Photometric redshifts and cluster tomography in the ESO Distant Cluster Survey

R. Pelló; G. Rudnick; G. De Lucia; L. Simard; D. I. Clowe; P. Jablonka; B. Milvang-Jensen; R. P. Saglia; S. D. M. White; A. Aragón-Salamanca; C. Halliday; B. Poggianti; P. Best; J. Dalcanton; M. Dantel-Fort; B. Fort; A. von der Linden; Y. Mellier; H. Rottgering; D. Zaritsky

doi:10.1051/0004-6361/200810644

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Volume 508 / No 3 (December IV 2009)

A&A, 508 3 (2009) 1173-1191

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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.
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