Relics of dissipational merging and past violent starbursts in elliptical galaxies - the gE galaxy NGC 4365.

Details Relics of dissipational merging and past violent starbursts in elliptical galaxies - the gE galaxy NGC 4365. Relics of dissipational merging and past violent starbursts in elliptical galaxies - the gE galaxy NGC 4365.

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...298..405s&link_type=abstract

Astronomy and Astrophysics, v.298, p.405

Astronomy and Astrophysics

Astrophysics

60

Galaxies: Elliptical And Lenticular, Cd, Galaxies: Kinematics And Dynamics, Galaxies: Abundances, Galaxies: Formation, Galaxies: Interactions, Galaxies: Individual: Ngc 4365

Scientific paper

The Virgo elliptical galaxy NGC 4365 harbours a kinematically decoupled, counter-rotating core region. Its line-of-sight integrated velocity distributions are studied along 3 spectroscopic axes using Gauss-Hermite moments and double-gaussian line models. Stellar populations are investigated through high-resolution (B-R) colour photometry and spectroscopic absorbtion line indices Mg_2_ , Hβ and , which are compared to population models of Worthey (1992). We find consistent evidences for a distinct core population C of stars with disk or bar-like structure, high rotation velocity and low kinematic temperature (v/σ=1.3), flattened density distribution (ɛ_C_=0.39+/-0.07 versus ɛ_spheroid_=0.21 ...0.245) and a mass content of at least (8.1+/-2.5) .10 9Msun_. The metallicity of this core population shows an excessively flattened distribution (relative to the isophotes) and reaches values of at least 2.3Zsun_ at a population age of about <=(7 +/-1.5)Gyr. We favour a formation scenario with gas included in early hierarchical or late major mergers, where the gas is subject to strong dissipation effects and chemical enrichment and produces a violent starburst of order 10 2Msun_/yr. Our line indices show the well-known enhanced [Mg/Fe] of massive Es, but furthermore excessive enhancement of magnesium relative to iron in the innermost core region. This is interpreted as confirming evidence for a violent gaseous merger which probably over-produced SNii versus SNia due to a top-heavy IMF or because of its burst-like star formation history.

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