skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: Stringent neutrino flux constraints on antiquark nugget dark matter

Authors:
;
Publication Date:
Sponsoring Org.:
USDOE
OSTI Identifier:
1354759
Resource Type:
Journal Article: Publisher's Accepted Manuscript
Journal Name:
Physical Review D
Additional Journal Information:
Journal Volume: 95; Journal Issue: 10; Related Information: CHORUS Timestamp: 2017-05-01 22:11:57; Journal ID: ISSN 2470-0010
Publisher:
American Physical Society
Country of Publication:
United States
Language:
English

Citation Formats

Gorham, P. W., and Rotter, B. J. Stringent neutrino flux constraints on antiquark nugget dark matter. United States: N. p., 2017. Web. doi:10.1103/PhysRevD.95.103002.
Gorham, P. W., & Rotter, B. J. Stringent neutrino flux constraints on antiquark nugget dark matter. United States. doi:10.1103/PhysRevD.95.103002.
Gorham, P. W., and Rotter, B. J. 2017. "Stringent neutrino flux constraints on antiquark nugget dark matter". United States. doi:10.1103/PhysRevD.95.103002.
@article{osti_1354759,
title = {Stringent neutrino flux constraints on antiquark nugget dark matter},
author = {Gorham, P. W. and Rotter, B. J.},
abstractNote = {},
doi = {10.1103/PhysRevD.95.103002},
journal = {Physical Review D},
number = 10,
volume = 95,
place = {United States},
year = 2017,
month = 5
}

Journal Article:
Free Publicly Available Full Text
This content will become publicly available on May 1, 2018
Publisher's Accepted Manuscript

Save / Share:
  • The dark matter halo of the Milky Way is predicted to contain a very large number of smaller subhalos. As a result of the dark matter annihilations taking place within such objects, the most nearby and massive subhalos could appear as point-like or spatially extended gamma-ray sources, without observable counterparts at other wavelengths. In this paper, we use the results of the Aquarius simulation to predict the distribution of nearby subhalos, and compare this to the characteristics of the unidentified gamma-ray sources observed by the Fermi Gamma-Ray Space Telescope. Focusing on the brightest high latitude sources, we use this comparisonmore » to derive limits on the dark matter annihilation cross section. For dark matter particles lighter than ~200 GeV, the resulting limits are the strongest obtained to date, being modestly more stringent than those derived from observations of dwarf galaxies or the Galactic Center. We also derive independent limits based on the lack of unidentified gamma-ray sources with discernible spatial extension, but these limits are a factor of ~2-10 weaker than those based on point-like subhalos. Lastly, we note that four of the ten brightest high-latitude sources exhibit a similar spectral shape, consistent with 30-60 GeV dark matter particles annihilating to b quarks with an annihilation cross section on the order of sigma v ~ (5-10) x 10^-27 cm^3/s, or 8-10 GeV dark matter particles annihilating to taus with sigma v ~ (2.0-2.5) x 10^-27 cm^3/s.« less
  • For any realistic halo profile, the Galactic Center is predicted to be the brightest source of gamma-rays from dark matter annihilations. Due in large part to uncertainties associated with the dark matter distribution and astrophysical backgrounds, however, the most commonly applied constraints on the dark matter annihilation cross section have been derived from other regions, such as dwarf spheroidal galaxies. In this article, we study Fermi Gamma-Ray Space Telescope data from the direction of the inner Galaxy and derive stringent upper limits on the dark matter's annihilation cross section. Even for the very conservative case of a dark matter distributionmore » with a significant (~kpc) constant-density core, normalized to the minimum density needed to accommodate rotation curve and microlensing measurements, we find that the Galactic Center constraint is approximately as stringent as those derived from dwarf galaxies (which were derived under the assumption of an NFW distribution). For NFW or Einasto profiles (again, normalized to the minimum allowed density), the Galactic Center constraints are typically stronger than those from dwarfs.« less
  • Cited by 14
  • Warm dark matter might more easily account for small scale clustering measurements than the heavier particles typically invoked in {lambda} cold dark matter ({lambda}CDM) cosmologies. In this paper, we consider a {lambda}WDM cosmology in which sterile neutrinos {nu}{sub s}, with a mass m{sub s} of roughly 1-100 keV, are the dark matter. We use the diffuse x-ray spectrum (total minus resolved point source emission) of the Andromeda galaxy to constrain the rate of sterile neutrino radiative decay: {nu}{sub s}{yields}{nu}{sub e,{mu}}{sub ,{tau}}+{gamma}. Our findings demand that m{sub s}<3.5 keV (95% C.L.) which is a significant improvement over the previous (95% C.L.)more » limits inferred from the x-ray emission of nearby clusters, m{sub s}<8.2 keV (Virgo A) and m{sub s}<6.3 keV (Virgo A+Coma)« less
  • In the indirect detection of dark matter through its annihilation products, the signals depend on the square of the dark matter density, making precise knowledge of the distribution of dark matter in the Universe critical for robust predictions. Many studies have focused on regions where the dark matter density is greatest, e.g., the galactic center, as well as on the cosmic signal arising from all halos in the Universe. We focus on the signal arising from the whole Milky Way halo; this is less sensitive to uncertainties in the dark matter distribution, and especially for flatter profiles, this halo signalmore » is larger than the cosmic signal. We illustrate this by considering a dark matter model in which the principal annihilation products are neutrinos. Since neutrinos are the least detectable standard model particles, a limit on their flux conservatively bounds the dark matter total self-annihilation cross section from above. By using the Milky Way halo signal, we show that previous constraints using the cosmic signal can be improved on by 1-2 orders of magnitude; dedicated experimental analyses should be able to improve both by an additional 1-2 orders of magnitude.« less