Applying scale-free mass estimators to the Local Group in Constrained Local Universe Simulations
Entity
UAM. Departamento de Física TeóricaPublisher
Royal Astronomical Society; Oxford University PressDate
2012-06-01Citation
10.1111/j.1365-2966.2012.21013.x
Monthly Notices of the Royal Astronomical Society 423.2 (2012): 1883-1895
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1111/j.1365-2966.2012.21013.xFunded by
YH has been partially supported by the Israel Science Foundation (13/08). NIL is supported by a grant by the Deutsche Forschungs Gemeinschaft. AKis supported by the Spanish Ministerio de Ciencia e Innovación (MICINN) in Spain through the Ramón y Cajal programme as well as the grants AYA 2009-13875-C03-02, AYA2009-12792-C03-03, CSD2009-00064 and CAM S2009/ESP-1496. GY acknowledges support from MICINN under research grants AYA2009-13875-C03-02, FPA2009-08958 and Consolider Ingenio SyeC CSD2007-0050.Project
Comunidad de Madrid S2009/ESP-1496/ASTROMADRIDEditor's Version
http://dx.doi.org/10.1111/j.1365-2966.2012.21013.xSubjects
Dark matter; Galaxies: haloes; Local Group; Methods: numerical; Galaxies: evolution; FísicaNote
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2012 RAS © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.Rights
© 2012 RAS; © 2012 The AuthorsAbstract
We use the recently proposed scale-free mass estimators to determine the masses of the Milky Way (MW) and Andromeda (M31) galaxy in a dark matter only Constrained Local Universe Simulation. While these mass estimators work rather well for isolated spherical host systems, we examine here their applicability to a simulated binary system with a unique satellite population similar to the observed satellites of MW and M31. We confirm that the scale-free estimators work also very well in our simulated Local Group galaxies with the right number of satellites which follow the observed radial distribution. In the isotropic case and under the assumption that the satellites are tracking the total gravitating mass, the power-law index of the radial satellite distribution N(< r) ∝ r 3-γ is directly related to the host's mass profile M(< r) ∝ r 1-α as α=γ- 2. The use of this relation for any given γ leads to highly accurate mass estimations which is a crucial point for observer, since they do not know a priori the mass profile of the MW and M31 haloes. We discuss possible bias in the mass estimators and conclude that the scale-free mass estimators can be satisfactorily applied to the real MW and M31 system
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Google Scholar:Di Cintio, Arianna
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Knebe, Alexander
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Libeskind, Noam I.
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Hoffman, Yehuda
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Yepes Alonso, Gustavo
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Gottlöber, Stefan
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