INTEGRAL Bright Source Catalog

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INTEGRAL U.S. Guest Observer Facility

INTEGRAL Bright Source Catalog

Here we present a compilation of the brightest sources seen by INTEGRAL in the 23-40 keV and 40-80 keV energy bands derived from publicly available data. This is a "quick-look" data compilation rather than a rigorous analysis, and it does not comprise a complete flux limited sample. ISGRI analysis has been performed at the INTEGRAL Science Data Centre, SPI analysis was done at the NASA INTEGRAL Guest Observer Facility. Apparent flux variations of non-variable sources are based on short exposure times and/or far off-axis position.

INTEGRAL/SPI fluxes are based on the assumption that f[20-40keV] = 0.1783 ph/cm**2/sec corresponds to 1 Crab. Highest flux measurements require at least a 3 sigma significance. Lowest flux represents the lowest measured flux with at least 1 sigma significance. The average fluxes are weighted means of all measurements with at least 1 sigma significance (if not mentioned different).

In contrast to the SPI fluxes, the ISGRI flux values are based on single science window measurements (usually 2000 sec long) and only include those values with at least 1.5 sigma significance.

In ISGRI the Crab has a nominal count rate of 90 counts/sec (23 - 40 keV) and 66 counts/sec (40 - 80 keV), respectively (determined for revolution 102 on-axis staring observation). For more information on sources seen by ISGRI, see also Bird et al. 2006, ApJ, 636. 765.

You can download the catalog in fits format here and use it as an input catalog (GNRL-REFR-CAT) in your analysis (note that the flux values in this catalog are the same as in the original ISDC reference catalog).

Download the Bright Source Catalog on your PalmOS® or Pocket PC® PDA

Note! These are preliminary results, and are intended as only a rough guide to those pursuing in-depth followup analyses.


