The Evolution of Galaxies in Clusters

We report on recent numerical investigations of the dynamical evolution of galaxies in clusters. Simulations of spiral galaxies falling into forming clusters show the development of the morphology-density relationship and the formation of regular and giant elliptical galaxies. The regular elliptical merger remnants end up in a fundamental plane very similar to the observed relation. The giant ellipticals have much in common with their real counterparts but their central velocity dispersions are too high. We also quantify the amount and distribution of diffuse light in clusters.

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The effect of environment on the fundamental plane of elliptical galaxies

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316010401 ◽

2014 ◽

Vol 11 (S308) ◽

pp. 471-472

Author(s):

R. Kipper ◽

A. Tamm ◽

P. Tenjes ◽

E. Tempel

Keyword(s):

Elliptical Galaxies ◽

Fundamental Relation ◽

Noticeable Effect ◽

Fundamental Plane ◽

Velocity Dispersions

AbstractWe study the effect of environment to fundamental relation of elliptical galaxies. We find that superclusters, filaments and groups give noticeable effect to slope of velocity dispersions while little to luminosity slope.

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The Stability of Axisymmetric Galaxy Models with Anisotropic Dispersions

Symposium - International Astronomical Union ◽

10.1017/s0074180900033040 ◽

1983 ◽

Vol 100 ◽

pp. 285-286

Author(s):

Tim de Zeeuw ◽

Marijn Franx ◽

Jacques Meys ◽

Karel Brink ◽

Harm Habing

Keyword(s):

Spiral Galaxies ◽

Theoretical Models ◽

Elliptical Galaxies ◽

Small Class ◽

Integrals Of Motion ◽

Equilibrium Configurations ◽

Velocity Dispersions ◽

The Stability

The possible equilibrium configurations for elliptical galaxies and the bulges of spiral galaxies are no longer thought to be confined to the small class of axisymmetric systems with isotropic velocity dispersions. Many of these systems are not supported by rotation but instead by anisotropic velocity dispersions which are maintained by nonclassical integrals of motion (e.g., Binney 1978), and may be triaxial. Few theoretical models for such systems exist (Schwarzschild 1981). Here we discuss some axisymmetric models that we have constructed by means of Schwarzschild's (1979) selfconsistent method, and in particular their stability.

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1.7. Secular dynamical evolution of spiral galaxies and the formation of galactic bulges

Symposium - International Astronomical Union ◽

10.1017/s0074180900083868 ◽

1998 ◽

Vol 184 ◽

pp. 29-30

Author(s):

Xiaolei Zhang

Keyword(s):

Spiral Galaxies ◽

Dynamical Evolution ◽

Galactic Bulge ◽

Secular Evolution ◽

Evolution Of Galaxies ◽

Hubble Sequence ◽

Accretion Process ◽

Hubble Time

We show that a recently discovered spiral-induced radial mass accretion process could account for the formation of the Galactic Bulge in a Hubble time. This process is thus expected to be important in the formation of bulges in spiral galaxies, and in the secular evolution of galaxies along the Hubble sequence from late to earlier types.

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The co-responsibility of mass and environment in the formation of lenticular galaxies

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320001908 ◽

2020 ◽

Vol 15 (S359) ◽

pp. 173-174

Author(s):

A. Cortesi ◽

L. Coccato ◽

M. L. Buzzo ◽

K. Menéndez-Delmestre ◽

T. Goncalves ◽

...

Keyword(s):

Active Galactic Nuclei ◽

Maximum Likelihood Method ◽

Spiral Galaxies ◽

Galactic Nuclei ◽

Rotation Velocity ◽

Elliptical Galaxies ◽

Likelihood Method ◽

Data Set ◽

Lenticular Galaxies ◽

Galaxies Kinematics

AbstractWe present the latest data release of the Planetary Nebulae Spectrograph Survey (PNS) of ten lenticular galaxies and two spiral galaxies. With this data set we are able to recover the galaxies’ kinematics out to several effective radii. We use a maximum likelihood method to decompose the disk and spheroid kinematics and we compare it with the kinematics of spiral and elliptical galaxies. We build the Tully- Fisher (TF) relation for these galaxies and we compare with data from the literature and simulations. We find that the disks of lenticular galaxies are hotter than the disks of spiral galaxies at low redshifts, but still dominated by rotation velocity. The mechanism responsible for the formation of these lenticular galaxies is neither major mergers, nor a gentle quenching driven by stripping or Active Galactic Nuclei (AGN) feedback.

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