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INTREFCAT - INTEGRAL Reference Catalog |
HEASARC Archive |
After the launch of INTEGRAL, a version of this catalog was placed on the ISDC website at http://isdc.unige.ch/index.cgi?Data+catalogs and has been updated periodically since then by adding, for example, new sources discovered by INTEGRAL itself (indicated by the IGR prefix in the name). Thus, as of mid-2004, the INTEGRAL Reference Catalog contained 1390 sources. This HEASARC table is based on the web version at the ISDC, and will be updated whenever the latter is updated.
Additional information pertaining to an earlier version of this catalog:
High-energy sources before INTEGRAL. INTEGRAL reference catalog.
Ebisawa K., Bourban G., Bodaghee A., Mowlavi N., Courvoisier T.J.-L.
<Astron. Astrophys. 411, L59 (2003)>
=2003A&A...411L..59E (SIMBAD/NED BibCode)
This catalog has been built by merging different ones available in the HEASARC database. These are: Liu's HMXB catalog (A&AS,2000,147,25) Liu's LMXB catalog (A&A,2001,368,1021) Macomb & Gehrels Gamma ray sources catalog (ApJS,1999,120,335) 4th Uhuru catalog (ApJS,1978,182,489) HEAO1 A4 catalog (ApJS,1984,54,581) Piccinotti's sample AGNs Batse observations (ApJ,1999,519,637) Tartarus reduced ASCA AGN data ASCA catalog of Sugizaki et al.(2001yCat..21340077S) ASCA catalog of Sakano et al. (ApJS,2002,138,19)
The class numbers correspond to the HEASARC classification. When no indication was available in the catalogs, this value has been set to '1000'. For the HEASARC class definitions, see: http://isdc.unige.ch/Data/cat/class.html http://heasarc.gsfc.nasa.gov/W3Browse/catalog/class.htmlThe spectral models are simple descriptions of the spectral energy distribution. The normalizations have been adjusted by fitting the flux measurements reported in the catalogs after the assignment of a default spectral model to each type of source. The default models and their parameters are described in: http://isdc.unige.ch/Data/cat/models.html
ISGRI_FLAG set to: 0: sources never detected in a single science window in the 18.3-59.9 keV band 1: sources detected at least once in a single science window in the 18.3-59.9 keV band.ISGRI_FLAG2 set to: 1: fsources detected at least once in a single scw (i.e. the same as ISGRI_FLAG) 2: sources detected only in a mosaic 3: sources with questionable detection (e.g. reported only in one particular publication and not seen in a later mosaic).
Instrument flags for JEM-X, SPI and PICsIT are set to: 0: when the source is not detected. 1: when the source is detected. 2: when the source is detected and its position should be fixed for OSA (i.e. the same as SouFit=1). These flags signify a detection at the Science Window or mosaic image level, which has been published either in an ATel or circular, a refereed journal, or through archival analyses.The catalog is updated regularly when new information is published in a refereed journal or on one of the following sites: IAUC new sources (from #7341) Astronomer's Telegrams IGR sources page maintained by J. Rodriguez: (http://isdc.unige.ch/
The latest catalog is always available for download at: http://isdc.unige.ch/Data/cat/ or viewable online at: http://isdc.unige.ch/Data/cat/latestIf you have any questions or comments about this catalog please contact Claudio Ricci (claudio.ricci@obs.unige.ch).
