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• W3100263192 abstract "NGC 5128, a giant elliptical galaxy only ∼4 Mpc away, is the dominant member of a galaxy group of over 80 probable members. The Centaurus group provides an excellent sample for a kinematic comparison between the halo of NGC 5128 and its surrounding satellite galaxies. A new study, presented here, shows no kinematic difference in rotation amplitude, rotation axis, or velocity dispersion between the halo of NGC 5128, determined from over ∼340 of its globular clusters, and those of the Centaurus group as a whole. These results suggest NGC 5128 could be behaving in part as the inner component to the galaxy group, and could have begun as a large initial seed galaxy, gradually built up by minor mergers and satellite accretions, consistent with simple cold dark matter models. The masses and mass-to-light ratios in the B band, corrected for projection effects, are determined to be (1.3 ± 0.5) × 1012 M⊙ and 52 ± 22 M⊙ L for NGC 5128 out to a galactocentric radius of 45 kpc and (9.2 ± 3.0) × 1012 M⊙ and 153 ± 50 M⊙ L for the Centaurus group, consistent with previous studies." @default.
• W3100263192 created "2020-11-23" @default.
• W3100263192 creator A5081875036 @default.
• W3100263192 date "2006-01-01" @default.
• W3100263192 modified "2023-09-25" @default.
• W3100263192 title "The Centaurus Group and the Outer Halo of NGC 5128: Are They Dynamically Connected?" @default.
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• W3100263192 doi "https://doi.org/10.1086/508631" @default.
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