INTEGRAL Bright Source Catalog
Source Type RA
(J2000.0)
DEC
(J2000.0)
ISGRI detections ISGRI results SPI average flux
[mCrab]
SPI highest flux
[mCrab]
SPI lowest flux
[mCrab]
SPI lightcurve Remarks on SPI analysis
V709 Cas CV 00 28 49 +59 17 22     4 ± 2   4 ± 2 X  
IGR J00370+6122 HMXB 00 37 06 +61 22 00     8 ± 2 8 ± 2 8 ± 2 X  
Gam Cas Be Star 00 56 43 +60 43 00     8 ± 1 11 ± 3 5 ± 2 X  
SMC X-1 HMXB 01 17 05 -73 26 36 35 23 ± 3 23 ± 3 22 ± 5 X  
3A 0114+650 HMXB 01 18 03 +65 17 30     13 ± 1 23 ± 3 6 ± 3 X  
4U 0115+634 HMXB 01 18 32 +63 44 24 6 X 11 ± 3 53 ± 13 4 ± 3 X  
RX J0146.9+6121 XRB 01 47 00 +61 21 24     13 ± 2 18 ± 4 9 ± 4 X  
NGC 1275 Sy2 03 19 48 +41 30 42     16 ± 3 15 ± 3 10 ± 10 X  
EXO 0331+530 HMXB 03 35 00 +53 10 24     290 ± 2 707 ± 6 29 ± 26 X V0332+53
X Per HMXB 03 55 23 +31 02 45 91 X       X  
LMC X-4 HMXB 05 32 50 -66 22 14 117 X 32 ± 1 79 ± 9 3 ± 2 X  
Crab SNR 05 34 32 +22 00 52 591 X 1000 ± 1 1059 ± 16 916 ± 24 X  
IGR J06074+2205 ? 06 07 18 +22 04 52 7 X 9 ± 1 33 ± 10 5 ± 2 X  
MRK 3 Sy2 06 15 36 +74 02 15     6 ± 2 8 ± 3 5 ± 2 X  
H 0614+091 LMXB 06 17 07 09 08 13 47 X 21 ± 2 67 ± 4 8 ± 3 X  
EXO 0748-676 LMXB 07 48 33 -67 45 00 47 X 19 ± 1 38 ± 13 6 ± 4 X  
Vela Pulsar Pulsar 08 35 21 -45 10 35     12 ± 1 59 ± 15 7 ± 3 X  
Ginga 0836-429 LMXB 08 37 25 -42 53 18 501 X 58 ± 1 81 ± 2 4 ± 2 X  
Vela X-1 HMXB 09 02 07 -40 33 17 572 X 199 ± 1 671 ± 17 17 ± 2 X  
MCG -05-23-16 Sy 1.9 09 47 40 -30 56 56 3         X  
GRO J1008-57 HMXB 10 09 46 -58 17 36     38 ± 3 48 ± 3 9 ± 9 X  
IGR J10109-5746 ? 10 10 50 -57 46 48     5 ± 2   2 ± 2 X  
Cen X-3 HMXB 11 21 16 -60 37 23 102 X 60 ± 1 140 ± 3 11 ± 9 X  
IGR J11305-6256 ? 11 30 30 -62 54 50     8 ± 2 48 ± 12 3 ± 3 X  
1E 1145.1-6141 HMXB 11 47 29 -61 57 14 80 X 33 ± 1 86 ± 5 5 ± 5 X  
NGC 4151 Sy 1.5 12 10 33 +39 24 21 157 X 37 ± 1 45 ± 9 6 ± 2 X  
NGC 4253 Sy 1.5 12 18 27 +29 48 46     7 ± 2   6 ± 3 X  
NGC 4388 Sy 2 12 25 47 +12 39 44 28 X 10 ± 2 13 ± 4 6 ± 6 X  
GX 301-2 HMXB 12 26 38 -62 46 13 290 X 116 ± 1 824 ± 7 25 ± 10 X  
3C 273 Blazar 12 29 07 +02 03 09 12 X 8 ± 1 16 ± 3 3 ± 3 X  
IGR J12349-6434 ? 12 34 54 -64 34 06     8 ± 1 29 ± 6 3 ± 3 X discovered June 2005
NGC 4507 Sy 2 12 35 37 -39 54 33     9 ± 2 14 ± 4 5 ± 3 X  
NGC 4593 Sy 1 12 39 39 -05 20 39     4 ± 1     X  
GX 304-1 HMXB 13 01 17.2 -61 36 07 0 11 ± 2 19 ± 4 7 ± 3 X  
1RXP J130159.6-635806 ? 13 01 59.6 -63 58 06     17 ± 7   11 ± 11 X  
