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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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