Stellar and gaseous velocity dispersions in type II AGNs at 0.3 &lt;<i>z</i>&lt; 0.83 from the Sloan Digital Sky Survey

Bian, Wei-Hao; Gu, Qiusheng; Zhao, Yi; Chao, Li-Chi; Qian, Cui,

doi:10.1111/j.1365-2966.2006.10915.x

Cited by 20 publications

(23 citation statements)

References 45 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“… We use SSP synthesis ( starlight ; Cid Fernandes et al 2005) to model the stellar contribution in the Galactic extinction‐corrected spectrum in the rest frame (Cid Fernandes et al 2005; Bian et al 2006, 2008; Bian, Chen & Gu 2007). The Galactic extinction law of Cardelli, Clayton & Mathis (1989) with R V = 3.1 is adopted, which is also used for the host extinction with V ‐band extinction (from 0 mag to 5.0 mag).…”

Section: Data and Analysismentioning

confidence: 99%

The host galaxy of a narrow-line Seyfert 1 galaxy, RE J1034+396, with X-ray quasi-periodic oscillations

Bian¹,

Huang²

2010

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Using simple stellar population synthesis, we model the bulge stellar contribution in the optical spectrum of a narrow-line Seyfert 1 galaxy, RE J1034+396. We find that its bulge stellar velocity dispersion is 67.7 ± 8 km s −1 . The supermassive black hole (SMBH) mass is about (1-4) × 10 6 M if it follows the well-known M BH -σ * relation found in quiescent galaxies. We also derive the SMBH mass from the Hβ second moment, which is consistent with that from its bulge stellar velocity dispersion. The SMBH mass of (1-4) × 10 6 M implies that the X-ray quasi-periodic oscillation (QPO) of RE J1034+396 can be scaled to a high-frequency QPO at 27-108 Hz found in Galactic black hole binaries with a 10-M black hole. With the mass distribution in different age stellar populations, we find that the mean specific star formation rate (SSFR) over the past 0.1 Gyr is 0.0163 ± 0.0011 Gyr −1 , the stellar mass in the logarithm is 10.155 ± 0.06 in units of solar mass and the current star formation rate is 0.23 ± 0.016 M yr −1 . For RE J1034+396, there is no relation between the Eddington ratio and the SSFR as suggested by Chen et al., despite a larger scatter in their relation. We also suggest that about 7.0 per cent of the total Hα luminosity and 50 per cent of the total [O II] luminosity come from the star formation process.

show abstract

Section: Data and Analysismentioning

confidence: 99%

The host galaxy of a narrow-line Seyfert 1 galaxy, RE J1034+396, with X-ray quasi-periodic oscillations

Bian¹,

Huang²

2010

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…We use the gas velocity dispersion of the narrow/core [O III] component from NLRs to trace the host stellar velocity dispersion, σ (Bian et al 2006). For SDSS spectra, the mean value of instrument resolution σ inst is 60 km s…”

Section: Smbh Mass Eddington Ratio and Stellar Velocity Dispersionmentioning

confidence: 99%

“…The fibers in the SDSS spectroscopic survey have a diameter of 3" on the sky. The SDSS spectra of lower-redshift quasars possibly have obvious stellar light contribution, which can be used to directly measure the stellar velocity dispersion (e.g., Kauffmann et al 2003;Heckman et al 2004;Bian et al 2006). For luminous quasars (M i < −22), the stellar light contribution can be omitted or has little effect on the mass calculation (e.g., Vanden Berk et al 2006).…”

Section: Uncertaintiesmentioning

confidence: 99%

Radio Luminosity, Black Hole Mass and Eddington Ratio for Quasars from the Sloan Digital Sky Survey

Bian¹,

Chen²,

Hu³

et al. 2008

Chin. J. Astron. Astrophys.

