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IBISCAT2 - Second IBIS/ISGRI Soft Gamma-Ray Survey Catalog



This table contains the second soft gamma-ray source catalog obtained with the IBIS/ISGRI gamma-ray imager on board the INTEGRAL satellite. The scientific data set is based on more than 10 Ms of high-quality observations performed during the first 2 years of the Core Program and public IBIS/ISGRI observations, and covers ~50% of the whole sky. The main aim of the first survey (available as the HEASARC Browse table IBISGPSCAT) was to scan systematically, for the first time at energies above 20 keV, the whole Galactic plane to achieve a limiting sensitivity of ~1 mCrab in the central radian. The target of the second year of the INTEGRAL mission was to expand as much as possible our knowledge of the soft gamma-ray sky, with the same limiting sensitivity, to at least 50% of the whole sky, mainly by including substantial coverage of extragalactic fields. This catalog comprises more than 200 high-energy sources detected in the energy range 20-100 keV, including new transients not active during the first year of operation, faint persistent objects revealed with longer exposure time, and several Galactic and extragalactic sources in sky regions not observed in the first survey. The mean position error for all the sources detected with significance above 10 sigma is ~40", enough to identify most of them with a known X-ray counterpart and to unveil the nature of most of the strongly absorbed ones, even though they are very difficult to detect in X-rays.

Catalog Bibcode



The Second IBIS/ISGRI Soft Gamma-Ray Survey Catalog.
    Bird A.J., Barlow E.J., Bassani L., Bazzano A., Belanger G., Bodaghee A.,
    Capitanio F., Dean A.J., Fiocchi, M., Hill A.B., Lebrun F., Malizia, A.,
    Mas-Hesse J.M., Molina M., Moran L., Renaud M., Sguera V., Shaw S.E.,
    Stephen J.B., Terrier R., Ubertini P., Walter R., Willis D.R., Winkler C.
   <Astrophys. J., 636, 765-776 (2006)>
   =2006ApJ...636..765B    (SIMBAD/NED BibCode)


This database table was created by the HEASARC in May 2006 based on the machine-readable version of Table 2 of the above-cited paper which was obtained from the electronic ApJ website.


The standard designation for the source. Sources discovered by INTEGRAL have been given names using the IGR prefix.

This parameter is a flag which can have the following non-blank values:

      a = 4U0352+30 in 1st IBIS/ISGRI catalog (Cat1);
      b = Values derived from staring observations during revolutions 50, 154
          and 203;
      c = Detected during revolution 139;
      d = Cannot recover fluxes due to proximity to 4U0919-54;
      e = Detected during revolution 203;
      f = A1145.1-6141 in Cat1;
      g = Position taken from 1E catalog, due to blending with 2E1145.5-6155;
      h = Position taken from 1E catalog, due to blending with 2E1145.1-6141;
      i = 4U1516-569 in Cat1;
      j = IGR J16195-4945 in Cat1;
      k = Triangulum Australis;
      l = IGR J16393-4643 in Cat 1;
      m = PSR J1649-4349 in Cat1;
      n = Equally well associated with NGC 6221, also Sy2;
      o = Detected during revolution 171;
      p = EXMS B1709-232 in Cat1;
      q = Tentative association with NGC6334;
      r = IGRJ17254-3616 in Cat1;
      s = Detected during revolution 120;
      t = 1E1740.7-2943 in Cat1;
      u = M1741-293 in Cat1;
      v = Within 1.1' of Sgr A*;
      w = Fluxes unreliable due to blending in final mosaic, see Section 3.6;
      x = Detected during revolution 175;
      y = IGR J18027-2016 in Cat1;
      z = HESS source (SNR/PWN?);
      A = 4U1849-31 in Cat1;
      B = Detected during revolution 189;
      C = IGR J19140+098 in Cat1;
      X = new detection since first catalog.

The Right Ascension of the high-energy source in the selected equinox. This was given in J2000.0 coordinates and to a precision of 0.001 degrees in the original table.

The Declination of the high-energy source in the selected equinox. This was given in J2000.0 coordinates and to a precision of 0.001 degrees in the original table.

The Galactic Longitude of the high-energy source.

The Galactic Latitude of the high-energy source.

The positional error of the high-energy source, in arcminutes, expressed as the radius of the 1-sigma error circle.

This parameter is set to '<' if the associated soft-band flux of the particular source is an upper limit rather than a detection.

The flux of the high-energy source in the soft energy band (20-40 keV), in units of milliCrab (mCrab). Appropriate conversion factors for this band are 10 mCrab = 7.57 x 10^-11 erg/cm^2/s = 1.71 x 10^-3 photons/cm^2/s.

The uncertainty in the 20-40 keV flux, in mCrab.

This parameter is set to '<' if the associated hard-band flux of the particular source is an upper limit rather than a detection.

