scholarly journals Constraining self-interacting dark matter with dwarf spheroidal galaxies and high-resolution cosmological N -body simulations

2022 ◽  
Vol 105 (2) ◽  
Toshihiro Ebisu ◽  
Tomoaki Ishiyama ◽  
Kohei Hayashi
2018 ◽  
Vol 98 (4) ◽  
Sebastian Bergström ◽  
Riccardo Catena ◽  
Andrea Chiappo ◽  
Jan Conrad ◽  
Björn Eurenius ◽  

2017 ◽  
Vol 468 (2) ◽  
pp. 1338-1348 ◽  
Shu-Rong Chen ◽  
Hsi-Yu Schive ◽  
Tzihong Chiueh

2004 ◽  
Vol 220 ◽  
pp. 365-366
J. R. Kuhn ◽  
D. Kocevski

A simple and natural explanation for the dynamics and morphology of the Local Group Dwarf Spheroidal galaxies, Draco (Dra) and Ursa Minor (UMi), is that they are weakly unbound stellar systems with no significant dark matter component. A gentle, but persistent, Milky Way (MW) tide has left them in their current kinematic and morphological state (the “parametric tidal excitation”). A new test of a dark matter dominated dS potential follows from a careful observation of the “clumpiness” of the dS stellar surface density.

2019 ◽  
Vol 490 (1) ◽  
pp. 231-242 ◽  
Manoj Kaplinghat ◽  
Mauro Valli ◽  
Hai-Bo Yu

ABSTRACT We point out an anticorrelation between the central dark matter (DM) densities of the bright Milky Way dwarf spheroidal galaxies (dSphs) and their orbital pericenter distances inferred from Gaia data. The dSphs that have not come close to the Milky Way centre (like Fornax, Carina and Sextans) are less dense in DM than those that have come closer (like Draco and Ursa Minor). The same anticorrelation cannot be inferred for the ultrafaint dSphs due to large scatter, while a trend that dSphs with more extended stellar distributions tend to have lower DM densities emerges with ultrafaints. We discuss how these inferences constrain proposed solutions to the Milky Way’s too-big-to-fail problem and provide new clues to decipher the nature of DM.

2020 ◽  
Vol 1468 ◽  
pp. 012011
Kohei Hayashi ◽  
Shigeki Matsumoto ◽  
Masahiro Ibe ◽  
Mino N. Ishigaki ◽  
Hajime Sugai ◽  

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