INTEGRAL Galactic bulge Monitoring
Revolution 1802: Observation start 2017-04-07T09:38 = MJD 57850.402
Total Observation GTI = 2022 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 ==================== ======== ======= === ======== ======== ====== ===== ===== ====== ===== ===== GRS 1716-249 259.885 -25.007 1.1 0.141 +7.011 152.2 5.69 26.7 68.1 2.83 24.1 GX 1+4 262.980 -24.744 2.3 1.924 +4.818 60.6 5.17 11.7 0.0 0.00 0.0 GX 3+1 266.992 -26.443 4.7 2.402 +0.849 25.0 0.00 5.3 0.0 0.00 0.0 IGR J17445-2747 266.169 -27.680 5.9 0.963 +0.833 21.3 5.14 4.1 0.0 0.00 0.0
JEM-X
JEM-X1+2 combined 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+2 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 1.9 0.34 5.5 0.6 0.36 1.6 1E 1740.7-2942 265.978 -29.745 359.116 -0.106 1.2 0.33 3.5 1.4 0.38 3.6 GX 1+4 263.009 -24.746 1.937 +4.795 2.1 0.58 3.7 1.8 0.61 2.9 GX 3+1 266.990 -26.578 2.284 +0.782 8.1 0.34 23.7 1.5 0.35 4.5 GX 5-1 270.281 -25.086 5.070 -1.020 125.1 1.94 64.5 15.4 1.06 14.5 SLX 1744-299_300 266.858 -29.999 359.297 -0.889 1.3 0.38 3.5 0.5 0.38 1.2 NEW SOURCE 271.669 -26.392 4.544 -2.750 9.6 2.20 4.3 0.0 0.00 0.0 NEW SOURCE 271.656 -27.197 3.835 -3.131 7.7 1.82 4.2 0.0 0.00 0.0 NEW SOURCE 271.389 -25.943 4.815 -2.311 10.2 2.28 4.5 1.6 1.36 1.2 NEW SOURCE 270.968 -25.595 4.933 -1.811 8.7 1.99 4.4 0.0 0.00 0.0 NEW SOURCE 270.003 -24.750 5.237 -0.634 6.2 1.61 3.9 0.9 0.92 1.0 NEW SOURCE 270.606 -25.225 5.095 -1.344 6.3 1.76 3.6 1.3 1.03 1.3 NEW SOURCE 271.322 -28.979 2.131 -3.738 5.4 1.48 3.6 0.0 0.00 0.0 NEW SOURCE 272.559 -25.715 5.525 -3.122 16.8 5.01 3.4 0.0 0.00 0.0