The formation of the Galactic bulge of the Milky Way

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ID: 97735
2012
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Abstract
We aim to determine if the bulge formed via mergers as predicted by Cold Dark Matter (CDM) theory, or from disk instabilities, as suggested by its boxy shape, or both processes. We are observing about 28,000 bulge stars in fields that span longitudes of − 31 to + 26° and latitudes of − 5° to − 10°, targeting mostly red clump giants and we are measuring stellar velocities and chemical abundances. We have almost concluded our observations and have analysed data of 23,000 stars. We find a cylindrical rotation profile for the bulge which blends smoothly out into the disk and from the [Fe/H] results we find the bulge to be comprised of separate components, with an underlying slowly rotating metal poor subsample which we believe to be the inner halo stars and metal weak thick disk. We find only a small [Fe/H] gradient with latitude in the bulge, of − 0.07dex/kpc. This weak gradient does not necessarily support a merger origin for our bulge and the composite nature of the bulge is consistent with formation out of the thin disk as per instability formation models.
Reference Key
k2012theepj Use this key to autocite in the manuscript while using SciMatic Manuscript Manager or Thesis Manager
Authors K., Freeman;M., Ness;
Journal epj web of conferences
Year 2012
DOI
DOI not found
URL
http://dx.doi.org/10.1051/epjconf/20121906003
Keywords
Medicine (General) Archaeology physics geography (general) business economics as a science economic theory. demography

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