IBISCAT3 - Third IBIS/ISGRI Soft Gamma-Ray Survey Catalog
The main aim of the first survey (Bird et al. 2004, ApJ, 607, L33) 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. This gave evidence of a soft gamma-ray sky populated with more than 120 sources, including a substantial fraction of previously unseen sources. 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 The second IBIS/ISGRI catalog (Bird et al. 2006) used a greatly increased data set (of ~ 10 Ms) to unveil a soft gamma-ray sky comprising 209 sources in the energy range 20-100 keV, again with a substantial component (~ 25%) of new and unidentified sources, 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 Third IBIS/ISGRI Soft Gamma-Ray Survey Catalog. Bird A.J., Malizia A., Bazzano A., Barlow E.J., Bassani L., Hill A.B., Belanger G., Capitanio F., Clark D.J., Dean A.J., Fiocchi M., Gotz D., Lebrun F., Molina M., Produit N., Renaud M., Sguera V., Stephen J.B., Terrier R., Ubertini P., Walter R., Winkler C., Zurita J. <Astrophys. J. Suppl., 170, 175-186 (2007)> =2007ApJS..170..175B (SIMBAD/NED BibCode)
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:
B = new detection since second catalog; h = Source type from Veron and Veron ; i = Possibly associated with BAL QSO, SDSS J03184-0015; j = Possibly blended with ESO121-28, 4.8' away; k = Eta Carinae or source therein; l = Source type from CFA catalog; m = Significantly offset from original source position; n = Blended with NGC 6221; o = Blended with ESO 138-1; p = Coincident with Sgr A*, but not unambiguously identified; in confused Galactic Center region; q = Coincident with G0.13-0.13 molecular cloud; in confused Galactic Center region; r = In confused Galactic Center region; s = Blended with RX J2135.9+4728; t = Blended with IGR J21347+4737.
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 90% confidence 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 time-averaged 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 time-averaged 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 - 100 keV Flux, in mCrab.
The astrophysical type of the high-energy source. The following abbreviations have been used:
A = Atoll source (neutron star); AGN = Active galactic nuclei; 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; DN = Dwarf Nova; G = Globular Cluster X-ray source; GRB = Gamma-Ray Burst; HMXB = High-mass X-ray binary; IP = Intermediate Polar; LMXB = Low-mass X-ray binary; Mol Cloud = Molecular cloud; NS = Neutron Star; P = Polar; PSR = Radio pulsar; PWN = Pulsar wind nebula; QSO = Quasar; RG = Radio Galaxy; SFXT = Supergiant Fast X-ray Transient; SG = Supergiant; SGR = Soft gamma-ray 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 maximum significance of the high-energy source in a single map. Refer to the map_codes parameter in order to identify the map which has the maximum significance.
The corrected on-source exposure time, in seconds (s). This parameter was given in kiloseconds (ks) to a precision of 1 ks in the original, as-published table.
This parameter identifies the energy-band map in which the source has its maximum significance: (B1) 20 - 40 keV; (B2) 30 - 60 keV; (B3) 20 - 100 keV; (B4) 17 - 30 keV; (B5) 18 - 60 keV; a prefix of "RXXX" indicates a detection in INTEGRAL revolution XXX, a prefix of "SXXX" indicates a detection in an INTEGRAL revolution sequence beginning at INTEGRAL revolution XXX; and (ST) indicates staring data.
The HEASARC Browse object classification, based on the value of the source_type parameter (typically the most specific part).