INTEGRAL Galactic bulge Monitoring

Revolution 1266: Observation start 2013-02-24T07:03 = MJD 56347.294
Total Observation GTI = 9751 seconds

IBIS/ISGRI

1266_isgri_mosa1.jpg 1266_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           255.992  -37.850 0.7  347.753   +2.167   54.9  1.12  49.2   16.7  0.76  22.0
Ginga 1826-24         277.357  -23.783 1.2    9.281   -6.073   16.3  0.69  23.8    5.2  0.48  10.8
GX 354-0              262.982  -33.833 1.3  354.300   -0.145   12.8  0.56  22.7    3.3  0.40   8.4
Swift J174510.8-2624  266.309  -26.404 1.2    2.117   +1.393   10.2  0.42  24.1    7.0  0.32  21.8
GRS 1758-258          270.297  -25.734 1.6    4.514   -1.353    8.9  0.50  17.7    6.6  0.36  18.1
XTE J1810-189         272.598  -19.078 1.9   11.361   +0.046   10.1  0.69  14.6    3.0  0.49   6.1
3A 1822-371           276.430  -37.098 3.2  356.852  -11.277    5.9  0.73   8.0    0.0  0.00   0.0
KS 1741-293           266.186  -29.330 2.7  359.564   -0.042    3.9  0.41   9.7    1.8  0.30   6.0
GX 349+2              256.450  -36.431 3.2  349.104   +2.735    8.0  0.99   8.0    0.0  0.00   0.0
GX 5-1                270.255  -25.061 4.3    5.080   -0.987    2.9  0.50   5.9    0.0  0.00   0.0
H 1820-303            275.871  -30.410 3.4    2.725   -7.898    4.7  0.63   7.5    0.0  0.00   0.0
4U 1722-30            261.860  -30.801 3.7  356.307   +2.319    3.4  0.49   6.8    0.0  0.00   0.0
IGR J17456-2901       266.396  -28.988 0.0  359.952   -0.020    2.5  0.00   6.0    0.0  0.00   0.0
SLX 1744-299_300      266.941  -30.082 3.8  359.263   -0.993    2.9  0.44   6.6    0.0  0.00   0.0
H 1702-429            256.537  -43.049 0.0  343.864   -1.311   17.3  0.00   5.6    0.0  0.00   0.0
SLX 1735-269          264.600  -26.919 4.9    0.873   +2.418    2.2  0.43   5.0    1.4  0.31   4.3
IGR J17091-3624       257.139  -36.390 3.3  349.470   +2.315    7.4  0.96   7.7    3.2  0.66   4.8
Swift J1753.7-2544    268.435  -25.704 6.0    3.699   +0.114    1.8  0.44   4.0    1.7  0.33   5.3
GX 3+1                266.964  -26.535 4.9    2.310   +0.823    2.3  0.45   5.1    0.0  0.00   0.0
IGR J17419-2802       265.472  -27.910 5.6    0.443   +1.237    1.8  0.00   4.4    0.0  0.00   0.0
GX 17+2               274.002  -13.984 0.0   16.476   +1.306    8.7  0.00   4.1    0.0  0.00   0.0
GX 1+4                263.015  -24.695 6.6    1.983   +4.818    1.9  0.52   3.7    0.0  0.00   0.0
NEW SOURCE            262.185  -27.090 4.2  359.561   +4.134    2.8  0.47   6.0    0.0  0.00   0.0

JEM-X

1266_jemx_mosa1.jpg 1266_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           266.498  -29.515  359.548   -0.371    5.7  0.28  19.9    0.4  0.11   4.0
1E 1743.1-2843        266.587  -28.729    0.260   -0.029    1.7  0.29   5.8    0.2  0.11   1.7
GX 3+1                266.979  -26.565    2.290   +0.796   38.9  0.41  94.4    2.3  0.15  15.2
GX 354-0              262.989  -33.835  354.302   -0.150    7.6  1.61   4.7    1.1  0.73   1.5
GX 5-1                270.278  -25.083    5.071   -1.015  104.8  1.02 102.7    4.8  0.36  13.2
XTE J1739-285         264.975  -28.496  359.714   +1.298    7.3  0.34  21.8    0.3  0.11   2.3
NEW SOURCE            272.766  -26.073    5.300   -3.458    7.2  1.59   4.5    0.0  0.00   0.0
Swift J174510.8-2624  266.298  -26.417    2.101   +1.394    1.9  0.40   4.9    0.6  0.16   3.6


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