Measurement of the Dark Matter Velocity Dispersion with Dwarf Galaxy Rotation Curves

Warm dark matter has, by definition, a velocity dispersion. Let vhms(a)=vhms(1)/a be the root-mean-square velocity of non-relativistic warm dark matter particles in the early universe at expansion parameter a. vhms(1) is an adiabatic invariant. We obtain vhms(1) in the core of 11 dwarf galaxies dominated by dark matter, from their observed rotation curves, up to a rotation and relaxation correction. We obtain a mean 0.490 km/s and standard deviation 0.160 km/s, with a distribution peaked at the lower end. We apply a mild, data driven, rotation and relaxation correction that obtains the adiabatic invariant in the core of the galaxies: vhms(1)=0.406 ±0.069 km/s. These two small relative standard deviations justify the prediction that the adiabatic invariant vhms(1) in the core of the galaxies is of cosmological origin if dark matter is warm. This result is in agreement with measurements of vhms(1) based on spiral galaxy rotation curves, galaxy ultra-violet luminosity distributions, galaxy stellar mass distributions, the formation of first galaxies, reionization, and the velocity dispersion cut-off mass.

Searching the Parameters of Dark Matter Halos on the Basis of Dwarf Galaxies’ Dynamics

Article devoted to searching the parameters of dark matter halos on the base of dwarf galaxies’ dynamics (Messier 32 and Leo I). For doing this, we propose the new approach founded on construction the coupled elliptical trajectory for a probe body in the gravitational fields of Newtonian potential and potential of dark matter’s halo. This allows more accuracy estimate its central density for the Navarro-Frenk-White profile and free parameter for the Einasto profile . Our result is in good correlation with results of other authors that are got by different numerical methods.

Measurements of the Dark Matter Mass, Temperature and Spin

We summarize several measurements of the dark matter temperature-to-mass ratio, or equivalently, of the comoving root-mean-square thermal velocity of warm dark matter particles vhrms(1). The most reliable determination of this parameter comes from well measured rotation curves of dwarf galaxies by the LITTLE THINGS collaboration: vhrms(1)=406±69 m/s. Complementary and consistent measurements are obtained from rotation curves of spiral galaxies measured by the SPARC collaboration, density runs of giant elliptical galaxies, galaxy ultra-violet luminosity distributions, galaxy stellar mass distributions, first galaxies, and reionization. Having measured vhrms(1), we then embark on a journey to the past that leads to a consistent set of measured dark matter properties, including mass, temperature and spin.

On the Dark Matter’s Halo Theoretical Description

We argued that the standard field scalar potential couldn’t be widely used for getting the adequate galaxies’ curve lines and determining the profiles of dark matter their halo. For discovering the global properties of scalar fields that can describe the observable characteristics of dark matter on the cosmological space and time scales, we propose the simplest form of central symmetric potential celestial-mechanical type, i.e. U(φ) = –μ/φ. It was shown that this potential allows get rather satisfactorily dark matter profiles and rotational curves lines for dwarf galaxies. The good agreement with some previous results, based on the N-body simulation method, was pointed out. A new possibility of dwarf galaxies’ masses estimation was given, also.

Expected LHAASO sensitivity to decaying dark matter signatures from dwarf galaxies gamma-ray emission

As a next-generation complex extensive air shower array with a large field of view,the large high altitude air shower observatory(LHAASO)is very sensitive to the very-high-energy gamma rays from^300 GeV to 1 PeV and may thus serve as an important probe for the heavy dark matter(DM)particles.In this study,we make a forecast for the LHAASO sensitivities to the gamma-ray signatures resulting from DM decay in dwarf spheroidal satellite galaxies(dSphs)within the LHAASO field of view.Both individual and combined limits for 19 dSphs incorporating the uncertainties of the DM density profile are explored.Owing to the large effective area and strong capability of the photon-proton discrimination,we find that LHASSSO is sensitive to the signatures from decaying DM particles above O(1)TeV.The LHAASO sensitivity to the DM decay lifetime reaches O(1026)∼O(1028)s for several decay channels at the DM mass scale from 1 TeV to 100 TeV.

Determination of dark matter distribution in Ursa Major III and constraints on dark matter annihilation

The recently discovered satellite dwarf galaxy Ursa Major III provides a promising opportunity to explore the signatures resulting from dark matter(DM)annihilation owing to its proximity and large J-factor.Given the absence of an excess ofγ-ray signatures originating from Ursa Major III,observations ofγ-rays,such as those from Fermi-LAT,can be utilized to set constraints on the DM annihilation cross-section.In this study,we determined the DM density profile and considered the relationship between DM density and velocity dispersion at different locations within Ursa Major III through Jeans analysis.We calculated the J-factor of Ursa Major III for s-wave annihilation along with the effective J-factors for p-wave and Sommerfeld enhanced annihilation scenarios.Employing these derived J-factors,we set stringent constraints on DM annihilation cross-sections in three scenarios.Given the substantial impact of member star identification on the J-factor of Ursa Major III,we further calculated J-factors under the exclusion of the largest velocity outlier.Our analysis reveals a notable reduction in the median value and an increase in the deviation of J-factors,thereby leading to considerably weaker constraints.

