INTEGRAL Galactic bulge Monitoring

Revolution 0907: Observation start 2010-03-21T00:25 = MJD 55276.018
Total Observation GTI = 7922 seconds

IBIS/ISGRI

0907_isgri_mosa1.jpg 0907_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        265.982  -29.751 1.1  359.112   -0.112   11.9  0.43  27.6    7.4  0.36  20.6
IGR J17391-3021       264.809  -30.341 1.2  358.075   +0.439   11.9  0.48  24.7    2.1  0.40   5.3
GX 5-1                270.292  -25.072 1.5    5.087   -1.021   10.1  0.52  19.4    0.0  0.00   0.0
GX 1+4                263.006  -24.748 1.8    1.933   +4.796    7.1  0.47  15.0    0.0  0.00   0.0
Ginga 1826-24         277.358  -23.808 2.0    9.259   -6.085   11.1  0.80  13.9    4.8  0.61   7.9
GX 354-0              262.997  -33.828 2.2  354.311   -0.152    6.7  0.56  12.0    0.0  0.00   0.0
GRS 1758-258          270.296  -25.724 2.1    4.522   -1.347    5.8  0.45  12.8    3.5  0.36   9.6
H 1820-303            275.919  -30.343 2.7    2.805   -7.906    6.6  0.68   9.6    0.0  0.00   0.0
SAX J1753.5-2349      268.390  -23.836 2.9    5.289   +1.096    3.8  0.42   8.9    2.3  0.34   6.6
GX 349+2              256.471  -36.434 2.9  349.112   +2.719    7.2  0.80   9.0    0.0  0.00   0.0
GX 9+1                270.411  -20.469 3.1    9.141   +1.162    4.4  0.53   8.3    0.0  0.00   0.0
GX 3+1                267.078  -26.628 4.0    2.282   +0.688    2.5  0.40   6.3    0.0  0.00   0.0
GX 17+2               273.975  -14.075 3.9   16.384   +1.286   11.2  1.73   6.5    0.0  0.00   0.0
4U 1722-30            261.870  -30.810 4.7  356.305   +2.307    2.5  0.48   5.3    0.0  0.00   0.0
3A 1822-371           276.374  -37.068 5.0  356.860  -11.224    5.4  1.09   5.0    0.0  0.00   0.0
4U 1812-12            273.746  -12.082 4.8   18.032   +2.430   19.2  3.68   5.2    0.0  0.00   0.0
1RXS J165424.7-29541  253.635  -29.814 5.6  352.919   +8.644    3.5  0.79   4.4    0.0  0.00   0.0
SLX 1744-299_300      266.939  -29.908 6.6  359.410   -0.902    1.7  0.48   3.7    0.0  0.00   0.0
1A 1743-288           266.665  -28.856 5.7    0.187   -0.153    1.7  0.39   4.3    1.4  0.00   4.1
Oph Cluster           258.180  -23.296 5.6    0.669   +9.264    2.4  0.55   4.4    0.0  0.00   0.0
4U 1700-377           255.961  -37.835 6.2  347.749   +2.195    4.3  0.00   3.9    0.0  0.00   0.0
IGR J17511-3057       267.754  -31.024 5.4  358.815   -2.078    2.0  0.45   4.5    0.0  0.00   0.0

JEM-X

0907_jemx_mosa1.jpg 0907_jemx_mosa2.jpg

JEM-X2 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-X2 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    5.0  0.46  10.7    0.7  0.26   2.8
1E 1740.7-2942        265.978  -29.745  359.116   -0.106    2.5  0.49   5.1    1.8  0.28   6.3
GX 3+1                266.988  -26.568    2.292   +0.788   33.2  0.47  70.0    3.7  0.22  17.1
GX 5-1                270.280  -25.076    5.078   -1.014  154.6  1.72  90.0   16.5  0.67  24.8
IGR J17391-3021       264.796  -30.341  358.069   +0.448    5.6  0.57   9.9    2.1  0.34   6.1
NEW SOURCE            270.400  -22.558    7.321   +0.138   19.3  3.97   4.9    2.1  1.88   1.1
NEW SOURCE            267.675  -21.959    6.570   +2.618   15.2  2.67   5.7    0.0  0.00   0.0
NEW SOURCE            270.772  -29.022    1.858   -3.339    7.4  1.43   5.2    0.0  0.00   0.0
NEW SOURCE            272.020  -26.567    4.544   -3.109   13.0  2.34   5.6    1.9  1.55   1.2
NEW SOURCE            270.542  -27.787    2.836   -2.556    4.8  1.03   4.7    0.6  0.48   1.2
NEW SOURCE            271.306  -25.845    4.864   -2.199    8.7  1.73   5.0    0.0  0.00   0.0
NEW SOURCE            271.679  -28.069    3.081   -3.571    6.1  1.81   3.4    3.5  1.18   3.0


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