“Dark Matter” Science-Research, September 2021, Week 4 — summary from Astrophysics Data System, OSTI GOV and Arxiv

Astrophysics Data System — summary generated by Brevi Assistant

In these talks I define a theory of dark matter superfluidity created in the last couple of years. The dark matter fragments are axion-like, with masses of order eV. We analyzed 11 years of Fermi-LAT data corresponding to the sky regions of 7 dwarf irregular galaxies. For each DM version and dIrr, we create a spatial layout of the expected DM-induced gamma-ray signal to be used in the analysis of Fermi-LAT data. The form distortion of the presumed Milky Way dark matter halo can affect the regional thickness of dark matter and hence the direct discovery program. We take a look at the population of stellar rotation curves measured by SPARC and fit them to dark matter haloes that are distorted with a multipole thickness circulation, finding a dramatically better fit with prolate haloes over spherically symmetric ones. The vibrant advancement of stellar bars in common Λ CDM versions is dominated by angular energy loss to the dark matter haloes through dynamical rubbing. In normal balance haloes, the first phase-space thickness within the caught area is higher at reduced angular energy. Atom interferometry is a powerful experimental technique that can be used to look for the oscillation of atomic change powers induced by ultra-light scalar dark matter. In this work, we generalise the treatment of the time-dependent signal generated by a linearly-coupled scalar ULDM prospect for vertical atom gradiometers of any kind of length and locate modification elements that specifically influence the ULDM signal in short-baseline gradiometer arrangements. In this work, we offer a look at Dark Matter prospect bits generated at the Large Hadron Collider, the procedure of the production of DM fragments, alongside a new theoretical gauge boson signified by Z ^’ is governed by a model called Mono-Z ^’. No evidence for the presence of dark matter prospects was found, and 95 confidence level limits were established on the mass of the Z ^’ the mass of the dark matter candidate fragment, and the cutoff scale of the efficient field theory.

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OSTI GOV — summary generated by Brevi Assistant

Cold dark matter haloes contain a fairly smooth dark matter part in addition to a system of bound subhaloes. This new characterization of smooth halo profiles can be valuable for many analyses, such as lensing and dark matter annihilation, in which the clumpy and smooth elements of a halo ought to be accounted for independently. In this work, we evaluate two devoted NuSTAR observations with exposure of ~190 ks located ~10 ° from the Galactic plane, one above and the various other listed below, to look for x-ray lines from the radiative decay of sterile-neutrino dark matter. We locate no evidence of anomalous x-ray lines in the energy range 5- 20 keV, corresponding to sterilized neutrino masses 10- 40 keV. Statistical evidence has previously indicated that the stellar center GeV excess comes from mostly from point resources, and not from obliterating dark matter. In a proof-of-principle instance with simulated data, we discover that unmodeled resources in the Fermi bubbles can result in a dark matter signal being misattributed to direct sources by the NPTF. Dark matter halos have been formerly understood to be triaxial, yet in studies of possible annihilation and decay signals they are commonly treated as around round. We thoroughly check out the results of the baryons on the sphericity of annihilation and degeneration signals for both the instance where the onlooker is at 8.5 kpc from the center of the halo, and for a viewer situated well outside the halo. Germanium detectors with capability of gauging a single electron- hole set are required to look for light dark matter down to the MeV scale. Using the measured mass leak present and the Döhler- Brodsky model, we get the worths for fee obstacle elevation and the thickness of local energy states near the Fermi energy level for the bottom and top get in touches with, specifically.

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Arxiv — summary generated by Brevi Assistant

Extending the Standard Model with 3 right-handed neutrinos and a basic QCD axion sector can make up neutrino oscillations, dark matter and baryon asymmetry; at the very same time, it fixes the solid CP issue, stabilizes the electroweak vacuum and can implement critical Higgs inflation. Although crucial Higgs inflation includes an inflection point of the inflaton potential, we show that DM can not get a contribution from prehistoric black holes in the aν MSM. We provide two alternate evidence for the cancellation mechanism in the U symmetrical pseudo-Nambu-Goldstone-Boson Dark Matter model. Thus, the DM-quark scattering generated by a mass mixing between the radial mode and the Higgs boson disappears at the restriction of zero-momentum transfer. We assess 11 years of Fermi-LAT data representing the sky areas of 7 dwarf irregular galaxies. The shape distortion of the presumed Milky Way dark matter halo can affect the regional thickness of dark matter and therefore the straight detection program. The ellipticities that we fit to rotation contour information seem to be far more significant than those calculated in cosmological simulations of dark matter haloes. In this work, we provide a search for Dark Matter prospect particles generated at the Large Hadron Collider, the process of the production of DM fragments, together with a new hypothetical gauge boson represented by Z ^’ is controlled by a model called Mono-Z ^’. No evidence for the presence of dark matter candidates was found, and 95 self-confidence level limitations were established on the mass of the Z ^’ the mass of the dark matter candidate bit, and the cutoff range of the efficient field theory. We make use of idealized N-body simulations of stability stellar disks embedded within course-grained dark matter haloes to examine the effects of spurious collisional home heating on disk structure and kinematics. The integrated impacts of collisional heating are determined by the mass of dark matter halo bits, their local thickness and characteristic speed diffusion, but are mostly insensitive to the stellar particle mass.

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