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Galaxy Clusters in the Line of Sight to Background Quasars. I. Survey Design and Incidence of Mg II Absorbers at Cluster Redshifts

  • Authors: S. Lopez, L. F. Barrientos, P. Lira, N. Padilla, D. G. Gilbank, M. D. Gladders, J. Maza, N. Tejos, M. Vidal, and H. K. C. Yee

Lopez et al. 2008 The Astrophysical Journal 679 1144.

  • Provider: AAS Journals

Caption: Fig. 4.

Cluster redshift path density, ﹩g_{c}( W^{\mathrm{min}\,}_{0},\, z_{i}) ﹩, of the high‐resolution sample (S1, ﹩W^{\mathrm{min}\,}_{0}=0.05﹩ Å; left) and low‐resolution sample (S2, ﹩W^{\mathrm{min}\,}_{0}=1.0﹩ Å; right). The thick line is for LOS‐cluster distances ﹩d< 2﹩ ﹩h^{-1}_{71}﹩ Mpc, the thin line for ﹩d< 1﹩ ﹩h^{-1}_{71}﹩ Mpc, and the dotted line for ﹩d< 0.5﹩ ﹩h^{-1}_{71}﹩ Mpc. The vertical dashed lines depict the redshift defined by the rEW detection thresholds. See § 4.2.2 for more details.

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