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The fundamental plane of brightest cluster galaxies and isolated elliptical galaxies

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Abstract

This work aims to investigate the fundamental plane, the Kormendy, the Faber-Jackson, and the size-luminosity relations for two galaxy samples (brightest cluster galaxies (BCGs) and isolated elliptical galaxies (IEs)) in different environments. These relations are investigated in different wavelength bands, griz, of the Sloan Digital Sky Survey (SDSS). We constructed a sample of 2002 BCGs from the redMaPPer clusters catalog with spectroscopic redshifts in the range (\(0.076 \leqslant \textit{z} \leqslant 0.394\)). The sample of IEs consists of 550 objects and is extracted from the catalog of isolated galaxies (SDSS-based Isolated Galaxies, SIG) with spectroscopic redshifts range (\(0.01 \leqslant \textit{z} \leqslant 0.08\)). In general, we found that slopes of all studied scaling relations are waveband dependent except for the Faber-Jackson relation. The fundamental plane (FP) for both samples steepens as one moves from shorter to longer wavelengths. We found that BCGs lie on a different FP from that of IEs. In average the coefficient a of BCGs is larger than that of IEs by about 5\(\sigma \), while the coefficient b is larger by about 11\(\sigma \). By studying the Kormendy relation (KR), we found that its slope varies through the waveband for both samples. Also, the slope of BCGs is smaller than that of IEs by about 7\(\sigma \), while the intercept is smaller by about 12\(\sigma \). We also examined the Faber-Jackson (FJ) relation and found that its slope is similar for all wavebands for both samples. BCGs defines a steeper FJ relation than IEs such that \(\mbox{L} \varpropto \sigma ^{6.25}\) for BCGs and \(\mbox{L} \varpropto \sigma ^{2.63}\) for IEs. We also studied the size-luminosity relation and found that its slope is decreasing slightly with waveband for both samples. We also found that BCGs define a steeper size-luminosity relation than IEs, in average the slope of BCGs is greater than that of IEs by \(\sim 7\sigma \).

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Acknowledgements

Authors acknowledge the help and fruitful discussions with Dr. Abdelrazek Shaltout, Astronomy Department, Faculty of Science, Al-Azhar University, Cairo, Egypt. Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/.

The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington.

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  1. National Research Institute of Astronomy and Geophysics (NRIAG), 11421, Helwan, Cairo, Egypt

    R. M. Samir, A. Takey & A. A. Shaker

  2. Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima, 739-8526, Japan

    A. Takey

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Appendix

Appendix

We have investigated the Faber-Jackson and Size-Luminosity relations for both BCGs and IEs samples in Sects. 4.3 and 4.4. In these relations, the independent variable is the luminosity in different wavebands griz. There are some galaxies from both samples with luminosities in the same narrow range (log Lr: 10.6 – 11.0 L⊙). Figure 5 shows the distribution of the luminosities in the r-band for both samples. Also, the overlapping luminosity range is shown in the figure. For the Faber-Jackson relation, the dependent variable is log\(\sigma _{0}\). Figure 6 shows the distributions of log\(\sigma _{0}\) of BCGs and IEs in the overlapping luminosity range. In the same way, Fig. 7 shows the distribution of logR50 (the dependent variable of the size luminosity relation) of both samples in the same luminosity overlapping range.

Fig. 6
figure 6

Distribution of log\(\sigma _{0}\) of BCGs (red dotted line) and IEs (green solid line) in the overlapped luminosity range from 10.6 to 11.0 L⊙ in r band

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Fig. 7
figure 7

Distribution of \(\log \mbox{R}_{50}\) of BCGs (red dotted line) and IEs (green solid line) in the overlapped luminosity range in r band

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Samir, R.M., Takey, A. & Shaker, A.A. The fundamental plane of brightest cluster galaxies and isolated elliptical galaxies. Astrophys Space Sci 365, 142 (2020). https://doi.org/10.1007/s10509-020-03857-8

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