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Hot gas in Milky Way size galaxies at z=0

Published online by Cambridge University Press:  21 March 2017

Santi Roca-Fàbrega
Affiliation:
Racah Institute of Physics, The Hebrew University, Jerusalem 91904, Israel email: santi.roca@mail.huji.ac.il
Pedro Colin
Affiliation:
Instituto de Radioastronomía y Astrofísica, UNAM, Morelia, Michoacán 58089, México
Octavio Valenzuela
Affiliation:
Instituto de Astronomía, UNAM, Ciudad Universitaria, México D.F.
Francesca Figueras
Affiliation:
IEEC-ICCUB, Martí i Franquès, 1, E-08028 Barcelona
Yair Krongold
Affiliation:
Instituto de Astronomía, UNAM, Ciudad Universitaria, México D.F.
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Abstract

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We present a new set of cosmological Milky Way size galaxy simulations using ART. In our simulations the main system has been evolved inside a 28 Mpc cosmological box with a spatial resolution of 109 pc. At z=0 our systems have an Mvir = 6 − 8 × 1011 M. In several of out models we have observed how a well defined disk is formed inside the dark matter halo and the overall amount of gas and stars is comparable with MW observations. Several non-axisymmetric structures arise out of the disk: spirals, bars and also a warp. We have also observed that a huge reservoir of hot gas is present at large distances from the disk, embedded in the dark matter halo region, accounting for only a fraction of the ”missing baryons”. Gas column density, emission (EM) and dispersion (DM) measure have been computed from inside the simulated disk at a position of 8 kpc from the center and in several directions. Our preliminary results reveal that the distribution of hot gas is non-isotropic according with observations (Gupta et al. 2012, Gupta et al. 2014). Also its metallic content presents a clear bimodality what is a consequence of a recent accretion of a satellite galaxy among others. After a careful analysis we confirm that due to the anisotropy in the gas distribution a new observational parameter needs to be defined to recover the real distribution of hot gas in the galactic halo (Roca-Fàbrega et al. 2016).

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2017 

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