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Detectability of Ultra Faint Dwarf Galaxies with Gaia

Published online by Cambridge University Press:  17 July 2015

C. Mateu
Affiliation:
Instituto de Astronomía, Universidad Nacional Autónoma de México (UNAM), Ensenada B.C., México Centro de Investigaciones de Astronomía (CIDA), Mérida, Venezuela
T. Antoja
Affiliation:
Instituto de Astronomía, Universidad Nacional Autónoma de México (UNAM), Ensenada B.C., México
L. Aguilar
Affiliation:
ESA, European Space Research and Technology Centre, Noordwijk, The Netherlands
F. Figueras
Affiliation:
Departament d'Astronomia i Meteorologia, Institut de Ciències del Cosmos, Universitat de Barcelona, Barcelona, Spain
A. Brown
Affiliation:
Sterrewacht Leiden, Leiden, The Netherlands
E. Antiche
Affiliation:
Departament d'Astronomia i Meteorologia, Institut de Ciències del Cosmos, Universitat de Barcelona, Barcelona, Spain
F. Hernández-Pérez
Affiliation:
Centro de Investigaciones de Astronomía (CIDA), Mérida, Venezuela
O. Valenzuela
Affiliation:
Instituto de Astronomía, Universidad Nacional Autónoma de México, México DF, México
A. Aparicio
Affiliation:
Instituto de Astrofísica de Canarias, Tenerife, Spain
S. Hidalgo
Affiliation:
Instituto de Astrofísica de Canarias, Tenerife, Spain
H. Velázquez
Affiliation:
Instituto de Astronomía, Universidad Nacional Autónoma de México (UNAM), Ensenada B.C., México
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Abstract

We present a technique to detect Ultra-Faint Dwarf Galaxies (UFDs) in the Galactic Halo, using sky and proper motion information.The method uses wavelet transforms to detect peaks in the sky and proper motion planes, and to evaluate the probability of these being stochastic fluctuations. We aim to map thoroughly the detection limits of this technique. For this, we have produced a library of 15,000 synthetic UFDs, embedded in the Gaia Universe Model Snapshot (GUMS) background (Robin et al. 2012), each at a different distance, different luminosity, half-light radius, velocity dispersion and center-of-mass velocity, varying in ranges that extend well beyond those spanned by known classical and ultra-faint dSphs. We use these synthetic UFDs as a benchmark to characterize the completeness and detection limits of our technique, and present our results as a function of different physical and observable parameters of the UFDs (see full poster for more details at https://gaia.ub.edu/Twiki/pub/GREATITNFC/ProgramFinalconference/Poster_UFGX_Bcn_C_Mateu.pdf).

Type
Research Article
Copyright
© EAS, EDP Sciences, 2015

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References

Robin, A.C., et al., 2012, A&A, 543, A100

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