Table 1
Log of all Swift/XRT observations used in the present paper.
| Sequence | Obs. | Start time | End time | Exposure | NH | Γ | Flux0.5-10 keV | cstat/d.o.f. |
|---|---|---|---|---|---|---|---|---|
| mode | (UTC) | (UTC) | (s) | (1023 cm−2) | ||||
| 00010244001 | PC | 2017-08-16 02:26:50 | 2017-08-16 02:45:55 | 1973 | 4.9 ± 4.0 | -0.9 |
2.9 |
39.6/23 |
| 00010244002 | PC | 2017-08-16 17:03:06 | 2017-08-16 20:02:21 | |||||
| 00010244003 | PC | 2017-08-22 03:47:02 | 2017-08-22 05:30:03 | 960 | 5.1 |
1.6 |
16.0 ± 3.0 | 55.8/49 |
| 00010244004 | PC | 2017-08-24 16:43:09 | 2017-08-24 23:11:00 | 872 | 6.6 |
1.4 |
4.9 |
28.8/26 |
| 00010244005 | PC | 2017-08-25 23:00:00 | 2017-08-26 06:39:00 | 601 | 2.5 |
-0.9 |
5.1 |
10.7/14 |
| 00010244006 | PC | 2017-08-26 08:06:00 | 2017-08-26 14:59:00 | 862 | 5.3 |
-0.4 |
7.8 |
13.7/15 |
| 00010244007 | PC | 2017-09-05 21:29:00 | 2017-09-05 23:17:00 | 659 | 4.2 |
1.8 |
3.6 |
25.9/18 |
| 00010244008 | PC | 2017-09-10 22:35:00 | 2017-09-10 22:53:00 | 952 | 6.6 |
1.1 |
3.6 |
18.0/19 |
| 00010244009 | PC | 2017-09-13 01:36:00 | 2017-09-13 06:28:00 | 717 | 8.2 |
3.2 |
2.7 |
19.7/14 |
| 00010244010 | PC | 2017-09-16 12:43:00 | 2017-09-16 13:02:00 | 1100 | 3.3 |
1.5 |
3.4 |
51.8/29 |
| 00010244011 | PC | 2017-09-23 15:10:00 | 2017-09-23 21:48:00 | 897 | 2.6 |
0.7 |
8.7 |
23.3/32 |
| 00010244012 | PC | 2017-09-30 16:25:00 | 2017-09-30 16:42:00 | 955 | 6.3 |
2.7 |
5.1 |
32.2/36 |
| 00010244013 | PC | 2017-10-07 01:12:00 | 2017-10-07 02:57:00 | 1508 | 1.6 |
0.7 ± 0.8 | 5.3 |
72.8/44 |
| 00010244014 | PC | 2017-10-14 03:51:00 | 2017-10-14 04:03:00 | |||||
| 00010244015 | PC | 2017-10-21 00:26:00 | 2017-10-21 01:56:00 | 1381 | 4.5 |
1.5 |
5.1 ± 0.8 | 53.7/57 |
| 00010244016 | PC | 2017-10-26 12:28:00 | 2017-10-26 12:45:00 | |||||
Notes. We also report for each observation the results obtained from the spectral analysis. In all cases, the best fit model isan absorbed power law (TBABS*POW in XSPEC), where we used wilm abundances (Wilms et al. 2000) and vern cross sections (Verner et al. 1996). The reported flux is in the 0.5–10 keV energy range and in units of 10−11 erg cm−2 s−1 (it is not corrected for absorption). We note that a few adjacent observations were merged together to obtain a reasonable statistics toperform the spectral fit. All spectra were fit with the C-statistics (Cash 1979) due to the relatively low number of counts.
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