INTEGRAL Galactic bulge Monitoring

Revolution 1021: Observation start 1999-12-31T23:58 = MJD 51544
Total Observation GTI = 9398 seconds

IBIS/ISGRI

1021_isgri_mosa1.jpg 1021_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 354-0              262.983  -33.836 0.8  354.298   -0.146   19.0  0.46  40.9    6.5  0.36  18.2
GX 5-1                270.268  -25.083 1.1    5.067   -1.007   13.0  0.46  28.1    0.0  0.00   0.0
1E 1740.7-2942        265.993  -29.737 1.3  359.130   -0.112    9.6  0.41  23.4    5.8  0.33  17.6
IGR J17091-3624       257.292  -36.413 1.6  349.525   +2.203   12.7  0.71  17.7    5.0  0.53   9.5
Ginga 1826-24         277.389  -23.778 1.8    9.298   -6.097   12.8  0.80  15.9    5.5  0.59   9.3
GRS 1758-258          270.316  -25.751 2.0    4.508   -1.376    6.2  0.46  13.5    3.7  0.35  10.5
IGR J17391-3021       264.806  -30.338 2.1  358.076   +0.443    5.1  0.40  12.7    0.0  0.00   0.0
OAO 1657-415          255.217  -41.645 2.1  344.384   +0.318   23.9  1.85  12.9    9.0  1.30   6.9
GX 349+2              256.424  -36.431 2.6  349.091   +2.751    7.8  0.76  10.2    0.0  0.00   0.0
H 1820-303            275.923  -30.365 3.1    2.786   -7.919    5.5  0.66   8.3    0.0  0.00   0.0
SLX 1735-269          264.700  -27.016 4.5    0.839   +2.292    2.3  0.40   5.6    0.0  0.00   0.0
4U 1722-30            261.928  -30.711 4.1  356.415   +2.320    2.8  0.46   6.2    2.1  0.36   5.8
3A 1822-371           276.440  -37.081 4.8  356.870  -11.277    5.2  1.00   5.2    0.0  0.00   0.0
GX 9+1                270.345  -20.528 0.0    9.060   +1.186    2.7  0.00   4.5    0.0  0.00   0.0
SLX 1744-299_300      266.862  -30.015 5.2  359.285   -0.901    1.8  0.39   4.7    0.0  0.00   0.0
GRS 1734-292          264.361  -29.139 5.1  358.884   +1.410    1.9  0.39   4.9    0.0  0.00   0.0
1A 1742-294           266.497  -29.504 0.0  359.557   -0.365    1.6  0.00   4.3    0.0  0.00   0.0
SAX J1806.5-2215      271.602  -22.242 7.0    8.142   -0.675    1.8  0.54   3.4    0.0  0.00   0.0
SAX J1712.6-3739      258.143  -37.652 5.4  348.928   +0.922    3.5  0.76   4.6    0.0  0.00   0.0
IGR J18027-2016       270.680  -20.277 6.0    9.433   +1.037    2.6  0.64   4.1    0.0  0.00   0.0
SLX 1737-282          265.230  -28.284 5.6    0.013   +1.221    1.9  0.42   4.4    0.0  0.00   0.0
NEW SOURCE            268.175  -26.966 4.4    2.494   -0.326    2.3  0.40   5.7    0.0  0.00   0.0

JEM-X

1021_jemx_mosa1.jpg 1021_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           266.522  -29.496  359.575   -0.379    8.8  0.33  26.5    1.5  0.19   8.2
1A 1743-288           266.763  -28.883    0.209   -0.240    8.4  0.34  24.6    0.7  0.19   3.7
1E 1740.7-2942        265.978  -29.745  359.116   -0.106    1.9  0.32   6.0    1.3  0.19   6.6
1E 1743.1-2843        266.587  -28.729    0.260   -0.029    2.1  0.33   6.4    0.2  0.18   1.2
GX 3+1                266.985  -26.568    2.291   +0.790   27.0  0.41  65.4    3.0  0.21  14.5
GX 354-0              262.989  -33.835  354.302   -0.150   10.5  1.36   7.7    4.3  1.05   4.1
GX 5-1                270.278  -25.082    5.072   -1.015  122.4  1.59  77.1   16.1  0.70  22.9
IGR J17391-3021       264.791  -30.341  358.066   +0.452    2.9  0.36   8.1    1.3  0.23   5.7
SLX 1744-299_300      266.858  -29.999  359.297   -0.889    2.0  0.33   6.1    0.6  0.19   3.0


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