To learn more about the properties of the Vela Supercluster (VSCL), located behind the Milky Way at cz ∼ 18,000 km s⁻¹, we determine the K _s -band luminosity function (LF) of VC04, the richest known galaxy cluster in the VSCL, and two other VSCL clusters (VC02 and VC08). The galaxy sample is based on NIR observations that are complete to an extinction-corrected absolute magnitude of MKso<−21.ͫ5 (∼2.ͫ5 below MK* ), within the clustercentric radius of r _c < 1.5 Mpc (∼70% of the Abell radius). For VC04, we obtained 90 new spectroscopic redshifts of galaxies, observed with the 11 m Southern African Large Telescope. We found the Schechter parameters of the VC04 LF to be M* = −24.ͫ41 ± 0.44, α = −1.10 ± 0.20, and ϕ* = 8.84 ± 0.20. Both the redshift data and the LF confirm VC04 to be a rich but not yet fully relaxed cluster. We independently determined the LF of VC04 on membership defined by the red-sequence method and demonstrated that this method can be used in the absence of high spectroscopic coverage over a cluster. This allowed us to determine the LFs of VC02 and VC08. We also derived the LFs of the Coma, Norma, and Virgo clusters to similar depth and extent as the VSCL clusters. We found that the Schechter parameters of VC04 are within 1σ uncertainties of these local clusters, as well as VC02 and VC08. We do not find significant differences between the LFs in the different cluster environments probed in this work down to MK*+2.ͫ5 .

中文翻译：

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船帆超星系团富星团VC04的K s 波段光度函数


为了更多地了解位于银河系后面 cz ∼ 18,000 km s ^-1的船帆座超星系团 (VSCL) 的特性，我们确定了 VC04（银河系中已知最丰富的星系团）的 K _s带光度函数 (LF)。 VSCL 和另外两个 VSCL 群集（VC02 和 VC08）。星系样本基于近红外观测，这些观测在 r _c < 1.5 Mpc (∼70阿贝尔半径的%）。对于 VC04，我们获得了 90 个新的星系光谱红移，这是用 11 m 南非大型望远镜观测到的。我们发现 VC04 LF 的 Schechter 参数为 M* = −24.ͫ41 ± 0.44、α = −1.10 ± 0.20 和 phi* = 8.84 ± 0.20。红移数据和 LF 都证实 VC04 是一个丰富但尚未完全松弛的星团。我们独立确定了 VC04 在由红色序列方法定义的成员资格上的 LF，并证明该方法可以在星团上缺乏高光谱覆盖的情况下使用。这使我们能够确定 VC02 和 VC08 的 LF。我们还导出了后发星团、诺玛星团和处女座星团的 LF，其深度和范围与 VSCL 星团相似。我们发现 VC04 的 Schechter 参数在这些局部簇以及 VC02 和 VC08 的 1σ 不确定性范围内。我们没有发现本工作中探索的不同集群环境中的 LF 之间存在显着差异，小至 MK*+2.ͫ5 。