The LMC vs. the Milky Way

2019 ◽  
Vol 14 (S353) ◽  
pp. 123-127 ◽  
Author(s):  
Gurtina Besla ◽  
Nicolás Garavito-Camargo
Keyword(s):  
Dark Matter ◽  
Milky Way ◽  
Large Magellanic Cloud ◽  
Dark Matter Halo ◽  
Matter Distribution ◽  
Structure And Dynamics ◽  
Gravitational Perturbations ◽  
Satellite Galaxy ◽  
Stellar Halo ◽  
Dark Matter Distribution

AbstractRecent advancements in astrometry and in cosmological models of dark matter halo growth have significantly changed our understanding of the dynamics of the Local Group. The most dramatic changes owe to a new picture of the structure and dynamics of the Milky Way’s most massive satellite galaxy, the Large Magellanic Cloud (LMC), which is most likely on its first passage about the Milky Way and ten times larger in mass than previously assumed. The LMC’s orbit through the Milky Way’s dark matter and stellar halo will leave characteristic signatures in both density and kinematics. Furthermore, the gravitational perturbations produced by both direct tidal forcing from the LMC and the response of the halo to its passage will together cause significant perturbations to the orbits of tracers of the Milky Way’s dark matter distribution. We advocate for the use of basis field expansion methods to fully capture and quantify these effects.

scholarly journals Analysis of the very inner Milky Way dark matter distribution and gamma-ray signals

2016 ◽  
Vol 94 (12) ◽  
Author(s):  
V. Gammaldi ◽  
V. Avila-Reese ◽  
O. Valenzuela ◽  
A. X. Gonzalez-Morales
Keyword(s):  
Dark Matter ◽  
Milky Way ◽  
Gamma Ray ◽  
Matter Distribution ◽  
Dark Matter Distribution

scholarly journals Baryonic impact on the dark matter distribution in Milky Way-sized galaxies and their satellites

2016 ◽  
Vol 458 (2) ◽  
pp. 1559-1580 ◽  
Author(s):  
Qirong Zhu ◽  
Federico Marinacci ◽  
Moupiya Maji ◽  
Yuexing Li ◽  
Volker Springel ◽  
...  
Keyword(s):  
Dark Matter ◽  
Milky Way ◽  
Matter Distribution ◽  
Dark Matter Distribution

scholarly journals Bayesian reconstruction of the Milky Way dark matter distribution

2019 ◽  
Vol 2019 (09) ◽  
pp. 046-046 ◽  
Author(s):  
E.V. Karukes ◽  
M. Benito ◽  
F. Iocco ◽  
R. Trotta ◽  
A. Geringer-Sameth
Keyword(s):  
Dark Matter ◽  
Milky Way ◽  
Matter Distribution ◽  
Bayesian Reconstruction ◽  
Dark Matter Distribution

scholarly journals Dark Matter distribution in the Milky Way: microlensing and dynamical constraints

2011 ◽  
Vol 2011 (11) ◽  
pp. 029-029 ◽  
Author(s):  
Fabio Iocco ◽  
Miguel Pato ◽  
Gianfranco Bertone ◽  
Philippe Jetzer
Keyword(s):  
Dark Matter ◽  
Milky Way ◽  
Matter Distribution ◽  
Dynamical Constraints ◽  
Dark Matter Distribution

scholarly journals MC2: CONSTRAINING THE DARK MATTER DISTRIBUTION OF THE VIOLENT MERGING GALAXY CLUSTER CIZA J2242.8+5301 BY PIERCING THROUGH THE MILKY WAY

2015 ◽  
Vol 802 (1) ◽  
pp. 46 ◽  
Author(s):  
M. James Jee ◽  
Andra Stroe ◽  
William Dawson ◽  
David Wittman ◽  
Henk Hoekstra ◽  
...  
Keyword(s):  
Dark Matter ◽  
Milky Way ◽  
Galaxy Cluster ◽  
Matter Distribution ◽  
Dark Matter Distribution

scholarly journals The barred inner Milky Way: dynamical models from surveys

2017 ◽  
Vol 13 (S334) ◽  
pp. 73-81
Author(s):  
Ortwin Gerhard
Keyword(s):  
Dark Matter ◽  
Survey Data ◽  
Milky Way ◽  
Matter Distribution ◽  
Dynamical Models ◽  
Unique Case ◽  
Dynamical Equilibrium ◽  
Pattern Speed ◽  
Central Bulge ◽  
Dark Matter Distribution

AbstractThe Milky Way is a barred galaxy whose central bulge has a box/peanut shape and consists of multiple stellar populations with different orbit distributions. This review describes dynamical and chemo-dynamical equilibrium models for the Bulge, Bar, and inner Disk based on recent survey data. Some of the highlighted results include (i) stellar mass determinations for the different Galactic components, (ii) the need for a core in the dark matter distribution, (iii) a revised pattern speed putting corotation at ~6 kpc, (iv) the strongly barred distribution of the metal-rich stars, and (v) the radially varying dynamics of the metal-poor stars which is that of a thick disk-bar outside ~1 kpc, but changes into an inner centrally concentrated component with several possible origins. On-going and future surveys will refine this picture, making the Milky Way a unique case for studying how similar galaxies form and evolve.

scholarly journals Hot gas in Milky Way size galaxies at z=0

2016 ◽  
Vol 11 (S321) ◽  
pp. 72-74
Author(s):  
Santi Roca-Fàbrega ◽  
Pedro Colin ◽  
Octavio Valenzuela ◽  
Francesca Figueras ◽  
Yair Krongold
Keyword(s):  
Dark Matter ◽  
Column Density ◽  
Milky Way ◽  
Galactic Halo ◽  
Careful Analysis ◽  
Dark Matter Halo ◽  
Hot Gas ◽  
Satellite Galaxy ◽  
Real Distribution ◽  
Axisymmetric Structures

AbstractWe 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).

scholarly journals Origins of Stellar Halos

2015 ◽  
Vol 11 (S317) ◽  
pp. 1-8
Author(s):  
Kathryn V. Johnston
Keyword(s):  
Dark Matter ◽  
Milky Way ◽  
Stellar Populations ◽  
Observational Evidence ◽  
Dark Matter Halo ◽  
Theoretical Understanding ◽  
Stellar Halo ◽  
The One ◽  
Halo Population

AbstractThis contribution reviews ideas about the origins of stellar halos. It includes discussion of the theoretical understanding of and observational evidence for stellar populations formed “in situ” (meaning formed in orbits close to their current ones), “kicked-out” (meaning formed in the inner galaxy in orbits unlike their current ones) and “accreted” (meaning formed in a dark matter halo other than the one they currently occupy). At this point there is general agreement that a significant fraction of any stellar halo population is likely “accreted”. There is modest evidence for the presence of a “kicked-out” population around both the Milky Way and M31. Our theoretical understanding of and the observational evidence for an “in situ” population are less clear.

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