Abstract
We investigate the association of Whiting 1 with the Sagittarius tidal stream by obtaining radial velocities for a sample of 101 stars observed with VIMOS. Our results reveal the presence of a component of the Sagittarius tidal stream with a radial velocity – and distance – compatible with that of the globular cluster. Therefore, we conclude that Whiting1 was formed in the interior of the Sagittarius dwarf spheroidal galaxy and later accreted by the Milky Way. In addition, our data also reveal the detection for the first time of an ancient wrap of the Sagittarius tidal stream along the same line-of-sight and at the same heliocentric distance.
Highlights
The accretion of massive satellites is believed to have contributed to the formation of a significant fraction of galaxy haloes by transferring a large amount of gas, stars and globular clusters (GC)
Compelling evidence for the latter comes from the GC systems of nearby galaxies (e.g. M31), where a large fraction of their globulars seems to align with tidal streams (e.g., [8])
The most pronounced accretion event in the Galaxy is the one corresponding to the Sagittarius (Sgr; [3]) dwarf spheroidal and its associated stellar structure, the so-called Sgr tidal stream (e.g., [4])
Summary
The accretion of massive satellites is believed to have contributed to the formation of a significant fraction of galaxy haloes by transferring a large amount of gas, stars and globular clusters (GC). Compelling evidence for the latter comes from the GC systems of nearby galaxies (e.g. M31), where a large fraction of their globulars seems to align with tidal streams (e.g., [8]).
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