Status of dark matter detection

The detection of dark matter has made great progresses in recent years. We give a brief review on the status and progress in dark matter detection, including the progresses in direct detection, collider detection at LHC and focus on the indirect detection. The results from PAMELA, ATIC, Fermi-LAT and relevant studies on these results are introduced. Then we give the progress on indirect detection of gamma rays from Fermi-LAT and ground based Cerenkov telescopes. Finally the detection of neutrinos and constraints on the nature of dark matter are reviewed briefly.

Constraining the Earth-mass Primordial Black Hole Mergers Model of the Non-repeating FRBs Using the First CHIME/FRB Catalog

In this paper,we upgrade the constraints for the Earth-mass primordial black hole mergers model based on the first Canadian Hydrogen Intensity Mapping Experiment(CHIME)/fast radio burst(FRB)catalog.Assuming the null hypothesis that the observed non-repeating FRBs originate from Earth-mass primordial black hole mergers,we find that how the charges were distributed in the primordial black hole population is well described by a double powerlaw function with typical charge value of law function with typical charge value of q_(c)/10^(-5)=1.60_(-0.28)^(+0.28),where the power-law index α_(1)=2.33_(-0.18)^(+0.15) for q<q_(c) and α_(2)=4.56_(-0.26)^(+0.30)for q≥q_(c).Here,q represents the charge of the black hole in units of√GM,where M is the mass of the black hole.Furthermore,we infer the local event rate of the bursts is 8.8_(-2.1)^(+5.7)×10^(4)Gpc^(-3) yr^(-1),which indicates that an abundance of the primordial black hole population f■10^(-4) is needed to account for the observed FRBs by CHIME.The results of this paper lay the basis for further research on the electromagnetic radiation background generated by the merger of primordial black hole mergers.

New Expansion Dynamics Applied to the Planar Structures of Satellite Galaxies and Space Structuration

Recent observations of Dwarf Satellite Galaxies (DSG) show that they have a clear tendency to stay in particular planes. Explanations with standard physics remain controversial. Recently, I proposed a new explanation of the galactic flat rotation curves, introducing a new cosmic acceleration due to expansion. In this paper, I apply this new acceleration to the dynamics of DSG’s (without dark matter). I show that this new acceleration implies planar structures for the DSG trajectories. More generally, it is shown that this acceleration produces a space structuration around any massive center. It remains a candidate to explain several cosmic observations without dark matter.

Astrophysics: Macroobject Shell Model

The model proposes that Nuclei of all macroobjects (Galaxy clusters, Galaxies, Star clusters, Extrasolar systems) are made up of Dark Matter Particles (DMP). These Nuclei are surrounded by Shells composed of both Dark and Baryonic matter. This model is used to explain various astrophysical phenomena: Multi-wavelength Pulsars;Binary Millisecond Pulsars;Gamma-Ray Bursts;Fast Radio Bursts;Young Stellar Object Dippers;Starburst Galaxies;Gravitational Waves. New types of Fermi Compact Stars made of DMP are introduced: Neutralino star, WIMP star, and DIRAC star. Gamma-Ray Pulsars are rotating Neutralino and WIMP stars. Merger of binary DIRAC stars can be a source of Gravitational waves.

Constraints on axion-like particles with different magnetic field models from the PKS 2155–304 energy spectrum

Axion-like particles(ALPs) are a promising kind of dark matter candidate particle that are predicted to couple with photons in the presence of magnetic fields. The oscillations between photons and ALPs traveling in the magnetic fields have been used to constrain ALP properties. In this work, we obtain some new constraints on the ALP mass ma and the photon-ALP coupling constant g with two different magnetic field models through TeV photons from PKS 2155–304. The first is the discrete-Φ model in which the magnetic field has the orientation angle Φ that changes discretely and randomly from one coherent domain to the next, and the second is the linearly-continuous-Φ model in which the magnetic field orientation angle Φ varies continuously across neighboring coherent domains. For the discrete-Φ model, we can obtain the best constraints on the ALP mass m1 = ma/(1 neV)= 0.1 and on the photon-ALP coupling constant g11= g/(10^-11 GeV^-1)= 5. The reasonable range of the ALP mass m1 is 0.08 ~ 0.2 when g11 = 5,and the only reasonable value of the photon-ALP coupling constant is g11 = 5 when m1 = 0.1. For the linearly-continuous-Φ model, we can obtain the best constraints on the ALP mass m1 = 0.1 and on the photon-ALP coupling constant g11 = 0.7. The reasonable range of the ALP mass m1 is 0.05 ~ 0.4 when g11= 0.7, and the reasonable range of the photon-ALP coupling constant g11 is 0.5 ~ 1 when m1 = 0.1.All of the results are consistent with the upper bound(g < 6.6 × 10^-11 GeV^-1, i.e., g11 < 6.6) set by the CAST experiment.

Searching for γ-ray emission from Reticulum Ⅱ by Fermi-LAT

Recently, many new dwarf spheroidal satellites（dSphs） have been discovered by the Dark Energy Survey（DES）. These dSphs are ideal candidates for probing for gamma-ray emissions from dark matter（DM） annihilation.However, no significant signature has been found by the Fermi-LAT dSph observations. In this work, we reanalyze the Fermi-LAT Pass 8 data from the direction of Reticulum II, where a slight excess has been reported by some previous studies. We treat Reticulum II（DES J0335.6-5403） as a spatially extended source, and find that no significant gamma-ray signature is observed. Based on this result, we set upper-limits on the DM annihilation cross section.