Access to Astronomical Catalogues

← Click to display the menu
J/ApJ/801/45  Quasars properties and reverberation mapping  (Hernitschek+, 2015)

Estimating black hole masses in hundreds of quasars. Hernitschek N., Rix H.-W., Bovy J., Morganson E. <Astrophys. J., 801, 45 (2015)> =2015ApJ...801...45H (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Active gal. nuclei ; Galaxies, photometry ; Redshifts ; Equivalent widths Keywords: galaxies: photometry - quasars: supermassive black holes Abstract: We explore the practical feasibility of active galactic nucleus (AGN) broadband reverberation mapping and present first results. We lay out and apply a rigorous approach for the stochastic reverberation mapping of unevenly sampled multi-broadband flux measurements, assuming that the broad-line region (BLR) line flux is contributing up to 15% in some bands, and is directly constrained by one spectroscopical epoch. The approach describes variations of the observed flux as the continuum, modeled as a stochastic Gaussian process, and emission line contribution, modeled as a scaled, smoothed, and delayed version of the continuum. This approach can be used not only to interpolate in time between measurements, but also to determine confidence limits on continuum-line emission delays. This approach is applied to Sloan Digital Sky Survey observations in Stripe 82 (S82), providing flux measurements that are precise to 2% at ∼60 epochs over ∼10 yr. The strong annual variations in the epoch sampling prove a serious limitation in practice. In addition, suitable redshift ranges must be identified where strong, broad emission lines contribute to one filter, but not to another. By generating and evaluating problem-specific mock data, we verify that S82-like data can constrain τdelay for a simple transfer function model. In application to real data, we estimate τdelay for 323 AGNs with 0.225<z<0.846, combining information for different objects through the ensemble-scaling relationships for BLR size and black hole mass. Our analysis tentatively indicates a 1.7 times larger BLR size of Hα and Mg II compared to Kaspi et al. (2000ApJ...533..631K; 2007ApJ...659..997K) and Vestergaard (2002ApJ...571..733V; 2006ApJ...641..689V), but the seasonal data sampling casts doubt on the robustness of the inference. Description: We present novel empirical relationships for estimating the BLR sizes in AGNs developed using multi-epoch photometry combined with single-epoch spectroscopy. The found that scaling relationships between line widths and luminosity are based on empirical relationships between the broad-line region (BLR) size and luminosities in various bands by Kaspi et al. (2000ApJ...533..631K), Bentz et al. (2013ApJ...767..149B), and Vestergaard (2002ApJ...571..733V). To obtain more definite results on the RBLR-L and MBH-L relations, we evaluate well-defined subsamples of reverberation-mapped AGN, as shown in the Tables 2-5. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 124 29 Sample 1 Properties and Reverberation Mapping Results z=0.225-0.291, with i Band: Hα, z Band: Continuum table3.dat 124 68 Sample 2 Properties and Reverberation Mapping Results z=0.555-0.591, with g Band: Mg II, r Band: Continuum table4.dat 124 111 Sample 3 Properties and Reverberation Mapping Results z=0.592-0.6999, with g Band: Mg II, r Band: Continuum table5.dat 124 115 Sample 4 Properties and Reverberation Mapping Results z=0.7-0.846, with g Band: Mg II, r Band: Continuum
See also: VII/69 : Asiago Catalogue of QSOs (Barbieri+ 1983) J/ApJ/613/682 : AGN central masses and broad-line region sizes (Peterson+, 2004) J/ApJ/669/791 : Quasar black hole masses (Wilhite+, 2007) J/A+A/525/A37 : Variability indexes of QSOs in SDSS Stripe 82 (Meusinger+, 2011) J/ApJ/805/96 : SDSS-RM project: velocity dispersions of QSOs (Shen+, 2015) Byte-by-byte Description of file: table2.dat table3.dat table4.dat table5.dat
Bytes Format Units Label Explanations
1- 18 I18 --- ID objid SDSS unique object identifier 20- 25 F6.4 --- z Redshift 27- 34 E8.3 0.1nm EW Rest frame equivalent width of broad line 36- 41 E6.3 0.1nm e_EW Uncertainty in EW 43- 52 E10.6 10+3km/s FWHM(Hb) ? FWHM of broad Hβ line 54- 59 E6.2 10+3km/s e_FWHM(Hb) ? Uncertainty in FWHM(Hb) 61- 67 F7.4 [10-7W] logL5100 Log luminosity at 5100Å (erg/s) 69- 74 F6.4 [10-7W] e_logL5100 Uncertainty in logL5100 76- 83 E8.5 173AU RBLRk BLR (broad-line region) size, computed from Kaspi relation (2000ApJ...533..631K), in rest frame, in light-days units 85- 90 E6.3 173AU E_RBLRk ? Upper limit uncertainty in RBLRk 92- 97 E6.3 173AU e_RBLRk ? Lower limit uncertainty in RBLRk 99-106 E8.4 173AU RBLR BLR size own computed from all points within the 68% confidence interval, in rest frame, in light-days units 108-115 E8.4 173AU E_RBLR Upper limit uncertainty in RBLR 117-124 E8.4 173AU e_RBLR Lower limit uncertainty in RBLR
History: From electronic version of the journal
(End) Prepared by Tiphaine Pouvreau [CDS] 25-Aug-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

catalogue service

© UDS/CNRS

Contact