INTEGRAL Galactic bulge Monitoring
Revolution 0599: Observation start 2007-09-09T08:18 = MJD 54352.347
Total Observation GTI = 12300 seconds
IBIS/ISGRI
IBIS/ISGRI significance mosaic images. Left: IBIS/ISGRI 18-40 keV. Right: 40-100 keV
Sources detected > 10σ in each band are marked on the image. The table below lists the fitted position, and statistical positional uncertainty in arcmin returned by the mosaic step of
OSA10.1, of all the sources detected in the 18 - 40 keV range (band A: 1 Crab ~ 208 cps ) and 40 - 100 keV range (band B: 1 Crab ~ 100 cps ) where available.NOTES: The table is constructed from the
isgri_mosa_res.fits file - fluxes in the mosaic output are known to be systematically ~10% lower than in the ScW light-curves (see known issues). The systematic noise increases towards the edge of the field of view and NEW SOURCEs < 6σ towards the border of the image may be spurious. IBIS/ISGRI Detected Sources 18-40 keV (A) and 40-100 keV (B)
Source Name RA dec +/- l b A(cps) +/- sig B(cps) +/- sig ==================== ======== ======= === ======== ======== ====== ===== ===== ====== ===== ===== GX 1+4 263.003 -24.746 1.0 1.934 +4.800 13.0 0.40 32.7 0.0 0.00 0.0 GX 349+2 256.444 -36.438 1.1 349.096 +2.734 18.3 0.63 29.2 0.0 0.00 0.0 Ginga 1826-24 277.363 -23.803 1.1 9.265 -6.087 17.4 0.62 28.0 6.8 0.49 13.9 H 1820-303 275.925 -30.347 1.2 2.804 -7.912 11.8 0.47 25.2 0.0 0.00 0.0 4U 1722-30 261.875 -30.795 1.7 356.319 +2.311 5.6 0.34 16.5 1.2 0.28 4.3 GX 3+1 267.008 -26.555 2.2 2.313 +0.779 3.7 0.30 12.1 0.0 0.00 0.0 3A 1822-371 276.426 -37.114 2.4 356.835 -11.281 6.9 0.62 11.1 0.0 0.00 0.0 SAX J1810.8-2609 272.657 -26.149 2.4 5.186 -3.408 4.9 0.44 11.2 2.6 0.36 7.2 OAO 1657-415 255.210 -41.646 2.3 344.380 +0.321 17.8 1.53 11.7 0.0 0.00 0.0 GX 5-1 270.301 -25.078 3.0 5.086 -1.031 3.4 0.39 8.8 0.0 0.00 0.0 GX 9+1 270.367 -20.583 3.0 9.022 +1.141 4.1 0.47 8.6 0.0 0.00 0.0 GX 13+1 273.638 -17.191 3.0 13.490 +0.085 7.0 0.80 8.7 0.0 0.00 0.0 GX 17+2 274.086 -14.036 3.1 16.469 +1.210 24.3 2.94 8.3 0.0 0.00 0.0 SLX 1735-269 264.541 -27.040 3.3 0.743 +2.398 2.5 0.31 7.9 0.0 0.00 0.0 IGR J17252-3616 261.336 -36.251 3.7 351.540 -0.362 3.2 0.46 6.9 0.0 0.00 0.0 H 1702-429 256.575 -43.064 3.6 343.870 -1.342 15.0 2.10 7.2 0.0 0.00 0.0 GX 354-0 263.005 -33.865 3.4 354.284 -0.177 2.8 0.37 7.6 0.0 0.00 0.0 GRS 1758-258 270.323 -25.738 3.8 4.523 -1.375 2.5 0.37 6.6 1.3 0.31 4.2 GRS 1734-292 264.392 -29.165 4.6 358.876 +1.373 1.7 0.31 5.4 0.0 0.00 0.0 1E 1742.8-2853 266.556 -28.931 4.7 0.073 -0.110 1.5 0.28 5.3 0.0 0.00 0.0 1A 1742-294 