Table 2: Best-fit spectral parameters of the log-parabolic model for the XRT (first section) and BeppoSAX (second section) observations of PKS 0548-322.
Instrument Date K(1) a(1) b(1) $E_{\rm p}$ F2-10(2) $\chi^2_{\rm r}$/d.o.f.
          (keV) (erg cm-2 s-1)  
Swift XRT 2005 April 26 1.41 (0.05) $\times$ 10-2 1.81 (0.07) 0.18 (0.13) 3.4 4.0 $\times$ 10-11 0.75/118
Swift XRT 2005 May 21 1.48 (0.04) $\times$ 10-2 1.71 (0.05) 0.38 (0.10) 2.4 4.0 $\times$ 10-11 0.90/196
    1.46 (0.04) $\times$ 10-2 1.78 (0.03) 0.18 frozen 3.5 4.2 $\times$ 10-11 0.94/197
Swift XRT 2005 May 22 1.66 (0.02) $\times$ 10-2 1.90 (0.02) 0.18 (0.04) 1.9 4.1 $\times$ 10-11 1.03/408
Swift XRT 2005 May 29 1.31 (0.04) $\times$ 10-2 1.77 (0.06) 0.34 (0.11) 2.2 3.3 $\times$ 10-11 1.01/181
    1.29 (0.04) $\times$ 10-2 1.83 (0.04) 0.18 frozen 2.7 3.5 $\times$ 10-11 1.03/182
Swift XRT 2005 June 24 1.52 (0.05) $\times$ 10-2 1.79 (0.06) 0.26 (0.11) 2.5 4.1 $\times$ 10-11 1.09/183
BeppoSAX LECS+MECS 1999 Feb. 20 0.77 (0.07) $\times$ 10-2 1.57 (0.10) 0.48 (0.10) 2.8 2.3 $\times$ 10-11 1.23/55
BeppoSAX LECS+MECS 1999 April 07 0.69 (0.06) $\times$ 10-2 1.82 (0.10) 0.42 (0.10) 1.6 1.5 $\times$ 10-11 0.91/55
(1) Numbers in parenthesis are statistical errors at the 90% confidence level.
(2) Fluxes in the 2-10 keV energy band are corrected for Galactic absorption.

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