2003/10/19 by Lisa J. Wright, Wright, Lisa J., Jeremiah P. Ostriker +6
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #Cosmology and Gravitation Theories #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0310513
19 pages and 23 figures, submitted to MNRAS
openalex publication_date 2003/10/19 · arxiv created 2003/10/22 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present the results of a series of gas dynamical cosmological simulations\nof the formation of individual massive field galaxies in the standard\nconcordance LCDM and in a LWDM cosmology. The galaxies form in an initial\nburst of star formation followed by accretion of small satellites. The\nsimulated galaxies are old (\≈ 10 Gyrs) hot stellar systems with\nmasses of \≈ 1.7 \× 1011 M odot. Baryonic matter dominates the\nmass in the luminous part of the galaxies up to \≈ 5 effective radii.\nThe LCDM galaxy is a slowly rotating spheroidal stellar system (E2) with\npredominantly disky isophotes. The line-of-sight velocity distributions deviate\nfrom Gaussian shape and h3 is anticorrelated with vlos. The\ncorresponding LWDM galaxy is more elongated (E3 - E4) and rotates faster. The\nanisotropy parameter (v/\σ)^* is close to unity. Within the uncertainties\nof M/L both galaxies follow the Fundamental Plane. We conclude that the\nproperties of the two galaxies simulated in the LCDM and LWDM cosmology are\nin good agreement with observations of intermediate mass elliptical or S0\ngalaxies (abstract abbreviated).\n