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Home All issues Volume 495 / No 3 (March I 2009) A&A, 495 3 (2009) 899-900 Full HTML
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Erratum
This article is an erratum for:
[https://doi.org/10.1051/0004-6361:20077899]

 

 

Table 3:

Best-fit parameters from the fits to the spectra of Elias 29, during 6 different time intervals (PN data only), using an absorbed 1T thermal model with an additional line at 6.4 keV (Fe fluorescent line).
Time interval $N({\rm H})$ kT Z $E\!M$ $f_{\rm 6.4 keV}$ $W_{\rm 6.4~keV}$ $\chi^2$/d.o.f. P $F_{\rm X}$ $R_{\rm 6.4~ keV}$\ddag
  N22 keV $Z_{\odot}$ $E\!M_{53}$ f-6 eV     F-13 %
seg1 5.5 $\pm$ 0.7 4.8 $\pm$ 1.0 1.1 $\pm$ 0.3 0.7 $\pm$ 0.3 0.1 $\pm$ 0.7 34.8 1.0 0.5 1.8 46
flare 9.4 $\pm$ 2.0 3.9 $\pm$ 1.4 0.9 $\pm$ 0.3 4.5 $\pm$ 3.4 2.0 $\pm$ 5.9 162.0 0.9 0.6 7.5 22
seg2 8.2 $\pm$ 1.3 2.8 $\pm$ 0.6 1.1 $\pm$ 0.3 0.8 $\pm$ 0.4 1.1 $\pm$ 0.6 834.0 1.3 0.1 1.1 0.1
seg3 6.6 $\pm$ 0.8 3.3 $\pm$ 0.6 0.7 $\pm$ 0.2 0.9 $\pm$ 0.4 0.5 $\pm$ 0.5 270.0 0.9 0.6 1.3 4.0
seg4 7.6 $\pm$ 0.6 3.6 $\pm$ 0.4 0.7 $\pm$ 0.1 1.7 $\pm$ 0.5 0.7 $\pm$ 0.7 171.0 1.3 0.1 2.7 3.1
seg5 4.9 $\pm$ 0.4 4.5 $\pm$ 0.8 0.6 $\pm$ 0.1 1.1 $\pm$ 0.3 1.1 $\pm$ 0.8 335.0 1.2 0.2 2.5 0.3
seg3+seg4+seg5 $\diamondsuit$ 6.4 $\pm$ 0.3 3.9 $\pm$ 0.3 0.6 $\pm$ 0.1 1.2 $\pm$ 0.2 1.0 $\pm$ 0.3 330.0 1.3 0.0 2.1 0.0
\ddag Probability that a line with a best-fit value equal or greater than $W_{\rm 6.4~keV}$ could be due to a random fluctuation in the data, as estimated via Monte Carlo simulations (see Sects. 3 and 4).

$\diamondsuit$ Results for the fit to the source's spectrum integrated over time intervals ``seg3'', ``seg4'', and ``seg5''.

Note: For the line, the total flux in the line ( $f_{\rm 6.4 ~keV}$ in units of f-6 = 10-6 photons cm-2 s-1) and the equivalent width ( $W_{\rm 6.4~keV}$) are given.


Source LaTeX | All tables | In the text

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