Version 30, 2008-03-10 Updated by Claudio Ricci
IGR J19378-0617=1H 1934-063 SWIFT J2000.6+3210=IGR J20006+3210 * Added new sources (ISGRI flag set to 1) Swift J1816.7-1613 (ATEL 1456) IGR J17062-6143 (Churazov et al. 2007 A&A 467, 529) IGR J16293-4603 (ATel 1774) IGR J20216+4359 (Bikmaev et al., Astr. Lett. 2008, 653) IGR J17375-3022 (ATel 1781) XTE J1701-407 (ATel 1569) SGR 0501+4516 (ATel 1676, GCN 8163) SAX J1753.5-2349 (ATel 1809) 1RXS J092418.0-314212 Swift J1842.5-1124 (ATel 1610) IGR J015712-7259 (ATel 1882) MCG-03-34-064 (Paltani et al. 2008, A&A 485, 707) IGR J12299+0305 (Paltani et al. 2008, A&A 485, 707) IGR J12069-1448 (Paltani et al. 2008, A&A 485, 707) NGC 4939 (Paltani et al. 2008, A&A 485, 707) IGR J12174-0131 (Paltani et al. 2008, A&A 485, 707) IGR J12042-0756 (Paltani et al. 2008, A&A 485, 707) IGR J12070+2535 (Paltani et al. 2008, A&A 485, 707) IGR J13133-1109 (Paltani et al. 2008, A&A 485, 707) IGR J12060+3818 (Paltani et al. 2008, A&A 485, 707) IGR J13517-0042 (Paltani et al. 2008, A&A 485, 707) IGR J11457-1827 (Paltani et al. 2008, A&A 485, 707) IGR J12172+0710 (Paltani et al. 2008, A&A 485, 707) IGR J12136-0527 (Paltani et al. 2008, A&A 485, 707) IGR J12310+1221 (Paltani et al. 2008, A&A 485, 707) IGR J11225-0419 (Paltani et al. 2008, A&A 485, 707) IGR J13353-1113 (Paltani et al. 2008, A&A 485, 707) IGR J11427+0854 (Paltani et al. 2008, A&A 485, 707) * Refined positions for: IGR J16287-5021 (ATel 1649, Chandra) IGR J19267+1325 (ATel 1653, Chandra) IGR J18246-1425 (ATel 1681, Swift/XRT) IGR J18246-1425 (ATel 1686, Swift/XRT) IGR J17379-3747 (ATel 1711, IBIS/ISGRI) IGR J17379-3747 (ATel 1714, Swift/XRT) IGR J17062-6143 (ATel 1840, Swift/XRT) IGR J18450-0435 (Zurita & Walter 2008. ArXiV 0811.0983) IGR J03184-0014 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J03532-6829 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J05319-6601 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J05346-5759 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J09025-6814 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J13000+2529 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J15479-4529 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J17353-3539 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J17476-2253 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J23206+6431 (Rodriguez et al. 2008, ArXiV 0811.4707) AX J183039-1002 (Bassani et al. 2009, ArXiV 0901.2499) 4U 1210-64 (ATel 1253) * Counterparts added IGR J18246-1425 (ATel 1681) IGR J18246-1425 (ATel 1680) IGR J17379-3747 (ATel 1709) IGR J18308-1232 (ATel 1710) IGR J18259-0706 (Burenin et al., ArXiV 0810.2512) IGR J16426+6536 (ATel 1800) IGR J17062-6143 (ATel 1840) IGR J06253+7334 IGR J19443+2117 (Landi et al. 2008, ArXiV 0811.2318) IGR J22292+6647 (Landi et al. 2008, ArXiV 0811.2318) IGR J02466-4222 (Masetti et al. 2008, ArXiV 0811.4085) IGR J09025-6814 (Masetti et al. 2008, ArXiV 0811.4085) IGR J03184-0014 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J03532-6829 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J05346-5759 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J09025-6814 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J13000+2529 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J17353-3539 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J17476-2253 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J15161-3827 (Rodriguez et al. 2008, ArXiV 0811.4707) AX J1550.8-5418 (GCN 8321) 1H 1254-690 4U 1210-64 (ATel 1861) Swift J1200.8+0650 (Paltani et al. 2008, A&A 485, 707) * Identification changed IGR J19267+1325 (ATel 1653) IGR J18246-1425 (ATel 1680) IGR J17098-3628 (Chen et al. 2008, ArxiV 0808.2359) IGR J18308-1232 (ATel 1710) IGR J18483-0311 (Rahoui & Chaty, ArxiV 0809.4415) IGR J18259-0706 (Burenin et al., ArXiV 0810.2512) IGR J16426+6536 (ATel 1800) IGR J17062-6143 (ATel 1853) IGR J08390-4833 (Masetti et al. 2008, ArXiV 0811.4085) IGR J11098-6457 (Masetti et al. 2008, ArXiV 0811.4085) IGR J17404-3655 (Masetti et al. 2008, ArXiV 0811.4085) IGR J21347+4737 (Masetti et al. 2008, ArXiV 0811.4085) IGR J02466-4222 (Masetti et al. 2008, ArXiV 0811.4085) IGR J09025-6814 (Masetti et al. 2008, ArXiV 0811.4085) IGR J00333+6122 (Masetti et al. 2008, ArXiV 0811.4085) IGR J05270-6631 (Masetti et al. 2008, ArXiV 0811.4085) IGR J09253+6929 (Masetti et al. 2008, ArXiV 0811.4085) IGR J10147-6354 (Masetti et al. 2008, ArXiV 0811.4085) IGR J12415-5750 (Masetti et al. 2008, ArXiV 0811.4085) IGR J16426+6536 (Masetti et al. 2008, ArXiV 0811.4085) IGR