SCALING RELATIONS IN DISSIPATIONLESS SPIRAL-LIKE GALAXY MERGERS

Journal Article · Sat Jun 20 04:00:00 EDT 2009 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/698/2/2023; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21307707

Aceves, H; Velazquez, H ^[1]

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1. Instituto de AstronomIa, Universidad Nacional Autonoma de Mexico, Apartado Postal 877, Ensenada BC 22800 (Mexico)

We determine both representations of the Fundamental Plane [FP; R {sub e} {proportional_to} {sigma} {sup a} {sub 0}(I){sup -b} {sub e} and R {sub e} {proportional_to} ({sigma}{sup 2} {sub 0}(I){sup -1} {sub e}){sup {lambda}}] and the luminosity-effective phase-space density (L {proportional_to} f {sup -{gamma}} {sub e}) scaling relation for N-body remnants of binary mergers of spiral-like galaxies. The main set of merger simulations involves a mass ratio of the progenitors in the range of about 1:1 to 1:5, harboring or not a bulge-like component, and are constructed using a cosmological motivated model. Equal-mass mergers are also considered. Remnants lead to average values for the scaling indices of (a) {approx} 1.6, (b) {approx} 0.6, ({lambda}) {approx} 0.7, and ({gamma}) {approx} 0.65. These values are consistent with those of K-band observations of ellipticals: (a) {approx} 1.5, (b) {approx} 0.8, ({lambda}) {approx} 0.7, and ({gamma}) {approx} 0.60. The b index is, however, not well reproduced. This study does not allow us to establish a conclusive preference for models with or without a bulge as progenitors. Our results indicate that the L-f {sub e} and FP scalings might be determined to a large extent by dissipationless processes, a result that appears to be in contradiction to other dissipationless results.

• OSTI ID: 21307707
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 698; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
GALAXIES
LUMINOSITY
MASS
PHASE SPACE
SIMULATION