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Characterization of Dark-Matter-induced anisotropies in the diffuse gamma-ray background

Fornasa, Mattia and Zavala, Jesús and Sánchez-Conde, Miguel A. and Siegal-Gaskins, Jennifer M. and Delahaye, Timur and Prada, Francisco and Vogelsberger, Mark and Zandanel, Fabio and Frenk, Carlos S. (2013) Characterization of Dark-Matter-induced anisotropies in the diffuse gamma-ray background. Monthly Notices of the Royal Astronomical Society, 429 (2). pp. 1529-1553. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20130117-105422426

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Abstract

The Fermi-LAT collaboration has recently reported the detection of angular power above the photon noise level in the diffuse gamma-ray background between 1 and 50 GeV. Such signal can be used to constrain a possible contribution from dark matter (DM) induced photons. We estimate the intensity and features of the angular power spectrum (APS) of this potential DM signal, for both decaying and annihilating DM candidates, by constructing template all-sky gamma-ray maps for the emission produced in the galactic halo and its substructures, as well as in extragalactic (sub)haloes. The DM distribution is given by state-of-the-art N-body simulations of cosmic structure formation, namely Millennium-II for extragalactic (sub)haloes, and Aquarius for the galactic halo and its subhaloes. We use a hybrid method of extrapolation to account for (sub)structures that are below the resolution limit of the simulations, allowing us to estimate the total emission all the way down to the minimal self-bound halo mass. We describe in detail the features appearing in the APS of our template maps and we estimate the effect of various uncertainties such as the value of the minimal halo mass, the fraction of substructures hosted in a halo and the shape of the DM density profile. Our results indicate that the fluctuation APS of the DM-induced emission is of the same order as the Fermi-LAT APS, suggesting that one can constrain this hypothetical emission from the comparison with the measured anisotropy. We also quantify the uncertainties affecting our results, finding ‘theoretical error bands’ spanning more than two orders of magnitude and dominated (for a given particle physics model) by our lack of knowledge of the abundance of low-mass (sub)haloes.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1207.0502v1arXivUNSPECIFIED
http://dx.doi.org/10.1093/mnras/sts444 DOIUNSPECIFIED
http://mnras.oxfordjournals.org/content/429/2/1529PublisherUNSPECIFIED
ORCID:
AuthorORCID
Zavala, Jesús0000-0002-7051-1100
Vogelsberger, Mark0000-0001-8593-7692
Additional Information:© 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2012 November 18. Received 2012 October 25; in original form 2012 July 27. First published online: December 22, 2012. We thank Alberto Dominguez for providing us with tables for the EBL attenuation factor and the referee, M. Kuhlen, for a thorough and constructive report. JZ thanks Niayesh Afshordi for fruitful discussions. We thank Alessandro Cuoco and Anne Green for useful comments and discussions. We also thank Chris Hirata and the support of the Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064. JZ is supported by the University of Waterloo and the Perimeter Institute for Theoretical Physics. Research at Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research & Innovation. The work of MASC is supported through the NASA grant NNH09ZDA001N for study of the Extragalactic Gamma-ray Background. JZ acknowledges financial support by a CITA National Fellowship. JSG acknowledges support from NASA through Einstein Postdoctoral Fellowship grant PF1-120089 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. TD was supported by the Spanish MICINNs Consolider-Ingenio 2010 Programme under grant CPAN CSD2007-00042. We also thank the support of the MICINN under grant FPA2009-08958, the Community of Madrid under grant HEPHACOSS2009/ESP-1473, and the European Union under the Marie Curie-ITN program PITN-GA-2009-237920. The calculations for this paper were performed on the ICC Cosmology Machine, which is part of the DiRAC Facility jointly funded by STFC, the Large Facilities Capital Fund of BIS, and Durham University, and the clusters at the Max-Planck Institute for Astrophysics. We acknowledge use of the facilities of the Shared Hierarchical Academic Research Computing Network (SHARCNET:www.sharcnet.ca)aCompute/Calcul Canada.
Group:TAPIR
Funders:
Funding AgencyGrant Number
Consolider-Ingenio 2010 ProgrammeCSD2009-00064
University of WaterlooUNSPECIFIED
Perimeter Institute for Theoretical PhysicsUNSPECIFIED
Government of Canada Industry CanadaUNSPECIFIED
Province of Ontario Ministry of Research & InnovationUNSPECIFIED
NASANNH09ZDA001N
CITA National FellowshipUNSPECIFIED
NASA Einstein Postdoctoral Fellowship GrantPF1-120089
NASANAS8-03060
Spanish MICINN Consolider-Ingenio 2010 ProgrammeCPAN CSD2007-00042
Spanish MICINNFPA2009-08958
Community of MadridHEPHACOSS2009/ ESP-1473
European Union Marie Curie-ITN programPITN-GA-2009-237920
STFCUNSPECIFIED
BIS Large Facilities Capital FundUNSPECIFIED
Durham-UniversityUNSPECIFIED
Max Planck Institute for Astrophysics clustersUNSPECIFIED
Subject Keywords:astroparticle physics – methods: numerical – cosmology: dark matter – gamma-rays: diffuse background
Issue or Number:2
Record Number:CaltechAUTHORS:20130117-105422426
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130117-105422426
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:36454
Collection:CaltechAUTHORS
Deposited By: JoAnn Boyd
Deposited On:12 Feb 2013 16:57
Last Modified:09 Mar 2020 13:19

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