INTEGRAL Galactic Bulge Monitoring Revolution 0485: Observation start 2006-10-03 = MJD 54011
Total Observation GTI = 12398 seconds
ISGRI
ISGRI significance mosaic images. Left: ISGRI 18-40 keV. Right: 40-100 keVSources 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
OSA7
, of all the sources detected in the 18 - 40 keV range (band A: 1 Crab ~ 206 cps ) and 40 - 100 keV range (band B: 1 Crab ~ 103 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 andNEW
sources < 6σ towards the border of the image may be spurious.
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+4 263.013 -24.743 0.7 1.941 +4.794 16.4 0.33 49.1 0.0 0.00 0.0 GX 5-1 270.280 -25.078 0.8 5.076 -1.014 13.3 0.31 42.3 0.9 0.25 3.4 IGR J17497-2821 267.414 -28.356 0.9 0.955 -0.458 11.6 0.32 36.6 8.2 0.27 30.6 Ginga 1826-24 277.378 -23.793 1.0 9.280 -6.095 17.9 0.56 31.9 6.6 0.43 15.2 GRS 1758-258 270.313 -25.734 1.2 4.522 -1.365 7.6 0.31 24.4 5.4 0.25 21.5 1E 1740.7-2942 265.985 -29.746 1.3 359.119 -0.111 7.4 0.32 23.3 5.4 0.27 20.1 H 1820-303 275.916 -30.345 1.4 2.802 -7.904 9.1 0.44 20.8 0.0 0.00 0.0 4U 1722-30 261.887 -30.795 1.9 356.325 +2.303 4.5 0.30 14.8 1.6 0.24 6.6 GX 354-0 262.994 -33.841 1.8 354.299 -0.157 5.1 0.33 15.7 0.0 0.00 0.0 IGR J17252-3616 261.292 -36.260 2.0 351.513 -0.338 5.9 0.43 13.6 0.0 0.00 0.0 1A 1742-294 266.526 -29.517 2.4 359.559 -0.392 3.3 0.29 11.3 0.0 0.00 0.0 SLX 1735-269 264.550 -27.005 2.2 0.777 +2.410 3.4 0.28 12.2 0.0 0.00 0.0 GX 349+2 256.447 -36.414 2.4 349.116 +2.747 6.3 0.57 11.1 0.0 0.00 0.0 3A 1822-371 276.433 -37.102 2.7 356.849 -11.281 5.9 0.61 9.7 0.0 0.00 0.0 GX 3+1 267.012 -26.588 2.7 2.286 +0.759 3.0 0.31 9.6 0.0 0.00 0.0 GX 9+1 270.416 -20.556 3.0 9.068 +1.115 3.7 0.42 8.7 0.0 0.00 0.0 XB 1832-330 278.880 -33.001 4.4 1.502 -11.336 3.5 0.61 5.7 0.0 0.00 0.0 3A 1728-169 262.925 -16.971 5.5 8.500 +9.040 3.1 0.69 4.5 0.0 0.00 0.0 SLX 1744-299_300 266.845 -29.965 5.3 359.319 -0.862 1.5 0.32 4.6 1.0 0.00 3.7 SLX 1737-282 265.197 -28.340 5.2 359.951 +1.215 1.5 0.31 4.7 0.0 0.00 0.0 GX 13+1 273.619 -17.113 0.0 13.550 +0.138 2.9 0.00 3.8 0.0 0.00 0.0 GRS 1734-292 264.324 -29.152 6.6 358.855 +1.430 1.0 0.28 3.6 0.0 0.00 0.0 IGR J18027-2016 270.733 -20.297 0.0 9.439 +0.984 1.6 0.00 3.7 0.0 0.00 0.0 Oph Cluster 258.064 -23.289 6.7 0.612 +9.355 1.6 0.00 3.6 0.0 0.00 0.0JEM-X
JEM-X significance mosaic images. Left: 3-10 keV. Right: 10-25 keV.Note: Sources labelled were detected with in the 3-10 keV image > 5σ and 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 ~ 88 cps); B = 10-25 keV (1 Crab ~ 32 cps).NOTE: 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.
JEM-X Detected Sources in 3-10 keV (A) and 10-25 keV (B).Source Name RA dec l b A(cps) +/- B(cps) +/- ==================== ======== ======== ======== ======== ====== ===== ====== ===== 1E 1740.7-2942 265.978 -29.745 359.116 -0.106 2.1 0.38 1.2 0.25 GX 354-0 262.989 -33.835 354.302 -0.150 19.2 1.52 4.2 0.98 1A 1742-294 266.523 -29.515 359.559 -0.389 1.7 0.31 0.6 0.20 GX 3+1 266.983 -26.564 2.294 +0.794 24.2 0.57 3.4 0.31 GX 5-1 270.284 -25.079 5.077 -1.019 103.2 2.26 15.9 1.05 IGR J17497-2821 267.404 -28.358 0.949 -0.451 2.1 0.39 0.9 0.23
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