The quantity of dark matter in early-type galaxies and its relation to the environment

Nigoche-Netro, A.; Ramos-Larios, G.; Lagos, P.; Fuente, Eduardo de la; Ruelas-Mayorga, A.; Méndez-Abreu, J.; Kemp, S. N.; Díaz, Rubén

doi:10.1093/mnras/stz1786

Cited by 8 publications

(5 citation statements)

References 115 publications

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“…However, if a dark matter halo surrounds the galaxy, our method can be used to estimate the dark matter up to the distance between a companion and host galaxy if the dark halo is spherically symmetric. Therefore, the derived results are unaffected by the shape, rotation, or brightness profiles of the host galaxies (Campbell et al 2017;Nigoche-Netro et al 2019).…”

Section: Datamentioning

confidence: 96%

Dynamics of Companion Galaxies of Early-Type Galaxies

Chen,

Hwang

2020

Preprint

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We estimated the dynamical masses of 115 early-type galaxies (ETGs) by analyzing the dynamics of satellite and companion galaxies of these ETGs. We selected galaxies with absolute magnitudes between -22 and -25 in the K s -band from the Extragalactic Distance Database (EDD). We also selected 216 spiral galaxies for comparison. We employed a simple model to simulate the observed dynamical mass from satellite galaxies at various distances. Our simulations showed that the dynamical masses derived from satellite galaxies with elliptical orbits would be smaller than those with circular orbits even they contain the same dark mass halos. Therefore, relationships between the observed M dyn /M b distributions and distances would depend on orbital shapes. From the relationships between our observed M dyn /M b distributions and distances, we suggest that the satellite galaxies of the ETGs have relatively more elliptical orbits than those of the spiral galaxies have and the M dyn /M b of the ETGs are greater than that of the spiral galaxies.

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Section: Datamentioning

confidence: 96%

Dynamics of Companion Galaxies of Early-Type Galaxies

Chen,

Hwang

2020

Preprint

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“…Another way to explore the distribution of dark matter in ETGs through the PPS regions is to consider the difference between the dynamical (virial) mass and the stellar mass of galaxies. We can estimate the dynamical mass using the following expression: Poveda 1958;Nigoche-Netro et al 2019), where 𝐾 (𝑛) is a scale factor that depends on the Sérsic index 𝑛 as follows 𝐾 (𝑛) = 8.87 − 0.831𝑛 + 0.00241𝑛 2 (4) (Cappellari et al 2006), with the Sérsic indices taken from the catalog of Simard et al (2011). We also define the ratio 𝑀 dyn /𝑀 * as…”

Section: Difference Between Dynamical and Stellar Massmentioning

confidence: 99%

“…following the work of Nigoche-Netro et al (2019). We present the cumulative distribution functions of Δ𝑀 for the PPS samples in Figure 9, and use the Conover test to compare them against each other (Conover & Iman 1979).…”

Section: Difference Between Dynamical and Stellar Massmentioning

confidence: 99%

Late growth of early-type galaxies in low-z massive clusters

Ribeiro¹,

Nascimento²,

Morell³

et al. 2023

Preprint

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We study a sample of 936 early-type galaxies (ETGs) located in 48 low-z regular galaxy clusters with 𝑀 200 ≥ 10 14 𝑀 at 𝑧 < 0.1. We examine variations in the concentration index, radius, and color gradient of ETGs as a function of their stellar mass and loci in the projected phase space (PPS) of the clusters. We aim to understand the environmental influence on the growth of ETGs according to the time since infall into their host clusters. Our analysis indicates a significant change in the behavior of the concentration index 𝐶 and color gradient around 𝑀 * ≈ 2 × 10 11 𝑀 ≡ M * . Objects less massive than M * present a slight growth of 𝐶 with 𝑀 * with negative and approximately constant color gradients in all regions of the PPS. Objects more massive than M * present a slight decrease of 𝐶 with 𝑀 * with color gradients becoming less negative and approaching zero. We also find that objects more massive than M * , in all PPS regions, have smaller 𝑅 90 for a given 𝑅 50 , suggesting a smaller external growth in these objects or even a shrinkage possibly due to tidal stripping. Finally, we estimate different dark matter fractions for galaxies in different regions of the PPS, with the ancient satellites having the largest fractions, 𝑓 𝐷 𝑀 ≈ 65%. These results favor a scenario where cluster ETGs experience environmental influence the longer they remain and the deeper into the gravitational potential they lie, indicating a combination of tidal stripping + harassment, which predominate during infall, followed by mergers + feedback effects affecting the late growth of ancient satellites and BCGs.

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“…Another way to explore the distribution of dark matter in ETGs through the PPS regions is to consider the difference between the dynamical (virial) mass and the stellar mass of galaxies. We can estimate the dynamical mass using the following expression: Po v eda 1958 ;Nigoche-Netro et al 2019 ), where K ( n ) is a scale factor that depends on the S érsic index n as follows (Cappellari et al 2006 ), with the S érsic indices taken from the catalog of Simard et al ( 2011 ). We also define the ratio M dyn / M * as R package (Signorell et al 2016 ).…”

Section: Difference Between Dynamical and Stellar Massmentioning

confidence: 99%

Late growth of early-type galaxies in low-z massive clusters

Ribeiro

Nascimento

Morell

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We study a sample of 936 early-type galaxies (ETGs) located in 48 low-z regular galaxy clusters with M200 ≥ 1014 M⊙ at z < 0.1. We examine variations in the concentration index, radius, and color gradient of ETGs as a function of their stellar mass and loci in the projected phase space (PPS) of the clusters. We aim to understand the environmental influence on the growth of ETGs according to the time since infall into their host clusters. Our analysis indicates a significant change in the behavior of the concentration index C and color gradient around $M_{\ast } \approx 2\times 10^{11} ~M_\odot \equiv \tilde{M}_{\ast }$. Objects less massive than $\tilde{M}_{\ast }$ present a slight growth of C with M* with negative and approximately constant color gradients in all regions of the PPS. Objects more massive than $\tilde{M}_{\ast }$ present a slight decrease of C with M* with color gradients becoming less negative and approaching zero. We also find that objects more massive than $\tilde{M}_{\ast }$, in all PPS regions, have smaller R90 for a given R50, suggesting a smaller external growth in these objects or even a shrinkage possibly due to tidal stripping. Finally, we estimate different dark matter fractions for galaxies in different regions of the PPS, with the ancient satellites having the largest fractions, fDM ≈ 65%. These results favor a scenario where cluster ETGs experience environmental influence the longer they remain and the deeper into the gravitational potential they lie, indicating a combination of tidal stripping + harassment, which predominate during infall, followed by mergers + feedback effects affecting the late growth of ancient satellites and BCGs.

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The quantity of dark matter in early-type galaxies and its relation to the environment

Cited by 8 publications

References 115 publications

Dynamics of Companion Galaxies of Early-Type Galaxies

Dynamics of Companion Galaxies of Early-Type Galaxies

Late growth of early-type galaxies in low-z massive clusters

Late growth of early-type galaxies in low-z massive clusters

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