Table B.1.
eROSITA All-Sky Survey observations of thermal INSs.
| Sky field | Date⋆ | MJD | Exp. | GTI† | Rate‡ |
|---|---|---|---|---|---|
| (days) | (s) | (%) | (s−1) | ||
| RX J0420.0−5022 | |||||
| 06714101 | 2020-01-24 | 58 877.77 | 941 | 78 | 0.108(19) |
| 06714102 | 2020-07-24 | 59 060.03 | 950 | 80 | 0.146(21) |
| 06714103 | 2021-01-18 | 59 236.45 | 634 | 80 | 0.121(23) |
| 06714104 | 2021-07-25 | 59 424.41 | 648 | 78 | 0.126(23) |
| RX J0720.4−3125 | |||||
| 11112001 | 2020-04-21 | 58 962.14 | 245 | 71 | 6.67(29) |
| 11112002 | 2020-10-24 | 59 147.77 | 216 | 80 | 7.17(31) |
| 11112003 | 2021-04-23 | 59 329.52 | 302 | 79 | 7.42(25) |
| 11112004 | 2021-10-25 | 59 514.40 | 317 | 87 | 7.76(33) |
| RX J0806.4−4123 | |||||
| 12113201 | 2020-05-07 | 58 978.14 | 331 | 71 | 1.58(13) |
| 12113202 | 2020-11-07 | 59 162.53 | 288 | 74 | 1.55(12) |
| 12113203 | 2021-05-10 | 59 345.93 | 259 | 76 | 1.74(13) |
| 12113204 | 2021-11-09 | 59 529.57 | 288 | 77 | 1.79(14) |
| 2XMM J104608.7−594306 | |||||
| 16315001 | 2020-01-01 | 58 852.22 | 533 | 84 | 0.086(25) |
| 16315002 | 2020-07-01 | 59 034.39 | 576 | 84 | 0.085(25) |
| 16315003 | 2021-01-01 | 59 217.67 | 418 | 81 | 0.111(33) |
| 16315004 | 2021-07-04 | 59 404.56 | 799 | 91 | 0.096(32) |
| RX J1308.6+2127 | |||||
| 19606901 | 2019-12-15 | 58 834.01 | 245 | 73 | 3.02(19) |
| 19606902 | 2020-06-14 | 59 015.18 | 187 | 79 | 2.67(21) |
| 19606903 | 2020-12-17 | 59 202.22 | 230 | 82 | 2.62(19) |
| 19606904 | 2021-06-19 | 59 385.89 | 245 | 77 | 2.46(17) |
| RX J1856.5−3754 | |||||
| 28212901 | 2020-04-09 | 58 949.34 | 115 | 69 | 5.86(31) |
| 28212902 | 2020-10-13 | 59 136.08 | 115 | 69 | 5.48(30) |
| 28212903 | 2021-04-08 | 59 313.30 | 158 | 73 | 5.60(30) |
| 28212904 | 2021-10-10 | 59 498.62 | 173 | 80 | 5.53(27) |
Notes. All eROSITA observations were processed with pipeline version c020. The telescope modules (TMs) were operated in SURVEY mode with FILTER setup.
We show the count rate of the targets from source detection and PSF fitting over the TMs unaffected by optical light leaks, with 1σ errors (0.2 − 1 keV; see Fig. B.1).
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