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J/ApJ/699/453      Determination of black hole masses      (Shaposhnikov+, 2009)

Determination of black hole masses in Galactic black hole binaries using scaling of spectral and variability characteristics. Shaposhnikov N., Titarchuk L. <Astrophys. J., 699, 453-468 (2009)> =2009ApJ...699..453S
ADC_Keywords: Binaries, X-ray ; Models Keywords: accretion, accretion disks - black hole physics - radiation mechanisms: non-thermal - stars: individual (XTE J1550-564, H 1743-322, GX 339-4, 4U 1630-47, GRS 1915+105, XTE 1650-500, XTE 1859+226, 4U 1543-47) Abstract: We present a study of correlations between X-ray spectral and timing properties observed from a number of Galactic black hole (BH) binaries during hard-soft state spectral evolution. We analyze 17 transition episodes from eight BH sources observed with Rossi X-Ray Timing Explorer. Our scaling technique for BH mass determination uses a correlation between the spectral index and quasi-periodic oscillation (QPO) frequency. In addition, we use a correlation between the index and the normalization of the disk "seed" component to cross-check the BH mass determination and estimate the distance to the source. We use GRO J1655-40 as a primary reference source for which the BH mass, distance, and inclination angle are evaluated by dynamical measurements with unprecedented precision among other Galactic BH sources. We apply our scaling technique to determine BH masses and distances for Cygnus X-1, GX 339-4, 4U 1543-47, XTE J1550-564, XTE J1650-500, H 1743-322, and XTE J1859-226. A good agreement of our results for sources with known values of BH masses and distance provides independent verification for our scaling technique. Description: For the study presented in this paper, we have analyzed data for 17 spectral transitions in seven BH transient sources observed with the Rossi X-Ray Timing Explorer (RXTE; data from We also analyzed a subset of Cyg X-1 data taken during 2001-2002 when the source showed a transition from the quiescent, low-hard state (LHS) to the high-soft (HSS). In Table 1, we summarize data for each transition and also provide references to previous analyses. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 53 17 Spectral transition data used in analysis table2.dat 149 363 Spectral and timing characteristics for RXTE data
See also: J/ApJ/687/471 : Observational comparison between ULXs and XRBs (Berghea+, 2008) J/ApJS/168/1 : Black hole mass estimates (Kelly+, 2007) J/ApJ/667/131 : Mass function of active black holes (Greene+, 2007) J/ApJ/614/91 : Black hole mass and accretion rate of AGNs (Wu+, 2004) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 13 A13 --- Source Source name 15- 23 A9 --- TID Transition identification 25- 32 A8 "YY/MM/DD" SDate Date of start 34- 41 A8 "YY/MM/DD" EDate Date of end 43- 47 A5 --- Type Transition type (rise, decay or mixed) 49- 53 A5 --- Ref Reference(s) (1)
Note (1): References as follows: 1 = Rodriguez et al. 2003ApJ...595.1032R; 2 = Rodriguez et al. 2004ApJ...612.1018R; 3 = McClintock et al. 2009ApJ...698.1398M; 4 = Belloni et al. 2006MNRAS.367.1113B; 5 = Belloni et al. 2005A&A...440..207B; 6 = Casella et al. 2004A&A...426..587C; 7 = Rossi et al. 2004NuPhS.132..416R; 8 = Trudolyubov et al. 2001ApJ...558..276T; 9 = Kalemci et al. 2005ApJ...622..508K; 10 = Park et al. 2004ApJ...610..378P; 11 = Shaposhnikov & Titarchuk (2007ApJ...663..445S); 12 = Trudolyubov 2001ApJ...558..276T; 13 = Vignarca et al. 2003A&A...397..729V
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 9 A9 --- TID Transition identification 11- 25 A15 --- OID Observation identification 27- 34 F8.2 d MJD Modified Julian Date at RXTE observation start 36- 38 A3 --- State Black hole state (1) 40- 46 F7.4 Hz nu ? Frequency of quasi-periodic oscillation 48- 53 F6.4 Hz e_nu ? Uncertainty in nu 55- 59 F5.3 --- alpha Model spectral index 61- 65 F5.3 --- e_alpha Uncertainty in alpha 67- 71 F5.3 keV kT Model temperature 73- 77 F5.3 keV e_kT Uncertainty in kT 79- 84 F6.3 [-] logA Model log(A) parameter (2) 86- 89 F4.2 [-] e_logA ? Uncertainty in logA 91 A1 --- f_logA [f] Indicates logA is fixed 93- 99 F7.5 --- Nbmc Bulk Motion Comptonization normalization i L/d2 if L in 1039erg/s and d in (10kpc) 101-107 F7.5 --- e_Nbmc Uncertainty in Nbmc 109-112 F4.1 keV Ecut ? High energy cut-off 114-116 F3.1 keV e_Ecut ? Uncertainty in Ecut 118 A1 --- f_Ecut [f] indicates Ecut is fixed 120-124 F5.1 keV Efold ? Cut-off folding energy 126-129 F4.1 keV e_Efold ? Uncertainty in Efold 131-137 F7.4 10-11W/m2 FX X-ray flux (in 10-8erg/s/cm2) 139-144 F6.4 10-11W/m2 e_FX Uncertainty in FX 146-149 F4.2 --- chi2 Model reduced χ2
Note (1): Black hole (BH) observational appearance is conventionally described in terms of BH state classification (see Remillard & McClintock 2006ARA&A..44...49R; Belloni 2005A&A...440..207B; Klein-Wolt & van der Klis 2008ApJ...675.1407K, for different flavors of BH state definitions). We adopt the following general BH state classification for five major BH states: quiescent, low-hard (LHS), intermediate (IS), high-soft (HSS), and very high states (VHS). Note (2): The resulting model spectrum is also characterized by a parameter log(A) related to a Comptonized fraction f, where f=A/(1+A). See section 2 for further details.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 23-Jun-2011
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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