Revolution 1858: Observation start 2017-09-03T07:29 = MJD 57999.312
Total Observation GTI = 1972 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 SOURCE
s < 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
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GX 5-1 270.296 -25.074 2.3 5.087 -1.025 18.4 1.61 11.4 0.0 0.00 0.0
GX 354-0 262.997 -33.834 2.2 354.306 -0.155 20.8 1.71 12.2 5.7 0.74 7.7
GRS 1758-258 270.320 -25.743 3.0 4.516 -1.376 13.3 1.53 8.7 5.5 0.70 7.8
1E 1740.7-2942 265.965 -29.729 2.9 359.123 -0.087 18.3 2.04 9.0 9.7 0.81 12.0
3A 1822-371 276.438 -37.156 0.0 356.801 -11.307 16.6 0.00 6.0 0.0 0.00 0.0
SAX J1818.6-1703 274.715 -16.846 4.3 14.283 -0.657 33.5 5.76 5.8 0.0 0.00 0.0
IGR J17464-3213 266.540 -32.131 3.7 357.332 -1.762 10.5 1.54 6.8 4.9 0.71 7.0
IGR J18027-2016 270.677 -20.401 4.5 9.323 +0.979 12.4 0.00 5.5 0.0 0.00 0.0
Swift J175759.9-2246 269.537 -22.784 4.5 6.728 +0.717 11.4 2.03 5.6 0.0 0.00 0.0
GX 3+1 266.937 -26.572 4.7 2.265 +0.824 7.7 1.44 5.3 0.0 0.00 0.0
IGR J17404-3655 265.161 -36.887 6.0 352.681 -3.284 8.3 2.05 4.1 0.0 0.00 0.0
GRS 1716-249 259.933 -25.102 5.0 0.087 +6.921 9.7 1.98 4.9 4.8 0.89 5.4
IGR J17536-2339 268.431 -23.600 4.9 5.511 +1.183 9.9 1.94 5.1 0.0 0.00 0.0
V745 Sco 268.952 -33.267 0.0 357.389 -4.087 6.8 0.00 4.3 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 SOURCE
s < 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
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