A "Baedecker" for the Dark Matter Annihilation Signal
We provide a ``Baedecker'' or travel guide to the directions on the sky where the dark matter annihilation signal may be expected. We calculate the flux of high energy gamma-rays from annihilation of neutralino dark matter in the centre of the Milky Way and the three nearest dwarf spheroid...
| Main Authors: | , , |
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| Format: | Journal article |
| Language: | English |
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2003
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| _version_ | 1797078980534206464 |
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| author | Evans, N Ferrer, F Sarkar, S |
| author_facet | Evans, N Ferrer, F Sarkar, S |
| author_sort | Evans, N |
| collection | OXFORD |
| description | We provide a ``Baedecker'' or travel guide to the directions on the sky where the dark matter annihilation signal may be expected. We calculate the flux of high energy gamma-rays from annihilation of neutralino dark matter in the centre of the Milky Way and the three nearest dwarf spheroidals (Sagittarius, Draco and Canis Major), using realistic models of the dark matter distribution. Other investigators have used cusped dark halo profiles (such as the Navarro-Frenk-White) to claim a significant signal. This ignores the substantial astrophysical evidence that the Milky Way is not dark-matter dominated in the inner regions. We show that the annihilation signal from the Galactic Centre falls by two orders of magnitude on substituting a cored dark matter density profile for a cusped one. The present and future generation of high energy gamma-ray detectors, whether atmospheric Cerenkov telescopes or space missions like GLAST, lack the sensitivity to detect any of the monochromatic gamma-ray annihilation lines. The continuum gamma-ray signal above 1 GeV and above 50 GeV may however be detectable either from the dwarf spheroidals or from the Milky Way itself. If the density profiles of the dwarf spheroidals are cusped, then the best prospects are for detecting Sagittarius and Canis Major. However, if the dwarf spheroidals have milder, cored profiles, then the annihilation signal is not detectable. For GLAST, an attractive strategy is to exploit the wide field of view and observe the Milky Way at medium latitudes, as suggested by Stoehr et al. This is reasonably robust against changes in the density profile. |
| first_indexed | 2024-03-07T00:39:07Z |
| format | Journal article |
| id | oxford-uuid:826e92e5-f58e-4611-84f2-e27202504a34 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T00:39:07Z |
| publishDate | 2003 |
| record_format | dspace |
| spelling | oxford-uuid:826e92e5-f58e-4611-84f2-e27202504a342022-03-26T21:37:21ZA "Baedecker" for the Dark Matter Annihilation SignalJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:826e92e5-f58e-4611-84f2-e27202504a34EnglishSymplectic Elements at Oxford2003Evans, NFerrer, FSarkar, SWe provide a ``Baedecker'' or travel guide to the directions on the sky where the dark matter annihilation signal may be expected. We calculate the flux of high energy gamma-rays from annihilation of neutralino dark matter in the centre of the Milky Way and the three nearest dwarf spheroidals (Sagittarius, Draco and Canis Major), using realistic models of the dark matter distribution. Other investigators have used cusped dark halo profiles (such as the Navarro-Frenk-White) to claim a significant signal. This ignores the substantial astrophysical evidence that the Milky Way is not dark-matter dominated in the inner regions. We show that the annihilation signal from the Galactic Centre falls by two orders of magnitude on substituting a cored dark matter density profile for a cusped one. The present and future generation of high energy gamma-ray detectors, whether atmospheric Cerenkov telescopes or space missions like GLAST, lack the sensitivity to detect any of the monochromatic gamma-ray annihilation lines. The continuum gamma-ray signal above 1 GeV and above 50 GeV may however be detectable either from the dwarf spheroidals or from the Milky Way itself. If the density profiles of the dwarf spheroidals are cusped, then the best prospects are for detecting Sagittarius and Canis Major. However, if the dwarf spheroidals have milder, cored profiles, then the annihilation signal is not detectable. For GLAST, an attractive strategy is to exploit the wide field of view and observe the Milky Way at medium latitudes, as suggested by Stoehr et al. This is reasonably robust against changes in the density profile. |
| spellingShingle | Evans, N Ferrer, F Sarkar, S A "Baedecker" for the Dark Matter Annihilation Signal |
| title | A "Baedecker" for the Dark Matter Annihilation Signal |
| title_full | A "Baedecker" for the Dark Matter Annihilation Signal |
| title_fullStr | A "Baedecker" for the Dark Matter Annihilation Signal |
| title_full_unstemmed | A "Baedecker" for the Dark Matter Annihilation Signal |
| title_short | A "Baedecker" for the Dark Matter Annihilation Signal |
| title_sort | baedecker for the dark matter annihilation signal |
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