Radio emission from dark matter annihilation in the Large Magellanic Cloud

被引：19

作者：

Siffert, Beatriz B. ^{[1
]}

Limone, Angelo ^{[1
]}

Borriello, Enrico ^{[1
,2
]}

Longo, Giuseppe ^{[1
,3
,4
]}

Miele, Gennaro ^{[1
,2
]}

机构：

[1] Univ Napoli Federico II, Dipartimento Sci Fis, I-80126 Naples, Italy

[2] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy

[3] INAF OACN, I-80128 Naples, Italy

[4] CALTECH, Dept Astron, Pasadena, CA 91125 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2011年 / 410卷 / 04期

关键词：

magnetic fields; galaxies: individual: Large Magellanic Cloud; dark matter; radio continuum: galaxies; EVOLUTION; ROTATION; CATALOG; FERMI; DUST; RAY;

D O I：

10.1111/j.1365-2966.2010.17613.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Large Magellanic Cloud (LMC), at only 50 kpc away from us and known to be dark matter dominated, is clearly an interesting place where to search for dark matter annihilation signals. In this paper, we estimate the synchrotron emission due to weakly interacting massive particle (WIMP) annihilation in the halo of the LMC at two radio frequencies, 1.4 and 4.8 GHz, and compare it to the observed emission, in order to impose constraints in the WIMP mass versus annihilation cross-section plane. We use available Faraday rotation data from background sources to estimate the magnitude of the magnetic field in different regions of the LMC's disc, where we calculate the radio signal due to dark matter annihilation. We account for the e(+)e(-) energy losses due to synchrotron, inverse Compton scattering and bremsstrahlung, using the observed hydrogen and dust temperature distribution on the LMC to estimate their efficiency. The extensive use of observations, allied with conservative choices adopted in all the steps of the calculation, allows us to obtain very realistic constraints.

引用

页码：2463 / 2471

页数：9

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