INTEGRAL Galactic bulge Monitoring

Revolution 1656: Observation start 2016-03-15T02:22 = MJD 57462.099
Total Observation GTI = 12479 seconds

IBIS/ISGRI

1656_isgri_mosa1.jpg 1656_isgri_mosa2.jpg

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                263.008  -24.743 0.7    1.939   +4.797   33.5  0.66  50.6    0.0  0.00   0.0
IGR J17464-3213       266.575  -32.236 0.8  357.257   -1.842   28.0  0.64  43.9   13.8  0.34  40.4
GX 354-0              263.002  -33.838 1.3  354.305   -0.161   13.0  0.58  22.3    3.1  0.31   9.9
IGR J17091-3624       257.284  -36.427 1.5  349.510   +2.200   19.9  1.02  19.5    9.4  0.51  18.4
GRS 1758-258          270.318  -25.755 1.8    4.505   -1.380   11.3  0.72  15.7    6.8  0.36  19.2
4U 1700-377           256.004  -37.790 2.9  347.806   +2.196    9.7  1.09   8.9    4.2  0.55   7.7
H 1820-303            275.958  -30.390 2.8    2.777   -7.956    9.4  1.00   9.4    0.0  0.00   0.0
1E 1740.7-2942        265.927  -29.752 2.9  359.087   -0.072    5.6  0.63   9.0    2.6  0.33   7.7
GX 349+2              256.443  -36.515 0.0  349.033   +2.688    6.9  0.00   6.9    0.0  0.00   0.0
3A 1822-371           276.454  -37.095 3.1  356.862  -11.293   10.7  1.27   8.4    0.0  0.00   0.0
SLX 1735-269          264.570  -27.001 3.8    0.789   +2.397    3.9  0.00   6.6    1.3  0.31   4.2
GX 3+1                266.869  -26.497 0.0    2.297   +0.916    3.6  0.00   6.4    0.0  0.00   0.0
IGR J18214-1318       275.414  -13.397 4.6   17.643   +0.375   96.2 17.72   5.4    0.0  0.00   0.0
SLX 1744-299_300      266.858  -30.012 3.6  359.285   -0.896    4.7  0.67   7.0    0.0  0.00   0.0
GX 5-1                270.367  -25.019 4.7    5.166   -1.054    4.2  0.00   5.3    0.0  0.00   0.0
SAX J1750.8-2900      267.570  -28.953 4.8    0.513   -0.881    2.9  0.00   5.2    0.0  0.00   0.0
Oph Cluster           258.036  -23.341 5.6    0.554   +9.346    3.8  0.86   4.4    0.0  0.00   0.0
AX J1749.1-2733       267.241  -27.490 5.9    1.619   +0.119    2.9  0.69   4.1    0.0  0.00   0.0
2E 1701.9-3723        256.462  -37.400 0.0  348.337   +2.142    5.4  0.00   4.8    0.0  0.00   0.0
SAX J1712.6-3739      258.268  -37.678 0.0  348.966   +0.827    4.4  0.00   4.8    0.0  0.00   0.0
GX 9+1                270.509  -20.499 6.2    9.161   +1.067    4.2  1.07   3.9    0.0  0.00   0.0

JEM-X

1656_jemx_mosa1.jpg 1656_jemx_mosa2.jpg

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    0.9  0.12   7.3    0.2  0.10   1.6
1E 1740.7-2942        265.978  -29.745  359.116   -0.106    0.4  0.12   3.0    0.2  0.10   1.6
GX 1+4                263.009  -24.746    1.937   +4.795    0.9  0.41   2.3    1.4  0.45   3.2
GX 3+1                266.983  -26.564    2.294   +0.794    1.5  0.18   8.4    0.2  0.17   1.1
GX 354-0              262.989  -33.835  354.302   -0.150    7.1  0.77   9.2    1.2  0.62   1.9
GX 5-1                270.284  -25.079    5.077   -1.019  117.3  3.58  32.8    6.4  1.44   4.4
IGR J17464-3213       266.564  -32.238  357.250   -1.834    2.3  0.22  10.5    0.6  0.19   3.1


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