INTEGRAL Galactic bulge Monitoring

Revolution 1655: Observation start 2016-03-12T10:34 = MJD 57459.441
Total Observation GTI = 12548 seconds

IBIS/ISGRI

1655_isgri_mosa1.jpg 1655_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  
==================== ========  ======= === ======== ======== ====== ===== ===== ====== ===== =====
4U 1700-377           255.988  -37.846 0.4  347.754   +2.172   87.9  0.90  97.9   29.6  0.49  60.2
IGR J17464-3213       266.573  -32.240 0.7  357.253   -1.842   29.6  0.54  54.3   16.5  0.32  52.4
GX 1+4                263.004  -24.752 0.7    1.929   +4.795   29.3  0.57  51.3    0.0  0.00   0.0
GRS 1758-258          270.311  -25.757 1.3    4.500   -1.375   11.9  0.54  22.1    6.9  0.31  22.5
IGR J17091-3624       257.277  -36.408 1.4  349.522   +2.215   15.1  0.74  20.3   10.4  0.41  25.1
GX 354-0              262.981  -33.855 1.8  354.282   -0.156    7.4  0.47  15.7    1.8  0.28   6.3
1E 1740.7-2942        265.986  -29.771 2.0  359.097   -0.125    6.0  0.44  13.5    3.2  0.27  11.8
H 1820-303            275.947  -30.375 2.5    2.787   -7.942    9.3  0.88  10.6    0.0  0.00   0.0
GX 349+2              256.440  -36.397 2.9  349.126   +2.761    6.8  0.75   9.1    0.0  0.00   0.0
SLX 1735-269          264.584  -26.992 3.1    0.804   +2.392    4.1  0.49   8.2    1.6  0.29   5.4
4U 1722-30            261.885  -30.821 3.6  356.302   +2.289    3.7  0.53   7.0    0.0  0.00   0.0
Swift J175759.9-2246  269.487  -22.669 3.8    6.805   +0.813    4.5  0.67   6.7    0.0  0.00   0.0
SLX 1744-299_300      266.829  -30.031 0.0  359.256   -0.884    3.1  0.00   6.9    1.3  0.00   4.9
3A 1822-371           276.417  -37.063 3.7  356.879  -11.253    6.3  0.92   6.8    0.0  0.00   0.0
GX 5-1                270.393  -25.100 4.8    5.108   -1.115    2.9  0.56   5.2    0.0  0.00   0.0
SAX J1752.3-3138      268.007  -31.661 0.0  358.376   -2.588    3.0  0.00   5.3    0.0  0.00   0.0
IGR J17456-2901       266.363  -28.976 6.2  359.947   +0.011    1.9  0.49   3.9    0.0  0.00   0.0
GRS 1734-292          264.466  -29.057 5.6  359.002   +1.376    2.1  0.48   4.4    0.0  0.00   0.0
IGR J18173-2509       274.331  -25.115 5.0    6.817   -4.246    3.6  0.73   5.0    0.0  0.00   0.0
IGR J16558-4150       254.094  -41.838 5.3  343.713   +0.856    7.9  0.00   4.6    0.0  0.00   0.0

JEM-X

1655_jemx_mosa1.jpg 1655_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           266.515  -29.511  359.559   -0.382    6.1  0.39  15.7    0.7  0.28   2.6
1E 1740.7-2942        265.978  -29.745  359.116   -0.106    1.4  0.36   4.0    0.9  0.28   3.1
GRS 1758-258          270.303  -25.741    4.511   -1.361    8.7  2.56   3.4    0.0  0.00   0.0
GX 3+1                266.982  -26.574    2.284   +0.789   15.1  0.71  21.3    0.9  0.47   2.0
GX 354-0              262.989  -33.835  354.302   -0.150    7.4  0.80   9.2    1.8  0.68   2.6
GX 5-1                270.289  -25.084    5.075   -1.024  103.9  5.13  20.2    8.6  3.31   2.6
IGR J17464-3213       266.567  -32.229  357.260   -1.832    7.7  0.46  16.6    3.9  0.36  10.7
Swift J174535.5-2901  266.398  -29.026  359.920   -0.042    1.7  0.39   4.4    0.0  0.00   0.0
SAX J1750.8-2900      267.596  -29.045    0.445   -0.948    1.9  0.43   4.4    0.0  0.00   0.0
NEW SOURCE            272.147  -27.053    4.173   -3.443   14.2  4.06   3.5    3.7  3.66   1.0
NEW SOURCE            270.021  -25.665    4.450   -1.102    7.6  2.41   3.2    0.0  0.00   0.0


Go back to the INTEGRAL Galactic bulge home page