Table 2: Catalogue of convergence peaks / galaxy clusters in CFHTLS Deep fields.
ID Convergence peak Optical counterpart(s) X-ray counterpart
  $\alpha$ $\delta$ $\nu$ $\sigma_{v,{\rm lens}}$ $z_{\rm tomo}$ $\Delta(\alpha,\delta)$ $z_{\rm phot}$ $\sigma_{v,{\rm lens}}$ $\Lambda$ $L_{{\rm X},[0.5-2.0]}$ $T_{\rm X}$
  J2000 J2000   $~ {\rm km~ s}^{-1}$   arcsec   $~ {\rm km~ s}^{-1}$   1043 erg/s keV
Cl-01 $22^{\rm h}16^{\rm m}58^{\rm s}$ $-17^{\rm o}25{\rm '}10{\rm ''}$ 6.2 $680^{\rm + 80}_{- 70}$ $0.16^{\rm +0.10}_{-0.08}$ (-8, 1) $0.139^{\rm +0.007}_{-0.007}$ $600^{\rm + 85}_{-105}$ $ 56^{\rm + 8}_{- 8}$ $14.5^{\rm +0.2}_{-0.2}\;^{a}$  
Cl-02 $02^{\rm h}24^{\rm m}27^{\rm s}$ $-04^{\rm o}50{\rm '}34{\rm ''}$ 5.5 $760^{\rm +125}_{-105}$ $0.52^{\rm +0.14}_{-0.11}$ (34, 13) $0.497^{\rm +0.011}_{-0.011}$ $683^{\rm +113}_{-142}$ $ 69^{\rm + 9}_{- 9}$    
Cl-03 $02^{\rm h}27^{\rm m}24^{\rm s}$ $-04^{\rm o}32{\rm '}19{\rm ''}$ 4.1 $680^{\rm +110}_{-100}$ $0.35^{\rm +0.11}_{-0.10}$ (2,-11) $0.286^{\rm +0.012}_{-0.012}$ $611^{\rm + 88}_{-108}$ $27^{\rm + 6}_{- 6}$ $\sim $$1.5\;^{b}$ $1.02^{\rm +0.19}_{-0.15}$
Cl-04 $02^{\rm h}25^{\rm m}24^{\rm s}$ $-04^{\rm o}10{\rm '}48{\rm ''}$ 4.1 $460^{\rm + 90}_{- 90}$ $0.00^{\rm +0.20}_{-0.50}$ - - - - X X
Cl-05 $02^{\rm h}25^{\rm m}21^{\rm s}$ $-04^{\rm o}41{\rm '}33{\rm ''}$ 4.0 $460^{\rm +155}_{-100}$ $0.06^{\rm +0.25}_{-0.20}$ (27, 38) $0.269^{\rm +0.014}_{-0.014}$ $457^{\rm +116}_{-159}$ $21^{\rm + 5}_{- 5}$ $\sim $$5.2\;^{c}$ $2.02^{\rm +0.49}_{-0.28}$
Cl-06 $14^{\rm h}19^{\rm m}01^{\rm s}$ $+52^{\rm o}36{\rm '}43{\rm ''}$ 3.8 $490^{\rm +120}_{-120}$ $0.09^{\rm +0.18}_{-0.18}$ (-1, 2) $0.533^{\rm +0.025}_{-0.025}$ $654^{\rm +132}_{-175}$ $19^{\rm + 5}_{- 5}$    
Cl-07 $02^{\rm h}27^{\rm m}40^{\rm s}$ $-04^{\rm o}51{\rm '}38{\rm ''}$ 3.8 $570^{\rm +130}_{-120}$ $0.22^{\rm +0.17}_{-0.16}$ (-25, 11) $0.292^{\rm +0.019}_{-0.019}$ $521^{\rm +114}_{-154}$ $33^{\rm + 7}_{- 7}$ $\sim $$6.5\;^{d}$ $1.71^{\rm +0.15}_{-0.11}$
Cl-08 $10^{\rm h}01^{\rm m}21^{\rm s}$ $+02^{\rm o}22{\rm '}58{\rm ''}$ 3.7 $635^{\rm +215}_{-215}$ $0.44^{\rm +0.18}_{-0.29}$ (-3, -27) $0.735^{\rm +0.012}_{-0.012}$ $416^{\rm +331}_{-416}$ $156^{\rm +13}_{-13}$    
Cl-09 $09^{\rm h}59^{\rm m}42^{\rm s}$ $+02^{\rm o}32{\rm '}20{\rm ''}$ 3.7 $680^{\rm +270}_{-220}$ $0.47^{\rm +0.17}_{-0.20}$ - - - -    
Cl-10 $02^{\rm h}27^{\rm m}16^{\rm s}$ $-04^{\rm o}07{\rm '}37{\rm ''}$ 3.7 $480^{\rm + 90}_{- 90}$ $0.16^{\rm +0.14}_{-0.18}$ - - - - X X
Cl-11 $14^{\rm h}20^{\rm m}28^{\rm s}$ $+52^{\rm o}59{\rm '}22{\rm ''}$ 3.6 $400^{\rm +170}_{-150}$ $0.35^{\rm +0.15}_{-0.50}$ - - - -    
Cl-12 $14^{\rm h}19^{\rm m}02^{\rm s}$ $+53^{\rm o}08{\rm '}44{\rm ''}$ 3.6 $330^{\rm +110}_{-110}$ $0.00^{\rm +0.36}_{-0.50}$ (42, -14) $0.296^{\rm +0.023}_{-0.023}$ $401^{\rm +149}_{-272}$ $35^{\rm + 7}_{- 7}$    
Cl-13 $10^{\rm h}01^{\rm m}30^{\rm s}$ $+01^{\rm o}53{\rm '}04{\rm ''}$ 3.6 $530^{\rm + 80}_{-110}$ $0.18^{\rm +0.11}_{-0.15}$ - - - -    
Cl-14 $02^{\rm h}25^{\rm m}29^{\rm s}$ $-04^{\rm o}15{\rm '}34{\rm ''}$ 3.6 $460^{\rm +150}_{-140}$ $0.16^{\rm +0.50}_{-0.20}$ (23, 72) $0.153^{\rm +0.011}_{-0.011}$ $289^{\rm +144}_{-289}$ $ 2.0^{\rm +1.4}_{-1.4}$ $\sim $$2.4\;^{e}$ $1.34^{\rm +0.21}_{-0.10}$
            (3, -10) $0.569^{\rm +0.024}_{-0.024}$ $479^{\rm +184}_{-351}$ $25^{\rm +5}_{-5}$ X X
Notes: a ROSAT cluster $(22^{\rm h}16^{\rm m}56.2^{\rm s},-17^{\rm o}25{\rm '}25.5{\rm ''})$ at z=0.13 (de Grandi et al. 1999), b XMM-LSS cluster at z=0.31 (XLSSC13), c XMM-LSS cluster at z=0.26 (XLSSC25), d XMM-LSS cluster at z=0.29 (XLSSC22), e XMM-LSS cluster at z=0.14 (XLSSC41). All XMM-LSS data (b, c, d, e) are from (Willis et al. 2005; Pierre et al. 2006). Rows filled with "-'' are likely false detections without a reliable optical counterpart. Rows filled with "X'' are in the D1 field part of the XMM-LSS survey but not detected in X-rays. Cl-02 is part of D1 but lies in a region lost by the XMM-LSS survey (due to high flare rates). The second component of Cl-14 is not detected by the XMM-LSS as it may be hidden by the foreground z=0.14 component.

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