XRAYSELBLL - X-Ray Selected BL Lac Objects Catalog

Overview

This table contains a catalog of 312 X-ray selected BL Lacertae objects (XBLs), optically identified through the end of 2011. It contains the names from different surveys, equatorial coordinates, redshifts, multi-frequency flux values, and luminosities for each source. In the reference, the different characteristics of these XBLs are statistically investigated (redshift, radio/optical/X-ray luminosities, central black hole (BH) mass, synchrotron peak frequency, broadband spectral indices, optical flux variability). Their values were collected through an extensive bibliographic and database search or calculated by the author. The redshifts range from 0.031 to 0.702 with a maximum of the distribution at z = 0.223. The 1.4-GHz luminosities of XBLs log (nu * L_nu) ~ 39 - 42 (in units of erg s^-1), while the optical V and X-ray (0.1-2.4 keV) bands show log (nu * L_nu) ~ 43 - 46 (same units). The XBL hosts are elliptical galaxies with effective radii r_eff = 3.26 - 25.40 kpc and ellipticities e = 0.04 - 0.52. Their R-band absolute magnitudes M_R range from -21.11 mag to -24.86 mag with a mean value of -22.83 mag. The V - R indices of the hosts range from 0.61 to 1.52 and reveal a fourth-degree polynomial relationship with z that enabled the author to evaluate the redshifts of five sources whose V - R indices were determined from the observations, but whose redshifts values are either not found or not confirmed. The XBL nuclei show a wider range of 7.31 mag for M_R, with the highest luminosity corresponding to M_R = -27.24 mag. The masses of the central BHs are found in the interval log M_BH = 7.39 - 9.30 (in units of solar masses), with the maximum of the distribution at log M_BH/M_sun = 8.30. The synchrotron peak frequencies are spread over the range log nu_peak = 14.56 - 19.18 Hz, with a peak of the distribution at log nu_peak = 16.60 Hz. The broad-band radio-to-optical (alpha_ro), optical-to-X-ray (alpha_ox), and radio-to-X-ray (alpha_rx) spectral indices are distributed in the intervals (0.17, 0.59), (0.56, 1.48), and (0.41, 0.75), respectively. In the optical energy range, the overall flux variability increases, on average, towards shorter wavelengths: Delta(m) = 1.22, 1.50, and 1.82 through the R, V, B bands of the Johnson-Cousins system, respectively. XBLs seem be optically less variable at intranight timescales compared to radio-selected BL Lacs (RBLs).

Catalog Bibcode

2013AJ....145...31K

References

Catalog and Statistical Study of X-Ray Selected BL Lacertae Objects
   Kapanadze, B.Z.
   Astronomical Journal, Volume 145, Issue 2, article id. 31, 28 pp. (2013).
   =2013AJ....145...31K   (SIMBAD/NED BibCode)

Provenance

This table was created by the HEASARC in June 2013 based on an electronic version of Table 2 from the reference paper which was obtained form the AJ web site.

Parameters

Name
The designation of the XBL in one of the surveys in which it was included.

Alt_Name_1
The designation of the XBL in another of the surveys in which it was included.

Alt_Name_2
The designation of the XBL in another of the surveys in which it was included.

Alt_Name_3
The designation of the XBL in another of the surveys in which it was included.

Alt_Name_4
The designation of the XBL in another of the surveys in which it was included.

RA
The Right Ascension of the XBL in the selected equinox. This was given in J2000.0 coordinates to a precision of 0.1 seconds of time in the original table, except for several objects for which it was given to a precision of 1 second of time.

Dec
The Declination of the XBL in the selected equinox. This was given in J2000.0 coordinates to a precision of 1 arcsecond in the original table.

LII
The Galactic Longitude of the XBL.

BII
The Galactic Latitude of the XBL.

Redshift_Limit
This limit parameter is set to '>' if the corresponding parameter value is a lower limit rather than a precise value.

Redshift
The redshift of the XBL. The redshifts of XBLs were provided by different authors (Padovani & Giommi 1995, MNRAS, 277, 1477; Nilsson et al. 2003, A&A, 400, 95; Schwope et al. 2000, AN, 321, 1; Donato et al. 2005, A&A, 433, 1163; Giommi et al. 2005, A&A, 434, 385; Jannuzi et al. 1993, ApJS, 85, 265) and in the 13th Edition of the Catalog of Quasars and Active Galactic Nuclei (Veron-Cetty & Veron 2010, A&A, 518, 10). For some objects, different values are given by these authors and the present author chose those provided in the latest version of the Roma BZCAT, the multi-frequency blazar catalog compiled by Massaro et al. (2009, A&A, 495, 691), which contains the updated values of this parameter.

Redshift_Flag
This flag parameter is set to 'U' to indicate that there is some uncertainty in the corresponding parameter value.

F_Rad
The flux density of the XBL at 1.4 GHz, in mJy. The sources of these data are discussed in Section 2 of the reference paper. In a small number of cases (indicated by non-blank values of the f_rad_flag parameter), the corresponding observations do not exist, and other available data are provided instead: for example, the 5-GHz and 843-MHz flux values are given instead of the missing 1.4 GHz fluxes.

F_Rad_Flag
This flag parameter indicates the radio frequency for the quoted radio flux density (f_rad):

      (blank) = 1.4 GHz,
            a = 5 GHz,
            b = 843 MHz.

Log_L_Rad_Limit
This limit parameter is set to '>' if the corresponding parameter value is a lower limit rather than a precise value.