J18249-3243 (Masetti et al. 2008, ArXiV 0811.4085) IGR J05319-6601 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J17476-2253 (Rodriguez et al. 2008, ArXiV 0811.4707) IGR J16479-4514 (ATel 1929) AX J1550.8-5418 (GCN 8321) AX J183039-1002 (Bassani et al. 2009, ArXiV 0901.2499) 4U 1210-64 (Masetti et al. 2009, A&A 495,121) * ISGRI flag switched to 1: HR 4492 AX J1550.8-5418 (GCN 8321) 1A1118-615 (ATel 1949) 4U 1210-64 (Masetti et al. 2009, A&A 495,121) NGC 4941 (Paltani et al. 2008, A&A 485, 707) Swift J1200.8+0650 (Paltani et al. 2008, A&A 485, 707) * ISGRI flag switched to 0: EXMS B1136-650 SLX 1744-300 (too close to SLX 1744-299 for being distinguished) PSR J1649-4349 (Identified as a new source IGR J16493-4348, Hill et al. 2008 MNRAS 385, 423) * JEMX flag switched to 1: 1A1118-615 (ATel 1949) STAMP = '2006-12-04T14:24:33 make_isdc_cat 1.8' CHECKSUM= 'dPVIdNSFdNSFdNSF' / HDU checksum updated 2007-09-14T07:57:44 DATASUM = '3720674799' / data unit checksum updated 2007-09-14T07:57:44 HISTORY File modified by user 'beckmann' with fv on 2007-09-14T09:51:02 HISTORY File modified by user 'ricci' with fv on 2008-02-22T17:12:08 HISTORY File modified by user 'ricci' with fv on 2008-02-22T17:14:44 END
Source_Number
The INTEGRAL Reference Catalog source number, in order of increasing J2000 RA.
Name
The INTEGRAL Reference Catalog source name. Often there are two or more names
commonly used for the same source. The authors have taken the name which they
consider to be the most popular in high-energy astrophysics and which is also
used as a SIMBAD source identifier. Thus, users can directly put the source
name into the SIMBAD query box.
RA
The Right Ascension of the high-energy source. In most cases, positions are
taken from SIMBAD. From time to time, however, the authors found and adopted
a more recent position determination than SIMBAD. The accuracy depends on the
individual sources, which was reflected in the representation of the source
positions in the original CDS table where the J2000 RAs were given with a
precision that varied from 0.001 seconds of time to 1 minute of time. To help
users, the HEASARC has added a parameter called ra_precision which has the
following values:
ra_precision meaning
60. position given with 1 minute of time precision
6. position given with 0.1 minutes of time precision
1. position given with 1 second of time precision
0.1 position given with 0.1 seconds of time precision
0.01 position given with 0.01 seconds of time precision
0.001 position given with 0.001 seconds of time precision
Dec
The Declination of the high-energy source. In most cases, positions are taken
from SIMBAD. From time to time, however, the authors found and adopted a more
recent position determination than SIMBAD. The accuracy depends on the
individual sources, which was reflected in the representation of the source
positions in the original CDS table where the J2000 Declinations were given
with a precision that varied from 0.01 arcseconds to 1 degree. To help
users, the HEASARC has added a parameter called dec_precision which has the
following values:
dec_precision meaning
3600. position given with 1 degree of precision
360. position given with 0.1 degrees of precision
60. position given with 1 arcminute of precision
6. position given with 0.1 arcminutes of precision
1. position given with 1 arcsecond of precision
0.1 position given with 0.1 arcseconds of precision
0.01 position given with 0.01 arcseconds of precision
RA_Precision
This parameter encodes the original precision of the RA in
the CDS table on which this HEASARC Browse table is based, as follows:
ra_precision meaning
60. position given with 1 minute of time precision
6. position given with 0.1 minutes of time precision
1. position given with 1 second of time precision
0.1 position given with 0.1 seconds of time precision
0.01 position given with 0.01 seconds of time precision
0.001 position given with 0.001 seconds of time precision
Dec_Precision
This parameter encodes the original precision of the Dec in
the CDS table on which this HEASARC Browse table is based, as follows:
dec_precision meaning
3600. position given with 1 degree of precision
360. position given with 0.1 degrees of precision
60. position given with 1 arcminute of precision
6. position given with 0.1 arcminutes of precision
1. position given with 1 arcsecond of precision
0.1 position given with 0.1 arcseconds of precision
0.01 position given with 0.01 arcseconds of precision
LII
The Galactic Longitude of the high-energy source.
