Table 1
Log of the INTEGRAL data used in this paper.
| Rev. | Observing time | Exposure time | Fluxa | |||
| START | STOP | ISGRI | JEM-Xa | ISGRI | JEM-Xb | |
| (MJD) | (MJD) | (ks) | (ks) | (20−70 keV) | (3−35 keV) | |
|
|
||||||
| 1329 | 56 535.85950 | 56 536.01338 | 8.6 | 4.9 | 13.0 ± 2.0 | <12.0 |
| 1330 | 56 538.69428 | 56 539.63178 | 73.3 | 8.0 | 19.7 ± 1.0 | 16.1 ± 4.0 |
| 1331 | 56 541.84263 | 56 542.66694 | 63.2 | 3.2 | <20.5 | <3.5 |
| 1332 | 56 544.85712 | 56 545.84130 | 74.0 | 7.7 | <2.7 | <9.8 |
| 1333 | 56 548.63922 | 56 548.79324 | 10.9 | 4.7 | <3.8 | <12.0 |
| 1334 | 56 552.33453 | 56 553.07995 | 59.3 | 7.3 | <3.1 | <12.5 |
| 1335 | 56 553.63791 | 56 554.41490 | 58.0 | 10.8 | <3.0 | <8.7 |
| 1336 | 56 556.62811 | 56 559.26417 | 71.3 | 14.6 | <2.3 | <7.2 |
| 1337 | 56 559.80640 | 56 560.39413 | 45.4 | 10.9 | <2.9 | <8.2 |
| 1339 | 56 565.59969 | 56 568.21845 | 199.7 | 23.9 | 8.8 ± 0.4 | 7.2 ± 2.0 |
| 1340 | 56 569.43604 | 56 571.05972 | 105.2 | 25.8 | 7.6 ± 0.7 | <5.8 |
| 1341 | 56 572.63094 | 56 574.06932 | 112.8 | 24.5 | 5.1 ± 0.7 | <5.6 |
| 1343 | 56 577.59515 | 56 578.53990 | 69.0 | 13.6 | 9.8 ± 0.9 | <7.6 |
| 1344 | 56 580.71753 | 56 582.17201 | 109.7 | 25.7 | 7.5 ± 0.6 | <5.5 |
| 1345 | 56 586.02326 | 56 586.58723 | 45.5 | 7.6 | 14.0 ± 1.0 | 15.3 ± 3.6 |
| 1346 | 56 586.73297 | 56 589.00642 | 110.4 | 20.1 | 8.7 ± 0.7 | 10.8 ± 2.2 |
| 1347 | 56 589.72509 | 56 590.51950 | 63.3 | 12.0 | 6.6 ± 0.8 | 19.0 ± 2.8 |
| 1348 | 56 592.54664 | 56 593.31612 | 60.8 | 5.8 | 8.3 ± 1.1 | 22.2 ± 5.0 |
Notes. We report the effective exposure times, detection significance and estimated fluxes for ISGRI, JEM-X1, and JEM-X2 in all revolutions considered for the data analysis. The detection significances are reported for ISGRI (JEM-X1, 2) in the 20−40 keV (3−10 keV) energy band. We considered a detection reliable in ISGRI and JEM-X only >6σ and >4σ, respectively. Lower significance detections have been considered only to derive upper limits on the source X-ray emission (all upper limits are at 3σ c.l.).
The flux in mCrab has been estimated by comparing the source count-rate measured from the mosaic to the count-rate from the Crab in the same energy band. The count-rate from the Crab has been measured by extracting ISGRI, JEM-X1, and JEM-X2 mosaics of the public calibration observations performed in satellite revolutions 1342 (i.e., the calibration observations performed during the outburst of Swift J1734.5-3027). From these data we measured a Crab count-rate of 206.1 ± 0.2 cts s-1 in ISGRI (20−70 keV energy band) and 119.4 ± 0.6 cts s-1 (134.5 ± 0.7) for JEM-X2 (JEM-X1) in the 3−35 keV energy band.
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