NGC 4945 Sy 2 13 05 27 -49 28 06 10 X 13 ± 1 34 ± 8 7 ± 4 X  
Cen A Sy 2 13 25 28 -43 01 09 113 X 37 ± 1 209 ± 57 18 ± 12 X  
4U 1323-62 LMXB 13 26 36 -62 08 10           X has not been considered in SPI analysis
MCG-06-30-015 Sy 1 13 35 54 -34 17 43     5 ± 1 42 ± 14 4 ± 3 X  
4U 1344-60 AGN 13 47 25 -60 38 36     8 ± 2 9 ± 2 6 ± 2 X  
IC 4329A Sy 1.2 13 49 19 -30 18 36     13 ± 1 46 ± 13 6 ± 4 X  
Circinus gal. Sy 2 14 13 10 -65 20 21     13 ± 1 36 ± 11 8 ± 5 X  
NGC 5506 Sy 1.9 14 13 15 -03 12 27 11       X  
PSR B1509-58 Pulsar 15 13 56 -59 08 08     15 ± 3 68 ± 14 7 ± 3 X  
Cir X-1 LMXB 15 20 41 -57 10 01 105 X 17 ± 1 384 ± 104 4 ± 3 X 1516-569
H 1538-522 HMXB 15 42 23 -52 23 10 286 X 23 ± 1 51 ± 13 7 ± 5 X  
IGR J15479-4529 ? 15 47 54 -45 29 00 6 X 15 ± 2 24 ± 3 5 ± 4 X  
XTE J1550-564 LMXB 15 50 59 -56 28 36 136 X 124 ± 2 431 ± 96 10 ± 5 X  
H 1608-522 LMXB 16 12 43 -52 25 23 146 X 26 ± 1 226 ± 35 9 ± 3 X  
Sco X-1 LMXB 16 19 55 -15 38 25 452 X 466 ± 1 773 ± 37 224 ± 140 X  
IGR J16318-4848 HMXB 16 31 48 -48 49 01 333 X 40 ± 2 115 ± 26 10 ± 9 X  
IGR J16320-4751 HMXB 16 31 49 -48 49 00 187 X 48 ± 4 148 ± 27 21 ± 12 X  
4U 1626-67 LMXB 16 32 17 -67 27 43     18 ± 3 98 ± 16 8 ± 5 X  
4U 1630-47 LMXB 16 34 00 -47 23 39 464 X 55 ± 6 92 ± 23 24 ± 19 X  
IGRJ16358-4726 LMXB 16 35 54 -47 25 39 41 X 43 ± 2 299 ± 19 10 ± 8 X  
H 1636-536 LMXB 16 40 56 -53 45 05 287 X 38 ± 1 924 ± 243 12 ± 4 X  
IGR J16418-4532 LMXB 16 41 48 -45 32 00 2 X 15 ± 2   11 ± 7 X  
GX 340+0 LMXB 16 45 48 -45 36 40 560 X 36 ± 3 99 ± 17 21 ± 12 X  
IGR J16479-4514 ? 16 47 54 -45 14 00 20 X 31 ± 3 41 ± 5 10 ± 9 X  
NGC 6221 Sy1/2 16 52 46 -59 13 07 20 X 14 ± 4 28 ± 9 11 ± 4 X  
GRO J1655-40 LMXB 16 54 00 -39 50 45     10 ± 2 15 ± 5 5 ± 4 X  
IGR J16558-5203 ? 16 55 48 -52 03 00 0 X 11 ± 2 16 ± 3 4 ± 3 X has not been considered in SPI analysis before revolution 100
OAO 1657-415 HMXB 17 00 48 -41 40 23 1051 X 85 ± 1 177 ± 17 25 ± 11 X  
GX 339-4 LMXB 17 02 50 -48 47 23 216 X 46 ± 1 501 ± 58 5 ± 5 X  
4U1700-377 HMXB 17 03 57 -37 50 39 1434 X 160 ± 1 693 ± 19 31 ± 7 X  
GX 349+2 LMXB 17 05 45 -36 25 23 994 X 34 ± 1 72 ± 11 15 ± 7 X  
H 1702-429 LMXB 17 06 15 -43 02 10 297 X 38 ± 2 73 ± 11 10 ± 9 X  
H 1705-250 LMXB 17 08 15 -25 05 29 1 X 17 ± 1 49 ± 13 8 ± 3 X  
H 1705-440 LMXB 17 08 55 -44 06 00 307 X 47 ± 1 92 ± 3 16 ± 11 X  
IGR J17091-3624 XB 17 09 02 -36 23 38     28 ± 2 50 ± 7 16 ± 8 X  
XTE J1720-318 XB 17 19 58 -31 46 48 119 X 22 ± 1 137 ± 17 5 ± 3 X  
