On the black hole-bulge mass relation in active and inactive galaxies

McLure, R. J.; Dunlop, James

doi:10.1046/j.1365-8711.2002.05236.x

Cited by 521 publications

(680 citation statements)

References 45 publications

Supporting

Mentioning

595

Contrasting

Unclassified

Order By: Relevance

“…In Figure 10 we report the relationship between M(BH) and host galaxy absolute magnitude Mi compared with the local relation by Bettoni et al (2003) that is in good agreement with those by McLure & Dunlop (2002) and Ferrarese (2002) based on similar datasets. The local relation by (Bettoni et al 2003) that is calibrated on the R (Vega mag system) filter was transformed into Mi taking into account both the different cosmology assumed and the filter transformations.…”

Section: Comparison With Previous Studiessupporting

confidence: 67%

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.

View full text Add to dashboard Cite

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.

show abstract

Section: Comparison With Previous Studiessupporting

confidence: 67%

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.

View full text Add to dashboard Cite

show abstract

“…Firstly, Magorrian et al (1998) found that the kinematic data of 36 nearby galaxies indicate the presence of a massive dark object in the center of the galaxies and that the mass of the dark object correlates with the bulge luminosity and mass. Recent studies of this relationship obtain M BH ∼ 0.001M bulge (McLure & Dunlop 2002;Merritt & Ferrarese 2001). Secondly, the central velocity dispersion of the bulge σ 0 has been found to exhibit a tight correlation with the central black hole mass (Ferrarese & Merritt 2000, Gebhardt et al 2000.…”

Section: Introductionmentioning

confidence: 87%

R-band imaging of the host galaxies of RGB BL Lacertae objects

Nilsson

Pursimo

Heidt³

et al. 2003

A&A

124

View full text Add to dashboard Cite

Abstract. We present optical R-band images of 100 BL Lacertae objects in the ROSAT-Green Bank (RGB) sample obtained at the Nordic Optical Telescope (NOT). For 62 objects we could not find any previously published images in the literature, of these 35 are new BL Lacs discovered during the RGB BL Lac survey. We were able to resolve the host galaxy in 62% of the objects. We analyze the host galaxies using a two-dimensional fitting procedure and tabulate the best-fit core magnitude and host galaxy parameters (magnitude, effective radius, ellipticity, position angle and shape parameter β) for each object. With two exceptions, all objects are better fit by a model representing an elliptical galaxy (β = 0.25) than by a disk galaxy model (β = 1.0). In the two exceptions the disk host fit is only marginally better than the elliptical host fit, however, and we do not find a single clear example of a disk-dominated host galaxy. The host galaxies have an average brightness M R = −23.9 ± 0.8 and average effective radius r eff = 13.2 ± 0.8 kpc. Their bulk properties are indistinguishable from normal elliptical and radio galaxies. The median β is 0.18, well below the value 0.25 that is normally used to describe ellipticals. However, the difference may be caused by a selection effect due to the dependence of β on host galaxy luminosity.

show abstract

“…Two M BH measurements were found for this blazar. The value of log(M BH /M ) = 8.69, given by Falomo et al (2003a), is based on the correlation with the host galaxy bulge luminosity in R-band (M R − M BH , McLure & Dunlop (2002)). Based on the same galaxy property correlation M R − M BH , a value of log(M BH /M ) = 8.5 was reported by Wu et al (2009).…”

Section: Smbh Masses and Corresponding Time Scalesmentioning

confidence: 99%

Minimal variability time scale – central black hole mass relation of theγ-ray loud blazars

Vovk

Babić

2015

A&A

View full text Add to dashboard Cite

Context. The variability time scales of the blazar γ-ray emission contain the imprints of the sizes of their emission zones and are generally expected to be larger than the light-crossing times of these zones. In several cases the time scales were found to be as short ∼10 min, suggesting that the emission zone sizes are comparable with the sizes of the central supermassive black holes. Previously, these measurements also led to the suggestion of a possible connection between the observed minimal variability time scales and the masses of the corresponding black holes. This connection can be used to determine the location of the γ-ray emission site, which currently remains uncertain. Aims. The study aims to investigate the suggested "minimum time scale -black hole mass" relation using the blazars, detected in the TeV band. Methods. To obtain the tightest constraints on the variability time scales this work uses a compilation of observations by the Cherenkov telescopes HESS, MAGIC, and VERITAS. These measurements are compared to the blazar central black hole masses found in the literature.Results. The majority of the studied blazars show the variability time scales which are at least comparable to the period of rotation along the last stable orbit of the central black hole -and in some cases as short as its light-crossing time. For several sources the observed variability time scales are found to be smaller than the black hole light-crossing time. This suggests that the detected γ-ray variability originates, most probably, from the turbulence in the jet, sufficiently far from the central black hole.

show abstract

On the black hole-bulge mass relation in active and inactive galaxies

Cited by 521 publications

References 45 publications

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

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

R-band imaging of the host galaxies of RGB BL Lacertae objects

Minimal variability time scale – central black hole mass relation of theγ-ray loud blazars

Contact Info

Product

Resources

About