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J/ApJ/809/20   The MBH-σ relation for active galaxies   (Bennert+, 2015)

A local baseline of the black hole mass scaling relations for active galaxies. III. The MBH-σ relation. Bennert V.N., Treu T., Auger M.W., Cosens M., Park D., Rosen R., Harris C.E., Malkan M.A., Woo J.-H. <Astrophys. J., 809, 20 (2015)> =2015ApJ...809...20B (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, Seyfert ; Active gal. nuclei ; Redshifts ; Velocity dispersion ; Spectroscopy Keywords: accretion, accretion disks - black hole physics - galaxies: active - galaxies: evolution - quasars: general Abstract: We create a baseline of the black hole (BH) mass (MBH)-stellar-velocity dispersion (σ) relation for active galaxies, using a sample of 66 local (0.02<z<0.09) Seyfert-1 galaxies, selected from the Sloan Digital Sky Survey (SDSS). Analysis of SDSS images yields AGN luminosities free of host-galaxy contamination, and morphological classification. 51/66 galaxies have spiral morphology. Out of these, 28 bulges have Sersic index n<2 and are considered candidate pseudo-bulges, with eight being definite pseudo-bulges based on multiple classification criteria met. Only 4/66 galaxies show signs of interaction/merging. High signal-to-noise ratio Keck spectra provide the width of the broad Hβ emission line free of Fe II emission and stellar absorption. AGN luminosity and Hβ line widths are used to estimate MBH. The Keck-based spatially resolved kinematics is used to determine stellar-velocity dispersion within the spheroid effective radius (σspat,reff). We find that σ can vary on average by up to 40% across definitions commonly used in the literature, emphasizing the importance of using self-consistent definitions in comparisons and evolutionary studies. The MBH-σ relation for our Seyfert-1 galaxy sample has the same intercept and scatter as that of reverberation-mapped AGNs as well as that of quiescent galaxies, consistent with the hypothesis that our single epoch MBH estimator and sample selection function do not introduce significant biases. Barred galaxies, merging galaxies, and those hosting pseudo-bulges do not represent outliers in the MBH-σ relation. This is in contrast with previous work, although no firm conclusion can be drawn on this matter due to the small sample size and limited resolution of the SDSS images. Description: The sample was selected from the SDSS Data Release (DR) six following these criteria: (i) MBH>107 M as estimated based on optical luminosity and FWHM of the broad Hβ line; (ii) redshift range 0.02<z<0.09 to measure stellar kinematics via the Ca II triplet line in the optical and to ensure that the objects are well resolved. A total of 103 objects were observed between 2009 January and 2010 March with the Low Resolution Imaging Spectrometer (LRIS) at Keck I using a 1" wide long slit, aligned with the host galaxy major axis as determined from SDSS ("expPhi_r"). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 91 79 Sample and Derived Quantities
See also: II/294 : The SDSS Photometric Catalog, Release 7 (Adelman-McCarthy+, 2009) J/ApJ/596/437 : Stellar-mass black holes in the SDSS (Chisholm+, 2003) J/ApJ/641/L21 : Black hole mass and velocity dispersion relation (Greene+, 2006) J/ApJ/667/131 : Mass function of active black holes (Greene+, 2007) J/ApJS/201/29 : Velocity dispersions in active galaxies (Harris+, 2012) J/ApJ/831/134 : BH masses + host galaxy dispersion vel. (van den Bosch, 2016) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Name Target name (HHMM+DDMM) 11- 12 I2 h RAh Hour of Right Ascension (J2000) 14- 15 I2 min RAm Minute of Right Ascension (J2000) 17- 21 F5.2 s RAs Second of Right Ascension (J2000) 23 A1 --- DE- Sign of the Declination (J2000) 24- 25 I2 deg DEd Degree of Declination (J2000) 27- 28 I2 arcmin DEm Arcminute of Declination (J2000) 30- 33 F4.1 arcsec DEs Arcsecond of Declination (J2000) 35- 40 F6.4 --- z Redshift from SDSS-DR7 (Cat. II/294) 42- 44 I3 km/s sigma ? Spatially resolved stellar-velocity dispersion within spheroid effective radius (1) 46- 50 F5.2 arcsec Re Spheroid effective radius 52- 55 I4 km/s sigmaH Second moment of broad Hβ 57- 59 I3 km/s e_sigmaH Uncertainty in sigmaH 61- 65 F5.3 10+37W L5100 Rest-frame luminosity at 5100Å (in 1044 erg/s) (2) 67- 70 F4.2 [Msun] logMBH Log of black hole mass (uncertainty of 0.4 dex) 72- 76 A5 --- Host Host-galaxy decomposition (3) 78 A1 --- Class [CP] Classification of spheroid (4) 80- 91 A12 --- Other Alternative name from NED
Note (1): Determined from CaT, if available, else MgIb or CaHK (Harris et al. 2012, J/ApJS/201/29) according to Equation (1) (uncertainty of 0.04 dex). Note (2): Determined from SDSS g' band surface photometry (fiducial error 0.1 dex). Note (3): Host-galaxy as follows: B = "bulge only"; BD = "bulge+disk"; BDB = "bulge+disk+bar"; (M) = Indicates an interacting or merging galaxy. Note (4): Classification as follows: C = Classical bulge; P = Pseudo-bulge.
History: From electronic version of the journal References: Bennert et al. Paper I 2011ApJ...726...59B Harris et al. Paper II 2012ApJS..201...29H, Cat. J/ApJS/201/29
(End) Prepared by Tiphaine Pouvreau [CDS] 20-Sep-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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