Dark matter in astro- and particle physics: proceedings of by Hans-Volker Klapdor-Kleingrothaus, Richard Arnowitt

By Hans-Volker Klapdor-Kleingrothaus, Richard Arnowitt

The quest for darkish topic within the universe has tested itself as the most interesting and vital fields of astrophysics, particle physics and cosmology. The lectures and talks during this e-book emphasize the experimental and theoretical prestige and destiny views, stressing particularly the interaction among astro- and particle physics.

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7. In the region adjacent to it the stau cannot decay fast into a neutralino and tau, in which case a stau and neutralino can annihilate into a tau plus photon. This coannihilation reduces W. de Boer 3 -1 <σv> [cm s ] 10 10 10 3 -1 <σv> [cm s ] 10 10 10 10 10 3 -1 <σv> [cm s ] 10 10 -27 200 400 600 200 400 800 V] 600 800 1000 Ge m [ 1/2 [Ge 1000 V] m0 sigv_bb -24 -25 10 10 10 -26 10 -27 200 400 600 200 400 800 V] 600 800 1000 Ge m [ 1/2 [Ge 1000 V] m0 sigv_tau -27 10 10 10 -28 10 -29 -30 10 10 -26 3 -1 10 -25 <σv> [cm s ] 10 -24 3 -1 10 <σv> [cm s ] 3 -1 <σv> [cm s ] 22 200 400 600 200 400 800 V] 600 800 1000 Ge m [ 1/2 [Ge 1000 V] m0 sigmav 10 -27 -28 -29 -30 200 400 600 200 400 800 V] 600 800 1000 Ge m [ 1/2 [Ge 1000 V] m0 sigv_tt -27 -28 -29 -30 200 400 600 200 400 800 V] 600 800 1000 Ge m [ 1/2 [Ge 1000 V] m0 sigv_WW -24 -25 -26 -27 200 400 600 200 400 800 V] 600 800 1000 Ge m [ 1/2 [Ge 1000 V] m0 sigmav Fig.

613, 962 (2004); astro-ph/0406254 9. , Astrophysical Journal 481, 205 (1997) 10. W. de Boer, M. Herold, C. Sander, V. Zhukov, A. V. Gladyshev and D. I. Kazakov, astro-ph/0408272 11. W. de Boer, hep-ph/0408166 12. W. V. Moskalenko, Astrophys. J. 509, 212 (1998); astroph/9807150 13. V. W. Strong, Astrophys. Space Sci. 272 (2000) 247; astroph/9908032 14. T. Kamae, T. Abe and T. Koi, astro-ph/0410617 15. B. , Astrophys. J. 588 (2003) 824 [Erratum-ibid. 605 (2004) 575]; astro-ph/0301029 16. A. J. F.

Number counts can then be computed: N (> fx , z, 2∆z) = Ω = =Ω z+∆z ∂N (Lx > 4πDl2 fx )dz z−∆z ∂z z+∆z Ω z−∆z N (> T (z))dV (z) z+∆z +∞ N (M, z)dM dV (z) z−∆z M (z) (2) where T (z) is the temperature threshold corresponding to the flux fx as given by the observations, being therefore independent of the cosmological model. For most surveys the above formula has to be adapted to the fact that the area varies with the flux limit, and eventually with redshift. Several Cosmology with Distant XMM-Newton Clusters 41 ingredients are needed: the local abundance of clusters as given by the temperature distribution function (N (T )), the mass-temperature relation and its evolution, the mass function and the knowledge of the dispersion.

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