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SALT and RR Lyrae variables Our Galaxy, The Magellanic Clouds and the Local Group
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First Robert Stobie SALT Workshop
Science with SALT Workshop Proceedings, Vol. 2, 2004
D.A.H. Buckley
SALT and RR Lyrae Variables: Our Galaxy, The
Magellanic Clouds and the Local Group
Michael Feast
Astronomy Department, University of Cape Town, Rondebosch, 7701,
South Africa.
mwf@artemisia.ast.uct.ac.za
Abstract. A review is given of the possibilities for the study of the
kinematics and metallicities of the old populations in galaxies of the Local
Group using SALT/PFIS observations of RR Lyrae variables.
1. Introduction
In her summary talk at the recent Carnegie Cosmology conference, Sandra Faber
(2003) made two predictions:
1. “The major era of chasing cosmological parameters is now closing”
2. “Understanding galaxy formation.....will continue to occupy cosmologists
for some time......But there is no fundamentally new physics 1 to be discovered
there.”
These are bold, perhaps rash, predictions, of the kind that are often falsified
by observations and SALT could well play a part in such falsification.
As regards galaxy formation, structure, and evolution, one gets some flavour
of the present situation by considering the dwarf spheroidal galaxies which are
often considered the simplest of systems. Below are summarized the conclusions
of some papers, all on dwarf spheroidals, published in the last few months.
On the one hand:
Dwarf spheroidals are formed by the coalescing of clusters in dark matter halos.
(astro-ph/0309202)
On the other:
Draco and UMi are weakly unbound systems - no significant dark matter.
(astro-ph/0309207)
But:
Draco is not the remnant of a tidally disrupted satellite but probably is strongly
dark matter dominated.
(ApJ 589, 798, 2003)
Though:
It is impossible to reproduce the tidal tail of UMi if it has a large dark matter
1As distinct, presumably, from new and unusual applications of known physics.
1
2 Feast
content.
(ApJ 586, L123, 2003)
But again:
UMi is one of the most dark
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