INTEGRAL Galactic bulge Monitoring

Revolution 0853: Observation start 1999-12-31T23:58 = MJD 51544
Total Observation GTI = 9657 seconds

IBIS/ISGRI

0853_isgri_mosa1.jpg 0853_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           255.990  -37.847 0.6  347.754   +2.170   53.1  0.79  67.2   14.2  0.60  23.6
1E 1740.7-2942        265.981  -29.745 1.0  359.118   -0.108   12.5  0.42  29.9    8.0  0.36  22.4
GX 5-1                270.279  -25.096 1.2    5.060   -1.022   13.3  0.52  25.6    0.0  0.00   0.0
GRS 1758-258          270.303  -25.729 1.5    4.521   -1.355    9.7  0.50  19.2    5.6  0.40  13.9
Ginga 1826-24         277.349  -23.789 1.7    9.272   -6.069   13.5  0.84  16.1    5.1  0.65   7.9
GX 1+4                263.028  -24.721 1.8    1.967   +4.794    7.0  0.46  15.3    0.0  0.00   0.0
IGR J17252-3616       261.296  -36.267 2.7  351.509   -0.344    5.5  0.56   9.8    0.0  0.00   0.0
H 1820-303            275.920  -30.346 2.5    2.802   -7.908    7.3  0.69  10.5    0.0  0.00   0.0
4U 1722-30            261.889  -30.826 2.8  356.300   +2.284    3.8  0.42   9.2    0.0  0.00   0.0
XTE J1751-305         267.836  -30.626 3.7  359.193   -1.936    3.0  0.43   6.9    0.0  0.00   0.0
OAO 1657-415          255.258  -41.667 3.3  344.385   +0.280   11.9  1.51   7.9    0.0  0.00   0.0
GX 349+2              256.459  -36.354 3.2  349.170   +2.775    6.1  0.74   8.2    0.0  0.00   0.0
IGR J17586-2129       269.616  -21.441 3.8    7.928   +1.323    3.9  0.59   6.7    0.0  0.00   0.0
SLX 1744-299_300      266.897  -30.026 3.9  359.291   -0.932    2.4  0.38   6.4    0.0  0.00   0.0
GX 9+1                270.331  -20.470 4.3    9.103   +1.227    3.9  0.67   5.9    0.0  0.00   0.0
GX 3+1                267.046  -26.560 3.5    2.326   +0.748    3.2  0.44   7.4    0.0  0.00   0.0
4U 1735-444           264.679  -44.495 3.9  345.992   -6.978   13.5  2.10   6.4    0.0  0.00   0.0
1A 1743-288           266.702  -28.831 0.0    0.225   -0.167    2.2  0.00   5.0    0.0  0.00   0.0
IGR J17475-2822       266.925  -28.487 4.0    0.621   -0.157    2.6  0.42   6.2    0.0  0.00   0.0
3A 1822-371           276.323  -37.076 5.3  356.834  -11.191    4.5  0.97   4.6    0.0  0.00   0.0

JEM-X

0853_jemx_mosa1.jpg 0853_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           266.500  -29.509  359.555   -0.369    6.3  0.34  18.2    0.9  0.21   4.5
1E 1740.7-2942        265.978  -29.745  359.116   -0.106    2.2  0.33   6.5    1.2  0.21   5.7
4U 1722-30            261.888  -30.802  356.320   +2.298    1.5  0.43   3.5    0.8  0.32   2.5
GRS 1741.9-2853       266.260  -28.914  359.953   +0.120    5.8  0.35  16.7    0.5  0.21   2.2
GX 3+1                266.983  -26.564    2.294   +0.794   31.9  0.67  47.5    3.2  0.35   9.1
GX 354-0              262.989  -33.835  354.302   -0.150    2.8  0.64   4.4    0.0  0.00   0.0
GX 5-1                270.279  -25.083    5.071   -1.017  117.0  4.57  25.6   17.1  2.39   7.2
SLX 1735-269          264.571  -26.994    0.796   +2.400    2.6  0.47   5.5    0.3  0.29   1.1
NEW SOURCE            268.819  -25.092    4.403   +0.124    7.1  1.57   4.6    0.0  0.00   0.0
IGR J17488-2338       267.121  -23.580    4.915   +2.226   15.3  3.50   4.4    0.0  0.00   0.0
NEW SOURCE            268.497  -25.653    3.772   +0.092    4.7  1.09   4.4    0.0  0.00   0.0
NEW SOURCE            266.013  -23.620    4.354   +3.073   10.4  2.58   4.0    0.0  0.00   0.0
NEW SOURCE            272.540  -27.626    3.837   -4.025   11.5  2.83   4.1    0.0  0.00   0.0


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