IGR J17252-3616 ? 17 25 12 -36 16 00 49 X 16 ± 1 38 ± 4 6 ± 4 X  
4U 1722-30 LMXB 17 27 33 -30 48 07 263 X 22 ± 1 91 ± 22 6 ± 5 X GRS 1724-308
IGR J17303-0601 ? 17 30 22 -05 59 34     78 ± 17 547 ± 161 64 ± 22 X  
3A 1728-169 LMXB 17 31 44 -16 57 42 36 X 16 ± 1 73 ± 12 6 ± 4 X GX 9+9
GX 354-0 LMXB 17 31 57 -33 50 05 1053 X 37 ± 1 130 ± 22 11 ± 7 X  
GX 1+4 LMXB 17 32 02 -24 44 44 1019 X 34 ± 1 127 ± 5 3 ± 3 X  
4U 1730-335 LMXB 17 33 24 -33 23 16 45 X 22 ± 2 77 ± 17 10 ± 6 X  
GRS 1734-292 Sy1 17 37 24 -29 10 48     20 ± 3 66 ± 10 14 ± 5 X AX J1737.4-2907
SLX 1735-269 LMXB 17 38 16 -27 00 16 17 X 15 ± 1 51 ± 11 5 ± 5 X  
4U 1735-444 LMXB 17 38 58 -44 27 00 372 X 22 ± 1 245 ± 41 6 ± 5 X  
IGR_J17391-3021 Be/NS binary ? 17 39 11 -30 20 38 16 X 21 ± 2 60 ± 10 11 ± 4 X  
GRS 1739-278 LMXB 17 42 37 -27 47 00 0 13 ± 1 73 ± 16 4 ± 3 X  
1E 1740.7-2942 LMXB 17 44 03 -29 43 25 602 X 71 ± 2 114 ± 5 33 ± 22 X source confusion
SAX J1744.7-2916 ? 17 44 42 -29 16 54 20 30 ± 7   28 ± 13 X has not been considered in SPI analysis before revolution 100
KS 1741-293 LMXB 17 44 49 -29 21 06 8 X 66 ± 44   66 ± 44 X  
1A 1742-294 LMXB 17 46 06 -29 30 55 203 X 52 ± 2 109 ± 6 13 ± 12 X source confusion
IGR J17464-3213 BHC 17 46 16 -32 14 01 435 X 38 ± 1 391 ± 34 5 ± 3 X  
GX 3+1 LMXB 17 47 56 -26 33 49 82 X 17 ± 1 36 ± 11 4 ± 3 X  
AX J1748.0-2829 LMXB 17 48 05 -28 28 26 4 26 ± 1 125 ± 27 5 ± 5 X J1748-288
IGR J17544-2619 HMXB 17 54 25 -26 19 53     18 ± 2 117 ± 27 9 ± 8 X  
AX J1758.0-2818 ? 17 58 00 -28 18 00     9 ± 1 20 ± 3 3 ± 3 X  
IGR J17597-2201 Neutron star 17 59 42 -22 01 00 9 X 22 ± 1 65 ± 12 6 ± 5 X  
GX 5-1 LMXB 18 01 08 -25 04 45 1164 X 44 ± 1 85 ± 7 18 ± 7 X source confusion with GRS 1758-258
GRS 1758-258 LMXB 18 01 12 -25 44 36 1075 X 65 ± 1 90 ± 6 12 ± 12 X source confusion with GX 5-1
GX 9+1 LMXB 18 01 32 -20 31 44 133 X 16 ± 1 73 ± 20 7 ± 4 X  
IGR J18027-1455 Sy1 18 02 47 -14 54 55     16 ± 2 85 ± 13 11 ± 10 X  
SAX J1805.5-2031 ? 18 05 34 -20 30 48 0 X 22 ± 1 48 ± 10 8 ± 7 X  
XTE J1807-294 Pulsar 18 07 00 -29 24 30 29 X 8 ± 2 11 ± 3 4 ± 4 X has not been considered in all SPI analyses
GX 13+1 LMXB 18 14 32 -17 09 27 142 X 26 ± 1 87 ± 18 10 ± 5 X 4U 1811-171
4U 1812-12 LMXB 18 15 12 -12 05 00 388 X 31 ± 1 482 ± 146 13 ± 12 X  
GX 17+2 LMXB 18 16 01 -14 02 11 867 X 43 ± 1 74 ± 14 16 ± 14 X  
AX J1820.5-1434 HMXB 18 20 30 -14 34 24 8 X 23 ± 4   19 ± 8 X has not been considered in all SPI analyses
H 1820-303 LMXB 18 23 40 -30 21 40 623 X 28 ± 1 169 ± 36 9 ± 4 X  
