Identification of Satellite Remnants in the Halo of our Galaxy with Gaia.

Details Identification of Satellite Remnants in the Halo of our Galaxy with Gaia. Identification of Satellite Remnants in the Halo of our Galaxy with Gaia.

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...20517602a&link_type=abstract

American Astronomical Society Meeting 205, #176.02; Bulletin of the American Astronomical Society, Vol. 37, p.380

Mathematics

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Scientific paper

We study the feasibility of identifying signatures of past accretion events in the halo of our galaxy using the Gaia database. Within current cosmological models, it is thought that galaxies are assembled from the bottom and thus galactic halos should retain signatures of this assemblage process.
The Gaia satellite will provide us with an unparallel database of kinematical and photometric information about our galactic halo. In order to interpret these data, it is necessary to perform N-body simulations of the process of accretion and tidal disruption of satellite galaxies. In most simulations to date, however, the simulated particles are projected in observable space without taking into consideration the stellar galactic background or the limitations of real surveys.
In this work we have concentrated our effort in addressing the problem of identifying satellite remnants in the Gaia database taking into consideration a realistic galactic background and modeling the observational errors of the Gaia mission. A mass, kinematic and photometric model of the galaxy is used to draw a Monte Carlo simulation of the Gaia survey. N-body simulations of the capture and destruction of a satellite are introduced in the simulated survey assuming a total luminosity, mass and age for the satellite. We then explore the feasibility of detecting the satellite in the angular momentum vs. energy space.
This work was done with support from UNAM-DGAPA grants IN113403 and IN111803, as well as CONACyT grant 27678-E.

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