2008
DOI: 10.1088/0004-6256/136/4/1587
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Host Galaxies of Luminous Quasars: Structural Properties and the Fundamental Plane

Abstract: We present stellar velocity dispersion measurements in the host galaxies of 10 luminous quasars (M V < −23) using the Ca H&K lines in off-nuclear spectra. We combine these data with effective radii and magnitudes from the literature to place the host galaxies on the Fundamental Plane (FP) where their properties are compared to other types of galaxies. We find that the radio-loud (RL) QSO hosts have similar properties to massive elliptical galaxies, while the radio-quiet (RQ) hosts are more similar to intermedi… Show more

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Cited by 28 publications
(49 citation statements)
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References 89 publications
(207 reference statements)
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“…Also the hosts of optical and radio quasars seem to have somewhat different structural properties (e.g. Wolf & Sheinis 2008).…”
Section: Discussionmentioning
confidence: 99%
“…Also the hosts of optical and radio quasars seem to have somewhat different structural properties (e.g. Wolf & Sheinis 2008).…”
Section: Discussionmentioning
confidence: 99%
“…For the remaining quasars, the tight correlation between the mass M and the stellar velocity dispersion σ is exploited to estimate their masses [110,111]. There are thirteen such sources for which σ is estimated from [112] and [113] and the masses derived from the relation are given in [114]. One can determine the bolometric luminosity using a number of observations, e.g., high quality optical [81], UV [82], far-UV [83], and soft X-ray [84].…”
Section: Numerical Analysis: What Does Observations Tell Us?mentioning
confidence: 99%
“…The Fe ii template was adopted from the I Zw 1 Fe ii template of Boroson & Green (1992). The stellar template is composed of seven stellar spectra of G and K giants with various temperatures from the Indo-US spectral library 10 ( Valdes et al 2004), which have been widely used for stellar velocity dispersion measure ments on Keck spectra in many studies (e.g., Wolf & Sheinis 2008;Suyu et al 2010;Bennert et al 2011a;Fern ández Lorenzo et al 2011;Harris et al 2012;Suyu et al 2013). These highresolution stellar template spectra (∼34 km s −1 ; Beifiori et al 2011) were degraded to match the Keck spectral resolution.…”
Section: Black Hole Mass 3 Derived Quantitiesmentioning
confidence: 99%