The fundamental plane of brightest cluster galaxies and isolated elliptical galaxies

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

doi:10.1007/s10509-020-03857-8

Cited by 13 publications

(9 citation statements)

References 84 publications

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“…Since it relates the distribution of light and size of an ETG, the correlation has also been used extensively to understand the evolution of the ETGs and in particular, the size evolution over the cosmic time (Trujillo et al 2006;Longhetti et al 2007;Rettura et al 2010;Trujillo et al 2011;Naab & Ostriker 2017). Nevertheless, several things remain unclear, e.g., how the Kormendy relation varies across different environments in the local universe as well as in the intermediate redshift range; whether there is a cluster to cluster bias; how it depends on the evolutionary stages of the ETGs, colors, magnitude range, wavelength (Bernardi et al 2003b;Nigoche-Netro et al 2007;La Barbera et al 2010;Samir et al 2020). We study here the KR for five different samples.…”

Section: Kormendy Relationmentioning

confidence: 99%

Morphology, color-magnitude and scaling relations of galaxies in Abell 426

Khanday¹,

Saha²,

Nasser³

et al. 2022

Preprint

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We present photometric properties of 183 member galaxies in the Abell 426 cluster using the Sloan Digital Sky Survey (SDSS) imaging and spectroscopic observation. Detailed morphology based on visual classification followed by multi-component image decomposition of 179 galaxies is presented in the SDSS g, r, i-bands. More than 80% of the members are Early-type galaxies (ETGs), with elliptical, dwarf elliptical (dE), and lenticular morphology and follow the red-sequence in the color-magnitude diagram (CMD). With a few dEs and spirals in the blue cloud, the cluster CMD is nearly unimodal. The dEs are ∼ 2-mag fainter and follow a different Sersic index and central velocity dispersion distribution than their bright counterparts. Further, we establish the Kormendy relation (KR) and the Fundamental Plane relation (FPR) for 5 different samples of ETGs constructed based on derived physical parameters such as Sersic index, concentration, central velocity dispersion in g, r, i-bands. The mean r-band slope and zero-point of the KR are 3.02 ± 0.1 and 18.65 ± 0.03 in close agreement to other cluster ellipticals in the local and higher redshift. Kinematics-based ETG sample produces the least scatter in KR with zero-point getting brighter by ∼ 1.3 mag from g to i band. The dEs and other low-mass ETGs follow the KR with a similar slope but with ∼ 1.3 mag fainter zero-point and form a parallel KR.The bright ellipticals follow an FPR with 𝑎 = 1.37 ± 0.003, 𝑏 = 0.35 ± 0.05 and 𝑐 = −9.37 ± 0.02 in the r-band; galaxies tend to deviate from this relation at the low-mass end. A catalog with morphology and 2D structural analysis is available online.

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Section: Kormendy Relationmentioning

confidence: 99%

Morphology, color-magnitude and scaling relations of galaxies in Abell 426

Khanday¹,

Saha²,

Nasser³

et al. 2022

Preprint

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“…All parameters in our sample are obtained and updated from the SDSS-DR16. Physical properties of BCGs and BGGs (the effective radius, absolute magnitude and central velocity dispersion (σ o )) are derived and corrected as in Samir et al (2020). The velocity dispersion of host groups and clusters (σ cl ) are taken from Wang et al (2014).…”

Section: Galaxy Samplementioning

confidence: 99%

“…BCGs properties may also be affected by their cluster halos mass at low redshift. BCGs Fundamental Plane (FP) in general follow the same FP of normal clusters Samir et al (2011), but BCGs FP and scaling relations are not the same as those of isolated galaxies and the FP is a waveband dependent Samir et al (2020).…”

Section: Introductionmentioning

confidence: 99%

Possible Relations between Brightest Central Galaxies and Their Host Galaxies Clusters and Groups

Samir

Shaker

2021

Applied Mathematics and Nonlinear Sciences

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The r-band of the Sloan Digital Sky Survey (SDSS) for 17,924 brightest cluster galaxies (BCGs) in clusters and groups within 0.02 ⩽ z ⩽ 0.20 are used to study possible environmental relations affecting the nature of these galaxies. We find a correlation between BCGs physical properties (the effective radius (Re ), absolute magnitude and central velocity dispersion (σ 0)) and their host groups and clusters velocity dispersion (σcl ). This type of relations suggests that the most massive groups or clusters host larger central galaxies. On the other hand, the σ 0/σcl ratio as a function of σcl is consistent with [10].

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“…For example, the scaling relations between luminosities (or stellar masses) and velocity dispersions/sizes/ surface brightness are nonlinear (Choi et al 2007;Desroches et al 2007;Hyde & Bernardi 2009a;Bernardi et al 2011b;Kormendy & Bender 2013;Yoon et al 2017) in the sense that very luminous ETGs have lower velocity dispersions, larger sizes, and fainter surface brightness than expected values that are extrapolated from the scaling relations based on less luminous ETGs. Similarly, Bernardi et al (2007) and Samir et al (2020) showed that the scaling relations for brightest cluster galaxies (BCGs) are different from those for less luminous normal ellipticals.…”

Section: Introductionmentioning

confidence: 99%

The Fundamental Plane Is Not a Plane: Warped Nature of the Fundamental Plane of Early-type Galaxies and Its Implication for Galaxy Formation

Yoon

Park

2022

ApJ

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Based on 16,283 early-type galaxies (ETGs) in 0.025 ≤ z spec < 0.055 from Sloan Digital Sky Survey data, we show that the fundamental plane (FP) of ETGs is not a plane in the strict sense but is a curved surface with a twisted shape whose orthogonal direction to the surface is shifted as the central velocity dispersion (σ 0) or mean surface brightness within the half-light radius (μ e ) changes. When ETGs are divided into subsamples according to σ 0, the coefficient of μ e of the FP increases, whereas the zero-point of the FP decreases at higher σ 0. Taking the z band as an example, the coefficient of μ e rises from 0.28 to 0.36 as σ 0 increases from ∼100 to ∼300 km s−1. At the same time, the zero-point of the FP falls from −7.5 to −9.0 in the same σ 0 range. The consistent picture on the curved nature of the FP is also reached by inspecting changes in the FP coefficients for ETG subsamples with different μ e . By examining scaling relations that are projections of the FP, we suggest that the warped nature of the FP may originate from dry merger effects that are imprinted more prominently in ETGs with higher masses.

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The fundamental plane of brightest cluster galaxies and isolated elliptical galaxies

Cited by 13 publications

References 84 publications

Morphology, color-magnitude and scaling relations of galaxies in Abell 426

Morphology, color-magnitude and scaling relations of galaxies in Abell 426

Possible Relations between Brightest Central Galaxies and Their Host Galaxies Clusters and Groups

The Fundamental Plane Is Not a Plane: Warped Nature of the Fundamental Plane of Early-type Galaxies and Its Implication for Galaxy Formation

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