INTEGRAL Galactic bulge Monitoring

Revolution 1082: Observation start 2011-08-26T09:02 = MJD 55799.377
Total Observation GTI = 13226 seconds

IBIS/ISGRI

1082_isgri_mosa1.jpg 1082_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           255.985  -37.855 0.6  347.746   +2.168   53.4  0.83  64.7   17.1  0.60  28.6
Ginga 1826-24         277.366  -23.791 1.2    9.277   -6.083   13.5  0.52  26.0    4.9  0.39  12.7
1E 1740.7-2942        265.981  -29.742 1.4  359.120   -0.106    6.6  0.32  20.3    4.6  0.27  17.2
GRS 1758-258          270.317  -25.758 1.9    4.502   -1.380    5.2  0.36  14.6    4.2  0.28  14.8
IGR J17498-2921       267.486  -29.324 2.3    0.156   -1.009    3.5  0.30  11.8    1.9  0.24   7.9
GX 354-0              263.039  -33.835 3.3  354.325   -0.185    3.0  0.39   7.7    0.0  0.00   0.0
GX 3+1                266.964  -26.582 2.9    2.270   +0.799    2.9  0.31   9.1    0.0  0.00   0.0
H 1820-303            275.889  -30.362 3.2    2.775   -7.891    3.8  0.47   8.0    0.0  0.00   0.0
4U 1722-30            261.882  -30.801 3.3  356.317   +2.303    2.8  0.36   7.9    1.6  0.28   5.9
3A 1822-371           276.432  -37.105 3.2  356.846  -11.281    5.2  0.65   8.0    0.0  0.00   0.0
GX 5-1                270.367  -25.104 3.5    5.093   -1.096    2.6  0.36   7.4    0.0  0.00   0.0
1E 1742.9-2849        266.526  -28.801 3.8    0.170   -0.020    1.9  0.29   6.7    0.0  0.00   0.0
GX 1+4                262.991  -24.715 3.6    1.955   +4.825    2.5  0.35   7.1    0.0  0.00   0.0
GX 17+2               273.943  -14.051 0.0   16.390   +1.324    7.7  0.00   6.0    0.0  0.00   0.0
GX 9+1                270.368  -20.576 4.1    9.028   +1.144    2.8  0.45   6.2    0.0  0.00   0.0
GX 349+2              256.473  -36.431 5.2  349.115   +2.720    3.3  0.69   4.8    0.0  0.00   0.0
IGR J17445-2747       266.127  -27.829 4.1    0.817   +0.787    1.8  0.30   6.2    0.0  0.00   0.0
IGR J17511-3057       267.807  -31.032 4.8  358.831   -2.121    1.6  0.31   5.2    0.0  0.00   0.0
IGR J17091-3624       257.205  -36.357 5.0  349.528   +2.292    3.0  0.60   4.9    0.0  0.00   0.0
1A 1744-361           267.188  -36.090 5.4  354.212   -4.263    2.0  0.44   4.5    0.0  0.00   0.0
GX 13+1               273.674  -17.112 5.2   13.575   +0.092    3.1  0.65   4.8    0.0  0.00   0.0

JEM-X

1082_jemx_mosa1.jpg 1082_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           266.536  -29.492  359.584   -0.387    7.6  0.27  28.3    1.1  0.14   7.6
1E 1740.7-2942        265.978  -29.745  359.116   -0.106    1.8  0.29   6.2    0.9  0.16   5.7
1E 1743.1-2843        266.587  -28.729    0.260   -0.029    1.0  0.26   3.8    0.4  0.14   2.8
4U 1722-30            261.888  -30.802  356.320   +2.298    2.8  0.81   3.5    0.0  0.00   0.0
GX 3+1                266.985  -26.563    2.295   +0.793    0.0  0.00   0.0    5.7  0.15  37.7
GX 5-1                270.286  -25.076    5.081   -1.018  110.7  0.82 135.5    7.8  0.33  23.4
SLX 1735-269          264.571  -26.994    0.796   +2.400    1.3  0.31   4.3    0.0  0.00   0.0
SLX 1744-299_300      266.858  -29.999  359.297   -0.889    1.0  0.28   3.6    0.3  0.16   2.0
NEW SOURCE            268.656  -24.918    4.478   +0.340    3.1  0.53   5.8    0.0  0.00   0.0
NEW SOURCE            269.213  -24.516    5.080   +0.105    3.4  0.65   5.2    0.4  0.30   1.5
NEW SOURCE            269.682  -33.352  357.619   -4.658    5.6  1.04   5.4    1.0  0.73   1.4
NEW SOURCE            271.931  -26.284    4.754   -2.903    4.6  0.85   5.4    0.7  0.44   1.6
IGR J17498-2921       267.476  -29.317    0.158   -0.998    1.0  0.27   3.9    0.6  0.14   4.5


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