J/MNRAS/425/477 Dark matter annihilation in galaxy clusters (Nezri+, 2012)
γ-rays from annihilating dark matter in galaxy clusters:
stacking versus single source analysis.
Nezri E., White R., Combet C., Hinton J.A., Maurin D., Pointecouteau E.
<Mon. Not. R. Astron. Soc., 425, 477-489 (2012)>
=2012MNRAS.425..477N 2012MNRAS.425..477N
ADC_Keywords: Clusters, galaxy ; Gamma rays ; Models
Keywords: astroparticle physics - dark matter - gamma-rays: galaxies: clusters
Abstract:
Clusters of galaxies are potentially important targets for indirect
searches for dark matter (DM) annihilation. Here we reassess the
detection prospects for annihilation in massive haloes, based on a
statistical investigation of 1743 clusters in the new Meta-Catalogue
of X-ray Clusters (MCXC). We derive a new limit for the extragalactic
DM annihilation background of at least 20 per cent of that
originating from the Galaxy for an integration angle of 0.1°.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 91 1743 J-values for the 1743 MCXC catalogue objects
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See also:
J/A+A/534/A109 : MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name Cluster name (from MCXC)
20- 23 I4 --- MCXC Indice of the cluster row in MCXC catalog,
(recno of Piffaretti et al., 2011,
Cat. J/A+A/534/109 mcxc file)
25- 30 F6.2 deg GLON Galactic longitude in degree (from MCXC)
32- 37 F6.2 deg GLAT Galactic latitude in degree (from MCXC)
39- 46 E8.3 kpc d Distance (from MCXC)
48- 55 E8.3 deg alphas smooth halo dimension αs (1)
57- 64 E8.3 Msun2/kpc5 Jsm(0.1) Astrophysical annihilation term (for a
smooth halo) for αint=0.1° (1)
66- 73 E8.3 Msun2/kpc5 Jsub(0.1) Astrophysical annihilation term (for a
halo with substructures)
for αint=0.1° (1)
75- 82 E8.2 deg alpha.8 Angle α.8 containing 80% of
the total J
84- 91 E8.2 --- J80 Value of annihilation signal for
αint=α.8
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Note (1): Parameters listed:
* the J-factor corresponds to the integral of the squared dark matter
density ρ over the line of sight (l) and the solid angle ({Omega)}:
J=∫∫ρ2(l,Ω).dl.dΩ
* the integration angle αint is defined with
Ω=2π(1-cosαint)
* a smooth dark matter halo is defined with a density profile
ρ(r)=ρs.(r/rs)-1.(1+r/rs)-2
where rs is the scale radius of the cluster
* the smooth halo dimension is defined with αs=atan(rs/d)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 27-May-2013