View full text Add to dashboard Cite

We investigate the M BH −σ * relation for radio-loud quasars with redshift z < 0.83 in Data Release 3 of the Sloan Digital Sky Survey (SDSS). The sample consists of 3772 quasars with better model of Hβ and [O III] lines and available radio luminosity, including 306 radio-loud quasars, 3466 radio-quiet quasars with measured radio luminosity or upper-limit of radio luminosity (181 radio-quiet quasars with measured radio luminosity). The virial supermassive black hole mass (M BH ) is calculated from the broad Hβ line, the host stellar velocity dispersion (σ * ) is traced by the core [O III] gaseous velocity dispersion, and the radio luminosity and the radio loudness are derived from the FIRST catalog. Our results are follows: (1) For radio-quiet quasars, we confirm that there is no obvious deviation from the M BH − σ * relation defined in inactive galaxies when M BH uncertainties and luminosity bias are concerned. (2) We find that radio-loud quasars deviate much from the M BH − σ * relation respect to that for radio-quiet quasars. This deviation is only partly due to the possible cosmology evolution of the M BH − σ * relation and the luminosity bias. (3) The radio luminosity is proportional to M 1.28+0.31 −0.24 for radio-quiet quasars and M 3.10+1.40 −1.10 for radio-loud quasars. The weaker correlation of the radio luminosity dependence upon the mass and the Eddington ratio for radio-loud quasars shows that other physical effects would account for their radio luminosities, such as the black hole spin.

show abstract

“…Zhang et al 2008). Using the MBH − σ * relation, the SMBH masses in type II AGNs are mainly derived from σ * (Kauffmann et al 2003a,b;Bian et al 2006). Considering the photon-ionization model of BLRs in AGNs, RBLRs can be estimated from the reverberation mapping (RM) method (e.g.…”

Section: Introductionmentioning

confidence: 99%

Calibration of the virial factor f in supermassive black hole masses of reverberation-mapped AGNs

Bian

Wang

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Using a compiled sample of 34 broad-line active galactic nuclei (AGNs) with measured Hβ time lags from the reverberation mapping (RM) method and measured bulge stellar velocity dispersions σ * , we calculate the virial factor f by assuming that the RM AGNs intrinsically obey the same M BH − σ * relation as quiescent galaxies, where M BH is the mass of the supermassive black hole (SMBH). Considering four tracers of the velocity of the broad-line regions (BLRs), i.e., the Hβ line width or line dispersion from the mean or rms spectrum, there are four kinds of the factor f . Using the Hβ Full-width at half-maximum (FWHM) to trace the BLRs velocity, we find significant correlations between the factor f and some observational parameters, e.g., FWHM, the line dispersion. Using the line dispersion to trace the BLRs velocity, these relations disappear or become weaker. It implies the effect of inclination in BLRs geometry. It also suggests that the variable f in M BH estimated from luminosity and FWHM in a single-epoch spectrum is not negligible. Using a simple model of thick-disk BLRs, we also find that, as the tracer of the BLRs velocity, Hβ FWHM has some dependence on the inclination, while the line dispersion σ Hβ is insensitive to the inclination. Considering the calibrated FWHM-based factor f from the mean spectrum, the scatter of the SMBH mass is 0.39 dex for our sample of 34 low redshift RM AGNs. For a high redshift sample of 30 SDSS RM AGNs with measured stellar velocity dispersions, we find that the SMBH mass scatter is larger than that for our sample of 34 low redshift RM AGNs. It implies the possibility of evolution of the M BH − σ * relation from high-redshift to low-redshift AGNs.

show abstract

Stellar and gaseous velocity dispersions in type II AGNs at 0.3 <z< 0.83 from the Sloan Digital Sky Survey

Cited by 20 publications

References 45 publications

The host galaxy of a narrow-line Seyfert 1 galaxy, RE J1034+396, with X-ray quasi-periodic oscillations

The host galaxy of a narrow-line Seyfert 1 galaxy, RE J1034+396, with X-ray quasi-periodic oscillations

Radio Luminosity, Black Hole Mass and Eddington Ratio for Quasars from the Sloan Digital Sky Survey

Calibration of the virial factor f in supermassive black hole masses of reverberation-mapped AGNs

Contact Info

Product

Resources

About