BII
The Galactic Latitude of the high-energy source.
Error_Radius
The positional uncertainty of the high-energy source, in arcseconds.
Pos_Ref_Bibcode
The ADS Bibcode for the source position reference. This is for readers who
need to know the position accuracy and/or position determination method.
Often SIMBAD gives the source position reference as well as the position
itself, in which case the authors have taken both. Otherwise, they searched
for the proper references themselves.
Pos_Ref_Author
The authors of the position reference specified by the pos_ref_bibcode
parameter.
Source_ID
This parameter is the unique identifier for the source, and, will remain the
same even if the source position is modified at a later date.
ISGRI_Flag
This parameter has the value of 1 if the source has been detected by ISGRI;
otherwise, it is set to 0.
JEMX_Flag
This parameter has the value of 1 if the source has been detected by JEMX;
otherwise, it is set to 0.
SPI_Flag
This parameter has the value of 1 if the source has been detected by SPI;
otherwise, it is set to 0.
PICSIT_Flag
This parameter has the value of 1 if the source has been detected by PICSIT;
otherwise, it is set to 0.
Spectral_Model_Type
The authors derived a "typical" spectral model and model parameters,
including the model normalization. They followed the XSPEC format (Arnaud
1996; http://xspec.gsfc.nasa.gov) for the definition of the models and the
model parameters. See Sect. 4 of the published paper for more details.
Spectral_Model_Pars
The authors derived a "typical" spectral model and model parameters,
including the model normalization. They followed the XSPEC format (Arnaud
1996; http://xspec.gsfc.nasa.gov) for the definition of the models and the
model parameters. See Sect. 4 of the published paper for more details.
Flux_3_10keV
The 3 - 10 keV energy flux, in ergs s-1 cm-2, and calculated from the
assumed spectral models. The authors have taken typical JEMX soft and hard
energy bands (3 - 10 keV and 10 - 30 keV) and ISGRI soft and hard bands
(20 - 60 keV and 60 - 200 keV).
Flux_10_30keV
The 10 - 30 keV energy flux, in ergs s-1 cm-2, and calculated from the
assumed spectral models. The authors have taken typical JEMX soft and hard
energy bands (3 - 10 keV and 10 - 30 keV) and ISGRI soft and hard bands
(20 - 60 keV and 60 - 200 keV).
Flux_20_60keV
The 20 - 60 keV energy flux, in ergs s-1 cm-2, and calculated from the
assumed spectral models. The authors have taken typical JEMX soft and hard
energy bands (3 - 10 keV and 10 - 30 keV) and ISGRI soft and hard bands
(20 - 60 keV and 60 - 200 keV).
Flux_60_200keV
The 60 - 200 keV energy flux, in ergs s-1 cm-2, and calculated from the
assumed spectral models. The authors have taken typical JEMX soft and hard
energy bands (3 - 10 keV and 10 - 30 keV) and ISGRI soft and hard bands
(20 - 60 keV and 60 - 200 keV).