3A 1822-371 LMXB 18 25 47 -37 06 19 491 X 30 ± 1 142 ± 30 8 ± 5 X  
Ginga_1826-24 LMXB 18 29 28 -23 47 49 1206 X 80 ± 1 139 ± 46 23 ± 4 X  
IGR J18325-0756 ? 18 32 30 -07 56 00 3 X 15 ± 1 17 ± 3 7 ± 4 X  
XB 1832-330 LMXB 18 35 44 -32 58 55     12 ± 1 17 ± 4 7 ± 7 X  
PKS 1830-211 Blazar 18 33 40 -21 03 40     11 ± 1 19 ± 5 8 ± 3 X  
Ser X-1 LMXB 18 39 58 +05 02 09 18 X 13 ± 1 44 ± 13 7 ± 3 X  
IGR J18406-0539 ? 18 40 36 -05 39 00 0 X 5 ± 4   5 ± 4 X  
IGR J18450-0435 ? 18 45 00 -04 35 00 1 X 13 ± 2 25 ± 7 6 ± 4 X  
AX J1847.6-0219 ? 18 47 41 -02 19 00     23 ± 23   23 ± 23 X  
IGR J18483-0311 ? 18 48 18 -03 11 00 30 X 15 ± 1 35 ± 9 6 ± 4 X  
3A 1850+087 var. star 18 53 05 -08 42 20     15 ± 3 31 ± 7 8 ± 6 X  
V1223 Sgr CV 18 55 02 -31 09 48     10 ± 2 13 ± 4 5 ± 4 X  
XTE_J1855-026 HMXB 18 55 31 -02 36 24 91 X 23 ± 1 57 ± 5 10 ± 4 X  
XTE_J1858+034 HMXB 18 58 43 +03 26 06     83 ± 2 119 ± 12 60 ± 4 X  
4U 1901+03 HMXB 19 03 37 +03 11 31 638 X 70 ± 1 197 ± 27 13 ± 4 X  
XTE J1908+094 HMXB 19 08 53 +09 23 05 7 X 19 ± 4 26 ± 8 11 ± 10 X  
4U 1909+07 HMXB 19 10 53 +07 40 00 135 X 17 ± 1 31 ± 3 9 ± 6 X  
Aql X-1 LMXB 19 11 16 +00 35 06 107 X 24 ± 1 334 ± 108 5 ± 5 X  
SS 433 Microquasar 19 11 50 +04 58 58 179 X 16 ± 1 29 ± 6 5 ± 2 X  
IGR J19140+0951 XB 19 14 03 +09 53 18 90 X 20 ± 1 56 ± 5 5 ± 5 X source confusion with GRS 1915+105
GRS 1915+105 LMXB 19 15 12 +10 56 44 740 X 277 ± 1 452 ± 30 33 ± 25 X  
4U 1916-053 LMXB 19 18 48 -05 14 11 10 X 17 ± 2 18 ± 5 11 ± 6 X  
1H 1934-063 Sy1 19 37 33 -06 13 05     11 ± 5   10 ± 6 X  
KS 1947+300 HMXB 19 49 31 +30 12 24 57 X 17 ± 1 39 ± 8 7 ± 3 X  
Cyg X-1 HMXB 19 58 22 +35 12 06 278 X 664 ± 1 1102 ± 12 286 ± 6 X  
EXO 2030+375 HMXB 20 32 15 +37 38 15 110 X 57 ± 1 125 ± 3 6 ± 3 X  
Cyg X-3 XB 20 32 26 +40 57 28 316 X 152 ± 1 246 ± 11 75 ± 4 X  
MRK 509 Sy1 20 44 10 -10 43 25     6 ± 2     X  
SAX J2103.5+4545 HMXB 21 03 33 +45 45 00 89 X 28 ± 1 239 ± 80 6 ± 5 X  
IGR J21247+5058 radio galaxy? 21 24 39 +50 58 26     19 ± 1 74 ± 20 6 ± 4 X  
SS Cyg Dwarf Nova 21 42 43 +43 35 09     10 ± 2 11 ± 2 9 ± 3 X has not been considered in SPI analysis before revolution 190
Cyg X-2 LMXB 21 44 41 +38 19 18 56 X 21 ± 1 58 ± 5 6 ± 2 X  
3A 2206+543 HMXB 22 07 56 +54 31 06 19 X 25 ± 2 63 ± 18 6 ± 5 X  
MR2251-178 Sy 1 22 54 06 -17 34 55     4 ± 2   4 ± 2 X Analysis Results
Cas A SNR 23 23 24 +58 48 54     6 ± 1 32 ± 10 3 ± 2 X  

GPS combined image revolution 25-50