EDP Sciences
Free Access
Issue
A&A
Volume 508, Number 3, December IV 2009
Page(s) 1173 - 1191
Section Cosmology (including clusters of galaxies)
DOI https://doi.org/10.1051/0004-6361/200810644
Published online 27 October 2009

Online Material

Table 9:   $z_{\rm phot}$ accuracy derived from simulations for galaxies in the spectroscopic sample, based on the GR code.

Table 10:   $z_{\rm phot}$ accuracy expected for the faintest galaxies in the EDisCS sample, based on the GR code.

\begin{figure}
{\hspace*{6mm}\psfig{file=10644f17.ps,angle=270,width=6.2cm}\hsp...
...pace*{6mm}}
\par {\psfig{file=10644f19.ps,angle=270,width=7.4cm} }\end{figure} Figure 16:

Comparison between spectroscopic and photometric redshifts for the low-z sample, obtained with Hyperz ( top panel) and GR ( central panel) codes. Solid (red) circles, open (blue) circles, and crosses correspond to objects with good (type 1), medium (type 2) and tentative (type 3) spectroscopic redshift determinations, respectively. Dot-dashed lines display $z_{\rm spec}$  =  $z_{\rm phot}$  $\pm $ 0.1 to guide the eye. The bottom panel displays the $z_{\rm spec} - z_{\rm phot}$ distribution obtained for this sample with Hyperz (solid black line) and GR (dotted red line). Vertical lines indicate the mean $\langle \Delta_z \rangle$.

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\begin{figure}
{\hspace*{5mm}\psfig{file=10644f20.ps,angle=270,width=6.2cm}\hsp...
...pace*{5mm}}
\par {\psfig{file=10644f22.ps,angle=270,width=7.2cm} }\end{figure} Figure 17:

(Comparison between spectroscopic and photometric redshifts for the high-z sample, obtained with Hyperz ( top panel) and GR ( central panel) codes. Solid (red) circles, open (blue) circles, and crosses correspond to objects with good (type 1), medium (type 2) and tentative (type 3) spectroscopic redshift determinations, respectively. Dot-dashed lines display $z_{\rm spec}$  =  $z_{\rm phot}$  $\pm $ 0.1 to guide the eye. The bottom panel displays the $z_{\rm spec} - z_{\rm phot}$ distribution obtained for this sample with Hyperz (solid black line) and GR (dotted red line). Vertical lines indicate the mean $\langle \Delta_z \rangle$.

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\begin{figure}
\par\psfig{file=10644f23.eps,width=9cm}
\end{figure} Figure 18:

A comparison of $P_{\rm clust}$ computed by the two different photometric redshift codes for the clusters with BVIK photometry. The black open circles represent all galaxies with I<24.5. The solid red squares are spectroscopically confirmed members and the solid green triangles are spectroscopically confirmed non-members. There is a broad correlation of $P_{\rm clust}$ between the two codes, such that the overwhelming number of galaxies have low $P_{\rm clust}$ for both methods with a smooth distribution of higher $P_{\rm clust}$ galaxies extending to the upper right, coincident with the confirmed members. The blue lines indicate the $P_{\rm thresh}$ values for each code that were determined to reject jointly the largest number of non-members, while retaining at least $90\%$ of the confirmed members. Objects to the left of the vertical blue line or beneath the horizontal blue line are flagged as interlopers.

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\begin{figure}
\par\psfig{file=10644f24.eps,width=9cm}
\end{figure} Figure 19:

Same as Fig. 18 but for the clusters with VRIJK photometry.

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\begin{figure}
\par\psfig{file=10644f25.eps,width=8.8cm}
\end{figure} Figure 20:

The histogram of $P_{\rm clust}$ values for the photometric sample (solid line) versus that of the spectroscopic sample (dotted line). Panel  a) is for the high-z sample at I<22.5 and panel  b) is for the low-z sample at I<22. In each case, the histograms represent the fraction of the total number of objects over all $P_{\rm clust}$.

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\begin{figure}
\par\psfig{file=10644f26.eps,width=9cm}
\end{figure} Figure 21:

Same as Fig. 14 except for Cl1420-1236.

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\begin{figure}
\par\psfig{file=10644f27.eps,width=9cm}
\end{figure} Figure 22:

Same as Fig. 14 except for Cl1040-1155.

Open with DEXTER

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