JEMX_Soft_Count_Rate
Using the nominal INTEGRAL detector responses, the expected count rate in the
Joint European X-Ray Monitor (JEMX), calculated for the soft JEMX energy band
(3 - 10 keV). In the actual QLA operation, JEMX and ISGRI source count rates
are measured in these energy bands so as to compare with the catalog. The
following calibration files, most recent ones in July 2003 (but still based
on pre-launch calibration), are used in this calculation:
jmx2_rmf_grp_0003.fits for JEMX and isgr_rmf_grp_0005.fits and
isgr_arf_rsp_0002.fits for ISGRI.
After the launch of INTEGRAL, the pre-launch estimate of the JEMX effective area was revealed to be overestimated by a factor of 2 (P. Kretschmar, private communication). Therefore, the authors divided the JEMX count rates calculated using the aforementioned responses by a factor of two. This prescription has been confirmed to be valid from simultaneous INTEGRAL-RXTE observations of the source 3C 273 (Courvoisier et al. 2003, A&A, 411, L343) and Cyg X-1 (Pottschmidt et al. 2003, A&A, 411, L383).
JEMX_Hard_Count_Rate
Using the nominal INTEGRAL detector responses, the expected count rate in the
Joint European X-Ray Monitor (JEMX), calculated for the hard JEMX energy band
(10 - 30 keV). In the actual QLA operation, JEMX and ISGRI source count rates
are measured in these energy bands so as to compare with the catalog. The
following calibration files, most recent ones in July 2003 (but still based
on pre-launch calibration), are used in this calculation:
jmx2_rmf_grp_0003.fits for JEMX and isgr_rmf_grp_0005.fits and
isgr_arf_rsp_0002.fits for ISGRI.
After the launch of INTEGRAL, the pre-launch estimate of the JEMX effective area was revealed to be overestimated by a factor of 2 (P. Kretschmar, private communication). Therefore, the authors divided the JEMX count rates calculated using the aforementioned responses by a factor of two. This prescription has been confirmed to be valid from simultaneous INTEGRAL-RXTE observations of the source 3C 273 (Courvoisier et al. 2003, A&A, 411, L343) and Cyg X-1 (Pottschmidt et al. 2003, A&A, 411, L383).
ISGRI_Soft_Count_Rate
Using the nominal INTEGRAL detector responses, the expected count rate in the
ISGRI CdTe array of the Imager on Board the INTEGRAL Satellite (IBIS)
instrument, calculated for the soft ISGRI energy band (20 - 60 keV). In the
actual QLA operation, JEMX and ISGRI source count rates are measured in these
energy bands so as to compare with the catalog. The following calibration
files, most recent ones in July 2003 (but still based on pre-launch
calibration), are used in this calculation: jmx2_rmf_grp_0003.fits for JEMX
and isgr_rmf_grp_0005.fits and isgr_arf_rsp_0002.fits for ISGRI.
For ISGRI, actual observations of the Crab pulsar and other sources confirmed that the pre-launch estimate of the effective area was more or less correct (within 20 % or so).
ISGRI_Hard_Count_Rate
Using the nominal INTEGRAL detector responses, the expected count rate in the
ISGRI CdTe array of the Imager on Board the INTEGRAL Satellite (IBIS)
instrument, calculated for the hard ISGRI energy band (60 - 200 keV). In the
actual QLA operation, JEMX and ISGRI source count rates are measured in these
energy bands so as to compare with the catalog. The following calibration
files, most recent ones in July 2003 (but still based on pre-launch
calibration), are used in this calculation: jmx2_rmf_grp_0003.fits for JEMX
and isgr_rmf_grp_0005.fits and isgr_arf_rsp_0002.fits for ISGRI.
For ISGRI, actual observations of the Crab pulsar and other sources confirmed that the pre-launch estimate of the effective area was more or less correct (within 20 % or so).
Source_Type
A characterization of the source type, such as low-mass X-ray binary,
high-mass X-ray binary, Seyfert-1 galaxy, etc.
Alt_Names
Various alternate names for the high-energy source. Since there are
many varieties of sources, the authors did not have a consistent rule to
decide which aliases to choose. However, they did try to put at least one
alias directly related to high-energy satellites and/or catalogs. For example,
"4U" for the 4th Uhuru catalog (Forman et al. 1978, ApJS, 182, 489), and
"2EG" for the 2nd EGRET source catalog (Thompson et al. 1995, ApJS, 101, 259).
Class
The HEASARC Browse object classification, based on the value of the
source_type parameter.