This article has an erratum: [https://doi.org/10.1051/0004-6361/201016348e]
Known superclusters at redshifts 0.2 < z < 1.0 with at least three member clusters.
|Name||RA||Dec||z||N(cluster)||rtrans × rlos [h-1 Mpc]||Mtot [× 1014 M⊙]||Further reading|
|CL0016||00:18:30||16:25:00||0.542 − 0.550||5||15 × 15||30 − 59||Tanaka et al. (2007)|
|MS0302||03:05:26||17:17:54||0.423||3||6 × 20||6.6 ± 1.0||Gavazzi et al. (2004)|
|A901/902||09:56:12||–09:58:12||0.165||4||3.0||7.24 ± 1.05||Heymans et al. (2008)|
|J1000+0231||10:00:12||02:31:12||0.65 − 0.85||3||13 × 400||60 ± 30||Guzzo et al. (2007)|
|A1437||12:00:28||03:20:18||0.125-0.138||7||87 × 46||−||Woudt (2009)|
|CL1604||16:04:14||43:15:00||0.84 − 0.96||9||13 × 100||> 3.6||Gal et al. (2008)|
|DXS1609||16:09:00||54:30:00||0.88 − 0.90||5||28 × 28||> 5||Swinbank et al. (2007)|
|SCL2243-0935||22:43:00||–09:35:00||0.435 − 0.456||> 5||45 × 50||30 ± 15||This paper|
Notes. In addition to redshift and the number of member clusters (or sub-structures in filaments), we report the extent transverse and along the line of sight, and an estimate for the total mass. Also included are A1437 at lower redshift, as it is similar in size and richness to SCL2243-0935, and A901/2 because together with MS0302 they are the only other two superclusters studied with weak lensing.
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