Issue |
A&A
Volume 417, Number 2, April II 2004
|
|
---|---|---|
Page(s) | 437 - 442 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20034368 | |
Published online | 19 March 2004 |
Formation of giant globular cluster G1 and the origin of the M 31 stellar halo
1
School of Physics, University of New South Wales, Sydney 2052, Australia
2
Astronomical Institute, Tohoku University, Sendai, 980-8578, Japan e-mail: chiba@astr.tohoku.ac.jp
Corresponding author: K. Bekki, bekki@bat.phys.unsw.edu.au
Received:
20
September
2003
Accepted:
21
October
2003
We demonstrate that globular cluster G1 could have been formed
by tidal interaction between M 31 and a nucleated dwarf galaxy (dE,N).
Our fully self-consistent numerical simulations
show that during tidal interaction between M 31 and G1's progenitor dE,N
with mag and its nucleus mass of ~107
,
the dark matter and the outer stellar envelope of the dE,N are nearly
completely stripped whereas the nucleus can survive the tidal stripping
because of its initially compact nature.
The naked nucleus (i.e., G1) has orbital properties similar to those
of its progenitor dE,N.
The stripped stars form a metal-poor ([Fe/H] ~ -1) stellar halo around M 31
and its structure and kinematics depend strongly on the initial orbit of
G1's progenitor dE,N.
We suggest that the observed large projected distance of G1 from M 31 (~40 kpc)
can give some strong constraints
on the central density of the dark matter halo of dE,N.
We discuss these results in the context
of substructures of M 31's stellar halo recently revealed by
Ferguson et al. ([CITE]).
Key words: galaxies: halos / galaxies: individual: M 31 / galaxies: interactions / galaxies: star clusters / Galaxy: globular clusters: individual: ω Centauri / Galaxy: globular clusters: individual: Mayall II = G1
© ESO, 2004
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