Log_L_Rad
The logarithm of the radio luminosity of the XBL, log (nu * L_rad), where L_rad is the monochromatic radio luminosity, in erg s^-1, for objects of known redshift.

Log_L_Rad_Flag
This flag parameter is set to 'U' to indicate that there is some uncertainty in the corresponding parameter value.

Vmag
The optical V-band magnitude of the XBL.

Vmag_Flag
This flag parameter indicates the following caveats concerning the quoted V magnitude:

        c = Derived from the B magnitude, as discussed in Section 2 of
            the reference paper,
        e = Derived from the V-band linear flux, as discussed in Section 2 of
            the reference paper,
        g = In cases where several measurements were available, the authors
            quotes the average value.

Log_L_Opt_Limit
This limit parameter is set to '>' if the corresponding parameter value is a lower limit rather than a precise value.

Log_L_Opt
The logarithm of the optical luminosity of the XBL, log (nu * L_opt), where L_opt is the monochromatic optical luminosity, in erg s^-1, for objects of known redshift.

Log_L_Opt_Flag
This flag parameter is set to 'U' to indicate that there is some uncertainty in the corresponding parameter value.

Fx
The X-ray flux of the XBL in the ROSAT 0.1-2.4 keV band, in erg cm^-2 s^-1, except for 2 cases (indicated by fx_flag = 'f') where the quoted values are the X-ray flux densities at 2 keV, in microJansky.

Fx_Flag
This flag parameter is set to 'f' if the quoted X-ray measurement is the X-ray flux density at 2 keV, in microJansky, rather than the X-ray flux in the 0.1-2.4 keV band, in erg cm^-2 s^-1.

Log_Lx_Limit
This limit parameter is set to '>' if the corresponding parameter value is a lower limit rather than a precise value.

Log_Lx
The logarithm of the X-ray luminosity of the XBL, log (nu * L_x), where L_x is the monochromatic X-ray luminosity, in erg s^-1, for objects of known redshift.

Log_Lx_Flag
This flag parameter is set to 'U' to indicate that there is some uncertainty in the corresponding parameter value.

Refs_Source
The reference source(s) for the radio, optical and X-ray data, respectively, for the particular XBL. The following abbreviations are given below (see reference paper for the full version of the references). Thus, 'RBC,B95/VV10,B97' means that the radio data came from the RBC, the optical data from B95 and VV10, and the X-ray data from B97.

      A10 = Abdo et al. (2010);
      A98 = Appenzeller et al. (1998);
      B94 = Brinkmann et al. (1995);
      B97 = Brinkmann et al. (1997);
      B95 = Brinkmann et al. (1995);
      B02 = Beckmann et al. (2003);
      B03 = Beckmann et al. (2003);
      C04 = Caccianiga et al. (2004);
      C98 = Condon et al. (1998);
      D05 = Donato et al. (2005);
      E92 = Elvis et al. (1992);
      F94 = Falomo et al. (1994);
      ESO = ESO Online Digitized Sky Survey service;
     FK99 = Falomo & Kotilainen (1999);
      G04 = Giroletti et al. (2004);
      G05 = Giommi et al. (2005);
      G87 = Giommi et al. (1987);
      G84 = Gioia et al. (1984);
      G90 = Gioia et al. (1990);
    GTB91 = Giommi et al. (1991);
    GCM05 = Galbiati et al. (2005);
      J93 = Jannuzi et al. (1993a);
      K10 = Kapanadze (2010b);
      M03 = Massaro et al. (2003);
      M85 = Moles et al. (1985);
      N96 = Nass et al. (1996);
      N03 = Nilsson et al. (2003);
      N06 = Nieppola et al. (2006);
      NED = NASA Extragalactic Database;
     PG95 = Padovani & Giommi (1995);
      P93 = Perlman & Stocke (1993);
      P96 = Perman et al. (1996);
      P07 = Piranomonte et al. (2007);
      R00 = Rector et al. (2000);
      R98 = Raiteri et al. (1998);
      RBC = Roma-BZCAT;
    SHL00 = Swope et al. (2000);
      S05 = Sbarufatti et al. (2005);
      S85 = Stocke et al. (1985);
      S91 = Stocke et al. (1991);
      S97 = Scarpa et al. (1997);
       TW = This work;
      V00 = Villata et al. (2000);
      V10 = Veron-Cetty & Veron (2010);
     WB92 = White & Becker (1992).

Fx_Over_F_Rad
The ratio of the X-ray flux to the radio flux for the XBL, in units of erg cm^-2 s^-1 Jy^-1.

Sample_IDs
The surveys corresponding to the quoted names for the XBL:

     BZCAT = Roma BZCAT
     EMSS  = Einstein Observatory Extended Medium Sensitivity Survey
     EXOSAT= EXO, Exosat Observatory
     HEAO-1= High Energy Astrophysical Observatory 1
     Mrk   = Markarian Catalog
     MSS-1 = Einstein Observatory Medium Sensitivity Survey, Paper 1
     MSS-2 = Einstein Observatory Medium Sensitivity Survey, Paper 2
     PG    = Palomar-Green Catalog
     RASS  = ROSAT All-Sky Survey
     Slew  = 1ES, the Einstein Slew Survey
     XBSS  = XMM-Newton Bright Serendipitous Survey

Contact Person

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Page Author: Browse Software Development Team
Last Modified: Monday, 16-Sep-2024 17:37:33 EDT