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Title: Directly Detecting MeV-Scale Dark Matter Via Solar Reflection

Abstract

If dark matter (DM) particles are lighter than a few MeV/c 2 and can scatter off electrons, their interaction within the solar interior results in a considerable hardening of the spectrum of galactic dark matter received on Earth. For a large range of the mass versus cross section parameter space, {m ee}, the “reflected” component of the DM flux is far more energetic than the end point of the ambient galactic DM energy distribution, making it detectable with existing DM detectors sensitive to an energy deposition of 10–10 3 eV. Furthermore after numerically simulating the small reflected component of the DM flux, we calculate its subsequent signal due to scattering on detector electrons, deriving new constraints on σ e in the MeV and sub-MeV range using existing data from the XENON10/100, LUX, PandaX-II, and XENON1T experiments, as well as making projections for future low threshold direct detection experiments

Authors:
; ; ;
Publication Date:
Research Org.:
California Institute of Technology (CalTech), Pasadena, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1431401
Alternate Identifier(s):
OSTI ID: 1502079
Grant/Contract Number:  
SC0011632
Resource Type:
Published Article
Journal Name:
Physical Review Letters
Additional Journal Information:
Journal Name: Physical Review Letters Journal Volume: 120 Journal Issue: 14; Journal ID: ISSN 0031-9007
Publisher:
American Physical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS

Citation Formats

An, Haipeng, Pospelov, Maxim, Pradler, Josef, and Ritz, Adam. Directly Detecting MeV-Scale Dark Matter Via Solar Reflection. United States: N. p., 2018. Web. doi:10.1103/PhysRevLett.120.141801.
An, Haipeng, Pospelov, Maxim, Pradler, Josef, & Ritz, Adam. Directly Detecting MeV-Scale Dark Matter Via Solar Reflection. United States. doi:10.1103/PhysRevLett.120.141801.
An, Haipeng, Pospelov, Maxim, Pradler, Josef, and Ritz, Adam. Wed . "Directly Detecting MeV-Scale Dark Matter Via Solar Reflection". United States. doi:10.1103/PhysRevLett.120.141801.
@article{osti_1431401,
title = {Directly Detecting MeV-Scale Dark Matter Via Solar Reflection},
author = {An, Haipeng and Pospelov, Maxim and Pradler, Josef and Ritz, Adam},
abstractNote = {If dark matter (DM) particles are lighter than a few MeV/c2 and can scatter off electrons, their interaction within the solar interior results in a considerable hardening of the spectrum of galactic dark matter received on Earth. For a large range of the mass versus cross section parameter space, {me,σe}, the “reflected” component of the DM flux is far more energetic than the end point of the ambient galactic DM energy distribution, making it detectable with existing DM detectors sensitive to an energy deposition of 10–103 eV. Furthermore after numerically simulating the small reflected component of the DM flux, we calculate its subsequent signal due to scattering on detector electrons, deriving new constraints on σe in the MeV and sub-MeV range using existing data from the XENON10/100, LUX, PandaX-II, and XENON1T experiments, as well as making projections for future low threshold direct detection experiments},
doi = {10.1103/PhysRevLett.120.141801},
journal = {Physical Review Letters},
number = 14,
volume = 120,
place = {United States},
year = {2018},
month = {4}
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record
DOI: 10.1103/PhysRevLett.120.141801

Citation Metrics:
Cited by: 7 works
Citation information provided by
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Figures / Tables:

FIG. 1. FIG. 1. : A schematic illustration of the reflected dark matter flux generated through solar scattering. For bound solar electrons with energy EekT, the DM recoil energy is bounded by the expression in Eq. (1) and can be ∼keV.

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    Figures/Tables have been extracted from DOE-funded journal article accepted manuscripts.