical flux is consistent with emission from an X-ray-heated accretion disk. Self-consistent modeling of the X-ray and optical emission during the outburst yields a best-fit extinction of and an inclination of emission and are too bright to be from either the disk or the companion, even in the presence of X-ray heating.

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“…Still, a clear picture has not emerged, with some studies claiming a high fraction of disk morphologies amongst the radio-quiets (e.g. Percival et al 2000), whilst others suggest that nearly all quasars are in giant ellipticals (e.g. McLure et al 2000).…”

Section: Introductionmentioning

confidence: 99%

Radio-quiet quasar environments at 0.5 <= z <= 0.8

Wold¹,

Lacy²,

Lilje³

et al. 2001

Monthly Notices of the Royal Astronomical Society

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We quantify the galaxy environments around a sample of 0.5≤z≤0.8 radio‐quiet quasars using the amplitude of the spatial galaxy–quasar correlation function, Bgq. The quasars exist in a wide variety of environments; some sources are located in clusters as rich as Abell class 1–2 clusters, whereas others exist in environments comparable to the field. We find that, on average, the quasars prefer poorer clusters of ≈Abell class 0, which suggests that quasars are biased tracers of mass compared with galaxies. The mean Bgq for the sample is found to be indistinguishable from the mean amplitude for a sample of radio‐loud quasars matched in redshift and optical luminosity. These observations are consistent with recent studies of the hosts of radio‐quiet quasars at low to intermediate redshifts, and suggest that the mechanism for the production of powerful radio jets in radio‐loud quasars is controlled by processes deep within the active galactic nucleus itself, and is unrelated to the nature of the hosts or their environments.

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The Host Galaxies of Luminous Radio-Quiet Quasars

Cited by 6 publications

References 41 publications

The Luminosity Function of QSO Host Galaxies

The Luminosity Function of QSO Host Galaxies

The Optical Counterpart of the Accreting Millisecond Pulsar SAX J1808.4−3658 in Outburst: Constraints on the Binary Inclination

Radio-quiet quasar environments at 0.5 <= z <= 0.8

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