INTEGRAL Galactic bulge Monitoring

Revolution 0293: Observation start 1999-12-31T23:58 = MJD 51544
Total Observation GTI = 8509 seconds

IBIS/ISGRI

0293_isgri_mosa1.jpg 0293_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           255.979  -37.841 0.5  347.753   +2.180   49.6  0.70  70.4   12.1  0.56  21.4
GRO J1655-40          253.494  -39.848 1.0  344.977   +2.458   36.6  1.24  29.5   26.8  0.91  29.4
1E 1740.7-2942        265.971  -29.763 1.0  359.097   -0.110   10.6  0.36  29.4    6.5  0.30  22.0
GRS 1758-258          270.307  -25.754 1.0    4.501   -1.370   12.1  0.39  30.8    7.3  0.33  22.3
Ginga 1826-24         277.380  -23.806 1.3    9.269   -6.102   15.7  0.71  22.0    4.9  0.53   9.3
GX 349+2              256.428  -36.415 1.6  349.107   +2.758   11.6  0.63  18.3    0.0  0.00   0.0
GX 354-0              262.985  -33.841 1.7  354.295   -0.150    6.6  0.39  17.0    0.0  0.00   0.0
1A 1742-294           266.547  -29.510 2.1  359.575   -0.404    4.8  0.37  12.9    2.0  0.33   6.0
GX 1+4                262.992  -24.745 1.9    1.929   +4.808    5.9  0.41  14.3    0.0  0.00   0.0
GX 5-1                270.312  -25.035 2.3    5.128   -1.019    4.3  0.37  11.5    0.0  0.00   0.0
4U 1722-30            261.873  -30.860 2.6  356.264   +2.277    3.6  0.36  10.0    0.0  0.00   0.0
GX 9+1                270.395  -20.513 2.8    9.096   +1.153    4.9  0.53   9.2    0.0  0.00   0.0
H 1820-303            275.904  -30.372 2.8    2.773   -7.907    4.9  0.52   9.4    0.0  0.00   0.0
GX 3+1                267.009  -26.532 3.4    2.333   +0.790    2.7  0.36   7.5    0.0  0.00   0.0
3A 1822-371           276.466  -37.099 3.6  356.863  -11.304    6.1  0.85   7.2    0.0  0.00   0.0
SLX 1735-269          264.570  -27.025 3.9    0.769   +2.384    2.5  0.38   6.5    1.6  0.31   5.1
3A 1728-169           262.944  -16.941 4.1    8.536   +9.041    4.4  0.70   6.2    0.0  0.00   0.0
GX 17+2               273.986  -14.051 5.5   16.410   +1.288   13.4  2.97   4.5    0.0  0.00   0.0
1E 1742.8-2853        266.539  -28.988 0.0    0.017   -0.127    1.8  0.00   5.0    0.0  0.00   0.0
IGR J17407-2808       265.231  -28.148 5.4    0.129   +1.292    1.8  0.39   4.5    0.0  0.00   0.0
SLX 1744-299_300      266.866  -30.072 6.9  359.238   -0.933    1.3  0.38   3.5    0.0  0.00   0.0

JEM-X

0293_jemx_mosa1.jpg 0293_jemx_mosa2.jpg

JEM-X1 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 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    2.0  0.29   7.1    0.6  0.16   3.6
1E 1740.7-2942        265.978  -29.745  359.116   -0.106    2.6  0.28   9.2    1.0  0.16   6.2
4U 1722-30            261.888  -30.802  356.320   +2.298    1.8  0.45   4.1    0.8  0.29   2.7
GRS 1741.9-2853       266.260  -28.914  359.953   +0.120    1.0  0.27   3.8    0.0  0.00   0.0
GX 3+1                266.981  -26.562    2.294   +0.796   26.0  0.39  66.2    2.9  0.18  15.9
GX 354-0              262.995  -33.828  354.310   -0.151   19.2  1.35  14.2    4.4  0.93   4.7
GX 5-1                270.286  -25.076    5.081   -1.019  110.9  1.70  65.4    9.4  0.74  12.7
SLX 1744-299_300      266.858  -29.999  359.297   -0.889    2.5  0.33   7.8    0.4  0.18   1.9
NEW SOURCE            271.711  -26.679    4.312   -2.922    9.1  1.62   5.6    0.0  0.00   0.0
NEW SOURCE            269.973  -25.473    4.595   -0.969    5.3  1.01   5.2    0.0  0.00   0.0
NEW SOURCE            271.863  -26.887    4.195   -3.142    6.9  1.61   4.3    0.0  0.00   0.0
NEW SOURCE            270.690  -27.409    3.229   -2.485    4.1  0.77   5.2    0.4  0.39   1.0
NEW SOURCE            268.798  -23.840    5.474   +0.773    7.1  1.40   5.1    0.0  0.00   0.0
NEW SOURCE            271.542  -26.818    4.117   -2.858    7.2  1.41   5.1    0.6  0.63   1.0


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