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Home All issues Volume 505 / No 2 (October II 2009) A&A, 505 2 (2009) 695-706 Full HTML
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Table 4:

Results from the analysis of the Spitzer/IRS and DROXO datasets (cf. Sects. 3.1 and 3.2).
\begin{displaymath}{\begin{tabular}{lr@{}lrr@{}lr\vert cr@{}lr@{}lr@{}l} \hline\... ....32$& & $45.21$& $_{ 0.00}^{1368.17}$\\ \hline \end{tabular}} \end{displaymath}
Notes: IR and X-ray fluxes and luminosities are corrected for extinction. Column 6 indicates the XMM-Newton/EPIC or Chandra (ACIS) detector(s) whose data was used for the fitting of the X-ray spectra: m1 = MOS1, m2 = MOS2, pn = pn, all = MOS1 + MOS2 + pn. Notes indicate the origin of $N_{\rm H}$, kT, and $L_{\rm X}$ for objects with no usable DROXO detection (Sect. 3.1.2): 1$L_{\rm X}$ from ACIS count-rate; 2 $L_{\rm X}$ upper limit from DROXO data; 3 $N_{\rm H}$ and kT from the spectral analysis of Chandra ACIS data by Imanishi et al. (2001), $L_{\rm X}$ from ACIS count-rate; 4 $N_{\rm H}$, kT, and $L_{\rm X}$ from Imanishi et al. (2001, )tex2html_wrap_inline3430# corrected for the differences in the assumed distance and energy band#.

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