The _{e}_{0})) and their host groups and clusters velocity dispersion (_{cl}_{0}/_{cl}_{cl}

#### Keywords

- brightest central galaxies
- BCGs
- galaxy clusters
- galaxy groups

#### MSC 2010

- 85-08
- 85A05
- 85A15

Brightest cluster galaxies (BCGs) are considered as one from the interesting objects that can explain some unsolved problems in studying galaxies. They are large, bright early type galaxies lying at centers of most galaxies groups and clusters. There are several unanswered questions related to BCGs nature. The principal mechanism for BCGs evolution is feedback rather than merging [1]. BCGs properties may also be affected by their clusters halo masses at low redshift. In general, BCGs follow the same fundamental plane (FP) of elliptical galaxies [6], but they have different FP and other scaling relations than those of isolated galaxies and the FP is a waveband dependent [8].

Previous studies found correlations between BCGs and their clusters properties such as cluster mass, richness and X-ray luminosity [2, 11, 12]. Understanding BCGs nature needs to study well environmental effects which affect on their physical properties [6, 7, 9].

In this work we present the sample and focus on investigating the relations between the physical properties of BCGs as the effective radii (_{e}_{o}_{cl}

This paper is organized as follows; Section 2 describes the selection of our BCGs sample, while in Section 3 we introduce and discuss our results and in Section 4 our main conclusions are summarized. In this paper we will adopt the cosmological parameters Ω_{m} = 0.3, Ω_{Λ} = 0.7, and Hubble constant H_{o} =70 km s^{−1} Mpc^{−1}.

BCGs and Brightest Groups Galaxies (BGGs) are selected using the catalog of [13] as it provides a huge list of galaxy clusters and groups in a broad redshift range. A sample of 17,924 elliptical galaxies in the _{e}_{o}_{cl}

In this section, we explore the relations between physical properties of the BCGs and their host clusters and groups. We consider absolute magnitude and central velocity dispersion as mass representatives of BCGs and BGGs. To measure the mass of cluster and group, we use _{cl}_{cl}_{cl}^{−1}.

In Figure 2, we plot the distribution of BCGs with their spectroscopic redshifts in the

Figure 3(a) shows the _{e}_{e}_{e}_{cl}_{cl}_{e}_{e}_{cl}_{e}

Figure 4(a) shows the _{r} < −22 mag) across redshift range, low redshift clusters and groups (z ≤ 0.04) host less luminous BCGs. These low redshift systems have also lower values of _{cl}_{cl}

Figure 5(a) presents _{o}_{o}_{o}_{cl}_{o}_{cl}_{o}_{o}_{cl}

We found that _{o}_{cl}

Figure 6 shows that the relation between _{o}_{cl}_{cl}_{o}_{cl}_{cl}_{o}_{cl}_{cl}_{o}_{cl}

The _{cl}_{o}_{o}_{cl}_{o}_{o}_{cl}_{cl}_{o}_{cl}_{o}_{cl}

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