266.552 -29.467 5.6 359.613 -0.386 1.3 0.29 4.3 0.0 0.00 0.0 4U 1700-377 255.952 -37.807 5.3 347.767 +2.217 3.2 0.69 4.6 0.0 0.00 0.0 1RXS J180408.9-34205 271.180 -34.337 5.5 357.364 -6.225 1.8 0.40 4.4 0.0 0.00 0.0 SAX J1712.6-3739 258.115 -37.756 5.4 348.831 +0.879 2.8 0.61 4.6 0.0 0.00 0.0 3A 1728-169 262.919 -16.953 5.1 8.513 +9.055 3.7 0.78 4.8 0.0 0.00 0.0 SGR 1806-20 272.142 -20.364 5.6 10.027 -0.201 2.3 0.53 4.3 0.0 0.00 0.0 IGR J17098-3628 257.384 -36.452 6.0 349.537 +2.120 2.4 0.58 4.1 2.1 0.47 4.5 IGR J17379-3747 264.448 -37.723 6.5 351.669 -3.248 1.9 0.00 3.7 0.0 0.00 0.0 Oph Cluster 258.107 -23.361 7.5 0.576 +9.281 1.6 0.50 3.2 0.0 0.00 0.0 Swift J1734.5-3027 263.676 -30.424 7.0 357.480 +1.219 1.2 0.34 3.4 0.0 0.00 0.0 IGR J17559-2612 269.096 -26.232 7.7 3.543 -0.665 1.0 0.34 3.1 0.0 0.00 0.0 IGR J17088-4008 257.264 -40.061 6.5 346.582 +0.046 3.2 0.85 3.7 0.0 0.00 0.0
JEM-X
JEM-X1 significance mosaic images. Left: 3-10 keV. Right: 10-25 keV.
Sources labelled were detected in the 3-10 keV image > 6σ. The sources detected above 3σ in the 3-10 keV and/or 10-25 keV band are listed in the table below. Fluxes are extracted at the known catalogue position of the source (i.e. no fitting of the source position is done), with
mosaic_spec, in two bands: A = 3-10 keV (1 Crab ~ 97 cps [J1], 103 cps [J2]); B = 10-25 keV (1 Crab ~ 29 cps [J1], 27 cps [J2]). NOTES: The object marked as SLX 1744-299_300 is used to indicate two low-mass x-ray binaries separated by 2.7 arcminutes, SLX 1744-299 and SLX 1744-300; the position for SLX 1744-299 is used, although it can not be ruled out that SLX 1744-300 may dominate the emission some of the time. The systematic noise increases towards the edge of the field of view and in the vicinity of very bright sources, such as GX 5-1;
NEW SOURCEs < 6σ towards the border of the image and/or near GX 5-1 may, therefore, be spurious.
JEM-X1 Detected Sources in 3-10 keV (A) and 10-25 keV (B).
Source Name RA dec l b A(cps) +/- sig B(cps) +/- sig ==================== ======== ======= ======== ======== ====== ===== ===== ====== ===== ===== 1A 1742-294 266.523 -29.515 359.559 -0.389 6.9 0.29 23.5 1.2 0.18 7.0 4U 1722-30 261.888 -30.802 356.320 +2.298 3.0 0.62 4.8 1.3 0.48 2.6 GX 3+1 266.982 -26.563 2.294 +0.795 39.5 0.49 81.2 4.2 0.25 16.9 GX 354-0 262.989 -33.835 354.302 -0.150 12.2 1.24 9.8 1.5 0.99 1.5 GX 5-1 270.283 -25.074 5.081 -1.015 90.1 1.69 53.4 4.9 0.74 6.7 SLX 1744-299_300 266.858 -29.999 359.297 -0.889 2.0 0.29 6.9 0.6 0.19 3.0 NEW SOURCE 270.154 -26.147 4.091 -1.445 4.0 0.84 4.7 0.0 0.00 0.0