INTEGRAL Galactic bulge Monitoring

Revolution 0851: Observation start 2009-10-01T20:54 = MJD 55105.871
Total Observation GTI = 12264 seconds

IBIS/ISGRI

0851_isgri_mosa1.jpg 0851_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  
==================== ========  ======= === ======== ======== ====== ===== ===== ====== ===== =====
1E 1740.7-2942        265.975  -29.742 0.9  359.117   -0.102   12.0  0.35  34.0    8.0  0.31  26.1
GX 5-1                270.282  -25.088 1.2    5.068   -1.021   11.0  0.42  25.9    0.0  0.00   0.0
GRS 1758-258          270.294  -25.756 1.2    4.494   -1.361    9.5  0.38  24.8    5.4  0.32  16.9
GX 349+2              256.461  -36.416 1.5  349.121   +2.736   12.8  0.69  18.7    0.0  0.00   0.0
Ginga 1826-24         277.371  -23.798 1.6    9.273   -6.091   11.5  0.66  17.5    4.1  0.52   7.9
GX 1+4                263.017  -24.770 1.7    1.920   +4.776    6.9  0.42  16.4    0.0  0.00   0.0
IGR J17586-2129       269.601  -21.398 2.8    7.959   +1.356    4.7  0.50   9.4    0.0  0.00   0.0
H 1820-303            275.924  -30.342 2.5    2.808   -7.909    4.9  0.47  10.4    0.0  0.00   0.0
3A 1822-371           276.428  -37.103 2.9  356.847  -11.278    5.6  0.62   9.0    0.0  0.00   0.0
4U 1722-30            261.849  -30.806 2.9  356.297   +2.324    3.6  0.40   9.0    2.0  0.33   6.3
GX 3+1                266.945  -26.568 3.7    2.272   +0.821    2.5  0.36   6.9    0.0  0.00   0.0
GX 9+1                270.394  -20.519 3.2    9.090   +1.151    4.9  0.62   8.0    0.0  0.00   0.0
SLX 1735-269          264.538  -27.012 3.5    0.765   +2.416    2.7  0.37   7.4    0.0  0.00   0.0
IGR J17511-3057       267.775  -31.048 4.0  358.802   -2.106    2.5  0.40   6.3    1.7  0.32   5.2
SLX 1744-299_300      266.738  -30.039 4.0  359.208   -0.821    2.0  0.31   6.4    0.0  0.00   0.0
GX 17+2               273.962  -13.954 4.7   16.484   +1.354   40.4  7.60   5.3    0.0  0.00   0.0
3A 1728-169           262.934  -16.944 5.3    8.528   +9.047    4.8  1.03   4.6    0.0  0.00   0.0
H 1702-429            256.665  -43.003 5.6  343.957   -1.358    7.1  0.00   4.4    0.0  0.00   0.0
1E 1742.8-2853        266.574  -28.993 6.0    0.029   -0.156    1.5  0.37   4.1    0.0  0.00   0.0

JEM-X

0851_jemx_mosa1.jpg 0851_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           266.527  -29.514  359.562   -0.392    6.7  0.30  22.5    0.9  0.19   4.6
1E 1740.7-2942        265.978  -29.745  359.116   -0.106    2.4  0.30   8.0    1.1  0.20   5.5
4U 1722-30            261.888  -30.802  356.320   +2.298    2.1  0.61   3.5    0.0  0.00   0.0
GRS 1741.9-2853       266.260  -28.914  359.953   +0.120    1.4  0.31   4.3    0.3  0.20   1.7
GX 3+1                266.983  -26.564    2.294   +0.794   31.3  0.64  48.8    3.1  0.35   8.9
GX 354-0              262.989  -33.835  354.302   -0.150    3.0  0.80   3.8    0.9  0.66   1.4
GX 5-1                270.284  -25.079    5.077   -1.019  113.9  2.25  50.7   13.3  1.12  11.9
SLX 1744-299_300      266.858  -29.999  359.297   -0.889    2.6  0.29   9.3    0.5  0.19   2.6
NEW SOURCE            269.911  -24.662    5.271   -0.517   11.9  2.29   5.2    2.5  1.42   1.7
NEW SOURCE            267.831  -24.372    4.567   +1.263    7.5  1.75   4.3    0.0  0.00   0.0
NEW SOURCE            268.481  -23.976    5.210   +0.954   11.5  2.80   4.1    1.7  1.58   1.1


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