The flux of the high-energy source in the hard energy band (40-100 keV), in units of milliCrab (mCrab). Appropriate conversion factors for this band are 10 mCrab = 9.42 x 10^-11 erg/cm^2/s = 9.67 x 10^-4 photons/cm^2/s.

The uncertainty in the 40-100keV Flux, in mCrab.

The maximum significance of the high-energy source, quoted either in the band specified by the significance_flag parameter, or, if the latter is blank, in one revolution.

This parameter is a flag which, if populated, indicates the detection band, in keV, to which the quoted maximum significance applies. If left blank, the quoted significance is for one revolution.

The corrected on-source exposure, in seconds (s). This parameter was given with a precision of kiloseconds in the original, as-published table.

The astrophysical type of the high-energy source. The following abbreviations have been used:

               A = atoll source (neutron star)
             AGN = active galactic nucleus
             AXP = anomalous X-ray pulsar
               B = burster (neutron star)
              Be = B-type emission-line star
              Bh = black hole (confirmed mass evaluation)
             BHC = black hole candidate
         Cluster = cluster of galaxies
              CV = cataclysmic variable
               D = dipping source
               G = globular cluster X-ray source
            HMXB = high-mass X-ray binary
            LMXB = low-mass X-ray binary
       Mol cloud = molecular cloud
              NS = neutron star
             PSR = radio pulsar
             PWN = pulsar wind nebula
             QSO = quasar
             SGR = soft gamma repeater
             SNR = supernova remnant
              Sy = Seyfert galaxy
            Symb = symbiotic star
               T = transient source
               U = ultrasoft source
              XB = Galactic X-ray binary
              XP = X-ray pulsar
               Z = Z-type source (neutron star)

The reference(s) for the particular source coded as follows (the full references are given in the published paper):

       1 = Downes et al. (2001);
       2 = Liu et al. (2000);
       3 = Raguzova & Popov(2005);
       4 = Veron-Cetty & Veron(2003);
       5 = Forman et al. (1978);
       6 = Liu et al. (2001);
       7 = Molina et al. (2004);
       8 = Bassani et al. (2005);
       9 = Masetti et al. (2005);
      10 = Done et al. (1996);
      11 = Dermer & Gehrels(1995);
      12 = Laurent et al. (1994);
      13 = Haberl et al. (2002);
      14 = Stephen et al. (2005a);
      15 = Orosz et al. (2002);
      16 = Stephen et al. (2005b);
      17 = Sidoli et al. (2005);
      18 = Walter et al. (2003);
      19 = Rodriguez et al. (2003);
      20 = Lutovinov et al. (2005a);
      21 = Patel et al. (2004);
      22 = Ebeling et al. (2002);
      23 = Combi et al. (2004);
      24 = Malizia et al. (2004);
      25 = Walter et al. (2004b);
      26 = Walter et al. (2004a);
      27 = Grebenev et al. (2005);
      28 = Cowley et al. (1987);
      29 = in't Zand et al. (2005a);
      30 = Lutovinov & Revnivtsev(2003);
      31 = Arnaud et al. (1987);
      32 = Rupen et al. (2003);
      33 = Sekimoto et al. (2000);
      34 = Barlow et al. (2005);
      35 = Masetti et al. (2004a);
      36 = Gaensicke et al. (2005);
      37 = Lutovinov et al. (2005b);
      38 = Harmon et al. (2004);
      39 = in't Zand et al. (2002);
      40 = Torres et al. (2004);
      41 = Sunyaev et al. (1991);
      42 = Mirabel et al. (1992);
      43 = Belanger et al. (2004);
      44 = Markwardt et al. (2003c);
      45 = Revnivtsev et al. (2004);
      46 = Gonzalez-Riestra et al. (2004);
      47 = Revnivtsev(2003);
      48 = Markwardt et al. (2003b);
      49 = Rodriguez et al. (1992);
      50 = Augello et al. (2003);
      51 = Hill et al. (2005);
      52 = Markwardt et al. (2003a);
      53 = Atteia et al. (1987);
      54 = Ubertini et al. (2005b);
      55 = Davelaar et al. (1986);
      56 = Malizia et al. (2005);
      57 = Bamba et al. (2001);
      58 = Vasisht & Gotthelf(1997);
      59 = Gotthelf & Vasisht(1998);
      60 = Remillard et al. (2002);
      61 = Galloway et al. (2003);
      62 = Woods et al. (2002);
      63 = Levine et al. (2004);
      64 = in't Zand et al. (2005b);
      65 = Rodriguez et al. (2005);
      66 = Mirabel & Rodriguez(1994);
      67 = Swank & Morgan(2000);
      68 = Negueruela et al. (2000);
      69 = Masetti et al. (2004b).

The HEASARC Browse object classification, based on the value of the source_type parameter (typically the first part of the latter only).

Contact Person

Questions regarding the IBISCAT2 database table can be addressed to the HEASARC User Hotline.
Page Author: Browse Software Development Team
Last Modified: Tuesday, 08-Aug-2006 14:02:43 EDT