scholarly journals Phase-space mass bound for fermionic dark matter from dwarf spheroidal galaxies

2018 ◽  
Vol 475 (4) ◽  
pp. 5385-5397 ◽  
Author(s):  
Chiara Di Paolo ◽  
Fabrizio Nesti ◽  
Francesco L Villante
Keyword(s):  
Dark Matter ◽  
Phase Space ◽  
Dwarf Spheroidal Galaxies ◽  
Spheroidal Galaxies

scholarly journals New constraints on the mass of fermionic dark matter from dwarf spheroidal galaxies

2020 ◽  
Vol 501 (1) ◽  
pp. 1188-1201
Author(s):  
James Alvey ◽  
Nashwan Sabti ◽  
Victoria Tiki ◽  
Diego Blas ◽  
Kyrylo Bondarenko ◽  
...  
Keyword(s):  
Dark Matter ◽  
Phase Space ◽  
Pauli Principle ◽  
Big Bang ◽  
Big Bang Nucleosynthesis ◽  
Sterile Neutrinos ◽  
Dwarf Spheroidal Galaxies ◽  
Dark Matter Mass ◽  
Model Independent ◽  
Spheroidal Galaxies

ABSTRACT Dwarf spheroidal galaxies are excellent systems to probe the nature of fermionic dark matter due to their high observed dark matter phase-space density. In this work, we review, revise, and improve upon previous phase-space considerations to obtain lower bounds on the mass of fermionic dark matter particles. The refinement in the results compared to previous works is realized particularly due to a significantly improved Jeans analysis of the galaxies. We discuss two methods to obtain phase-space bounds on the dark matter mass, one model-independent bound based on Pauli’s principle, and the other derived from an application of Liouville’s theorem. As benchmark examples for the latter case, we derive constraints for thermally decoupled particles and (non-)resonantly produced sterile neutrinos. Using the Pauli principle, we report a model-independent lower bound of $m \ge 0.18\, \mathrm{keV}$ at 68 per cent CL and $m \ge 0.13\, \mathrm{keV}$ at 95 per cent CL. For relativistically decoupled thermal relics, this bound is strengthened to $m \ge 0.59\, \mathrm{keV}$ at 68 per cent CL and $m \ge 0.41\, \mathrm{keV}$ at 95 per cent CL, while for non-resonantly produced sterile neutrinos the constraint is $m \ge 2.80\, \mathrm{keV}$ at 68 per cent CL and $m \ge 1.74\, \mathrm{keV}$ at 95 per cent CL. Finally, the phase-space bounds on resonantly produced sterile neutrinos are compared with complementary limits from X-ray, Lyman α, and big bang nucleosynthesis observations.

scholarly journals J-factors for self-interacting dark matter in 20 dwarf spheroidal galaxies

2018 ◽  
Vol 98 (4) ◽  
Author(s):  
Sebastian Bergström ◽  
Riccardo Catena ◽  
Andrea Chiappo ◽  
Jan Conrad ◽  
Björn Eurenius ◽  
...  
Keyword(s):  
Dark Matter ◽  
Dwarf Spheroidal Galaxies ◽  
Spheroidal Galaxies

scholarly journals Jeans analysis for dwarf spheroidal galaxies in wave dark matter

2017 ◽  
Vol 468 (2) ◽  
pp. 1338-1348 ◽  
Author(s):  
Shu-Rong Chen ◽  
Hsi-Yu Schive ◽  
Tzihong Chiueh
Keyword(s):  
Dark Matter ◽  
Dwarf Spheroidal Galaxies ◽  
Wave Dark Matter ◽  
Spheroidal Galaxies

scholarly journals Evidence for Light-weight Local Group Dwarf Spheroidal Galaxies

2004 ◽  
Vol 220 ◽  
pp. 365-366
Author(s):  
J. R. Kuhn ◽  
D. Kocevski
Keyword(s):  
Dark Matter ◽  
Milky Way ◽  
Local Group ◽  
Light Weight ◽  
Natural Explanation ◽  
Dwarf Spheroidal Galaxies ◽  
Ursa Minor ◽  
Matter Component ◽  
Morphological State ◽  
Spheroidal Galaxies

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.

scholarly journals Too big to fail in light of Gaia

2019 ◽  
Vol 490 (1) ◽  
pp. 231-242 ◽  
Author(s):  
Manoj Kaplinghat ◽  
Mauro Valli ◽  
Hai-Bo Yu
Keyword(s):  
Dark Matter ◽  
Milky Way ◽  
Large Scatter ◽  
Too Big To Fail ◽  
Dwarf Spheroidal Galaxies ◽  
Ursa Minor ◽  
Spheroidal Galaxies

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.

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