Results from DROXO - I. The variability of fluorescent Fe 6.4 keV emission in the young star Elias 29. High-energy electrons in the star's accretion tubes?

G. Giardino; F. Favata; I. Pillitteri; E. Flaccomio; G. Micela; S. Sciortino

doi:doi:10.1051/0004-6361/20077899e

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This article is an erratum for: [this article]

Table 1:

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.
Time interval	$N({\rm H})$	kT	Z	$E\!M$	$\chi^2$ /d.o.f.	P	$F_{\rm X}$
	N₂₂	keV	$Z_{\odot}$	$E\!M_{53}$			F_-13
seg1	5.7 $\pm$ 0.7	4.6 $\pm$ 0.9	1.0 $\pm$ 0.3	0.7 $\pm$ 0.3	1.0	0.6	1.8
flare	9.5 $\pm$ 2.0	4.1 $\pm$ 1.5	0.9 $\pm$ 0.3	4.5 $\pm$ 3.4	0.9	0.5	7.5
seg2	8.1 $\pm$ 1.3	3.1 $\pm$ 0.8	1.0 $\pm$ 0.3	0.7 $\pm$ 0.5	1.5	0.0	1.1
seg3	6.6 $\pm$ 0.8	3.4 $\pm$ 0.7	0.7 $\pm$ 0.2	0.8 $\pm$ 0.4	1.0	0.5	1.3
seg4	7.7 $\pm$ 0.6	3.7 $\pm$ 0.5	0.7 $\pm$ 0.1	1.7 $\pm$ 0.5	1.4	0.0	2.7
seg5	4.9 $\pm$ 0.4	4.7 $\pm$ 0.8	0.6 $\pm$ 0.1	1.1 $\pm$ 0.3	1.3	0.1	2.5

Note: units are $N_{22} = 10^{22}~{\rm cm^{-2}}$ , $E\!M_{53} = 10^{53}$ cm^-3, and F_-13= 10^-13 erg cm^-2 s^-1. The spectral fits were carried out in the energy range 1.0-9.0 keV. Flux values refer to energy range 1.0-7.5 keV. The error bars are at 1 $\sigma$ . Reduced $\chi^2$ and null-hypothesis probability (P) for the fits are also given.

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