TY - JOUR

T1 - Effect of the environment on the fundamental plane of elliptical galaxies

AU - Evstigneeva, EA

AU - Reshetnikov, VP

AU - Sotnikova, NY

PY - 2002/1

Y1 - 2002/1

N2 - We present an analysis of the location of interacting E/S0 galaxies on the Fundamental Plane (FP). Using the NEMO package, we performed N-body simulations of close encounters and mergers of two self-gravitating spherical galaxies. Two models for encounting galaxies - Plummer's and Hernquist's - were used. The number of particles ranged from 20 000 to 50 000 per galaxy. The changes of central density, half-mass radius and central velocity dispersion were analysed. It was found that close encounters between galaxies alter noticeably the above parameters within a very short time interval (10(7)-10(8) years) just before the final merger. The amplitudes of parameter changes strongly depend on the initial mass concentration of a model. In some experiments we considered an encounter of two spherical galaxies with dark matter components. The effect of parameter changes was less pronounced than for the experiments without a dark halo. The results of the simulations were used to discuss the FP for interacting early-type galaxies.

AB - We present an analysis of the location of interacting E/S0 galaxies on the Fundamental Plane (FP). Using the NEMO package, we performed N-body simulations of close encounters and mergers of two self-gravitating spherical galaxies. Two models for encounting galaxies - Plummer's and Hernquist's - were used. The number of particles ranged from 20 000 to 50 000 per galaxy. The changes of central density, half-mass radius and central velocity dispersion were analysed. It was found that close encounters between galaxies alter noticeably the above parameters within a very short time interval (10(7)-10(8) years) just before the final merger. The amplitudes of parameter changes strongly depend on the initial mass concentration of a model. In some experiments we considered an encounter of two spherical galaxies with dark matter components. The effect of parameter changes was less pronounced than for the experiments without a dark halo. The results of the simulations were used to discuss the FP for interacting early-type galaxies.

KW - galaxies : kinematics and dynamics

KW - techniques : photometric

KW - KINEMATICAL DATA

KW - BINARY GALAXIES

KW - COMPACT-GROUPS

KW - ORIGINS

KW - CLUES

U2 - 10.1051/0004-6361:20011379

DO - 10.1051/0004-6361:20011379

M3 - статья

VL - 381

SP - 6

EP - 12

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 0004-6361

IS - 1

ER -