Open Access

Table B.1.

Results of the spectral analysis of the Swift-XRT observations of BL Lac during September to November 2022.

Day MJD ObsID Exposure Significance [σ] Flux (0.3 − 10 keV) Flux (2.0 − 10 keV) Spectral index
[s] Log-parabola model [×10−12 erg cm−2 s−1] [×10−12 erg cm−2 s−1]
09/16 59838.6 00014925014 1981 1.7 53 ± 5 24 ± 2 1.81 ± 0.02

09/18 59840.5 00014925015 1994 1.9 19 ± 2 11 ± 1 1.63 ± 0.02

09/20 59842.3 00014925016 572 0.9 26 ± 3 13 ± 3 1.82 ± 0.02

09/23 59845.5 00014925017 705 0.3 24 ± 3 14 ± 2 1.70 ± 0.02

10/17 59869.8 00014925018 1102 1.5 42 ± 3 18 ± 2 2.10 ± 0.02

10/17 59869.9 00014925019 1412 0.4 40 ± 3 18 ± 2 2.00 ± 0.02

10/22 59874.4 00014925021 1978 3.7 77 ± 5 24 ± 3 2.33 ± 0.02

10/23 59875.8 00014925020 1832 4.3 56 ± 5 26 ± 2 1.92 ± 0.02

10/25 59877.0 00014925023 1008 3.8 55 ± 6 27 ± 5 1.82 ± 0.02

10/26 59878.3 00096990012 1034 1.9 37 ± 3 23 ± 2 1.70 ± 0.02

10/29 59881.1 00014925024 1661 3.4 78 ± 5 27 ± 3 2.09 ± 0.02

11/01 59884.1 00014925026 951 1.1 72 ± 3 27 ± 2 2.16 ± 0.02

11/04 59887.3 00014925027 1240 2.3 87 ± 5 32 ± 3 2.22 ± 0.02

11/07 59890.1 00014925028 1035 4.2 60 ± 5 24 ± 3 2.15 ± 0.02

11/12 59895.4 00096990013 849 1.9 219 ± 11 50 ± 3 2.60 ± 0.03

11/13 59896.3 00014925030 1278 2.2 64 ± 3 21 ± 2 2.33 ± 0.02

11/21 59904.8 00014925032 1681 2.4 66 ± 3 26 ± 2 2.14 ± 0.02

11/23 59906.0 00014925033 1447 2.7 124 ± 8 34 ± 3 2.43 ± 0.02

11/25 59908.4 00096990014 865 2.0 93 ± 5 27 ± 2 2.43 ± 0.02

11/25 59908.7 00014925034 2021 2.5 69 ± 6 24 ± 3 2.14 ± 0.02

11/26 59909.5 00096990015 905 2.6 71 ± 6 27 ± 3 2.14 ± 0.02

11/27 59910.2 00096990016 834 2.8 97 ± 15 29 ± 6 2.35 ± 0.02

11/28 59911.9 00089562001 1473 3.7 61 ± 5 24 ± 2 2.09 ± 0.02

11/29 59912.2 00096990017 826 2.7 98 ± 8 31 ± 5 2.33 ± 0.02

11/30 59913.4 00096990018 895 3.7 84 ± 13 47 ± 10 1.82 ± 0.02

12/01 59914.1 00096990019 960 3.2 80 ± 8 32 ± 5 2.09 ± 0.02

Notes. For each observation, the following quantities are reported: day, MJD, Swift ObsID, exposure, intrinsic flux reconstructed in the 0.3 − 10 keV and 2.0 − 10 keV bands and photon index from the fit assuming a power-law model for the intrinsic source spectrum. For those observations in which the log-parabola model was preferred over the power-law at a significance greater than 3σ, the reported fluxes were reconstructed from the best-fit log-parabola model.

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