Revolution 1741: Observation start 2016-10-27T06:28 = MJD 57688.27
Total Observation GTI = 4832 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
==================== ======== ======= === ======== ======== ====== ===== ===== ====== ===== =====
GX 1+4 263.028 -24.756 2.0 1.937 +4.775 11.7 0.84 13.9 0.0 0.00 0.0
GX 5-1 270.309 -25.120 2.9 5.053 -1.058 7.5 0.84 8.9 0.0 0.00 0.0
KS 1741-293 266.169 -29.368 3.2 359.525 -0.050 5.9 0.73 8.0 2.3 0.42 5.6
AX J1820.5-1434 275.210 -14.630 3.9 16.462 -0.031 27.8 0.00 6.5 0.0 0.00 0.0
1E 1740.7-2942 265.976 -29.776 0.0 359.089 -0.120 4.3 0.00 5.5 3.0 0.00 6.6
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
==================== ======== ======= ======== ======== ====== ===== ===== ====== ===== =====
1A 1742-294 266.523 -29.515 359.559 -0.389 3.6 0.38 9.7 0.3 0.24 1.2
GX 3+1 266.983 -26.564 2.294 +0.794 14.9 0.39 38.0 0.6 0.22 2.5
GX 5-1 270.294 -25.076 5.085 -1.024 46.5 1.57 29.6 0.0 0.00 0.0
NEW SOURCE 268.430 -30.700 359.389 -2.414 3.8 0.59 6.5 0.0 0.00 0.0
SLX 1735-269 264.571 -26.994 0.796 +2.400 2.3 0.33 6.8 0.3 0.22 1.3
KS 1741-293 266.203 -29.339 359.564 -0.059 2.0 0.36 5.6 0.5 0.22 2.1
NEW SOURCE 264.879 -35.003 354.159 -2.093 17.2 1.73 9.9 4.3 1.36 3.2
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