| Issue |
A&A
Volume 501, Number 2, July II 2009
|
|
|---|---|---|
| Page(s) | 485 - 494 | |
| Section | Extragalactic astronomy | |
| DOI | https://doi.org/10.1051/0004-6361/200911850 | |
| Published online | 19 May 2009 | |
Online Material
Appendix A: X-ray source catalog in the ``Daddi field'' and X-ray spectra of EROs
Table A.1: X-ray properties of the sources detected by Chandra in the ``Daddi field''.
![\begin{figure}
\par\includegraphics[angle=-90,width=10cm]{1850f207.ps}\par\inclu...
...1850f216.ps}\par\includegraphics[angle=-90,width=10cm]{1850f362.ps}
\end{figure}](/articles/aa/olm/2009/26/aa11850-09/img187.png) |
Figure A.1:
Chandra spectra (folded with the response of the ACIS-I instrument) of the three X-ray EROs with most counts in the 0.5-8 keV band.
While for the spectrum of ERO #2073 a single power law model was assumed,
for the remaining two objects absorption at the source rest-frame (using the spectroscopic
redshift for ERO #2160 and the photometric redshift for ERO #3629; see Table 1)
was included in the spectral fitting, as described in Sect. 4.2.
The three bottom panels illustrate the data/model ratio in units of |
| Open with DEXTER | |
.
![\begin{figure}
\par\includegraphics[angle=-90,width=10cm]{1850EROs.ps}
\end{figure}](/articles/aa/olm/2009/26/aa11850-09/img188.png) |
Figure A.2: Rest-frame X-ray spectrum of the 11 EROs that are individually detected in the Chandra observations. The underlying model consists of an absorbed power law. |
| Open with DEXTER | |
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