Detectability of neutralino clumps via atmospheric Cherenkov telescopes

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 66, Issue 8, 2002, Pages

  Tasitsiomi, Argyro ^a   Olinto, Angela V ^a  

^a UNIVERSITY OF CHICAGO   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ANALYTICAL EQUIPMENT; ARTICLE; ASTRONOMY; DENSITY; ELEMENTARY PARTICLE; GAMMA RADIATION; MASS; SPACE; TELECOMMUNICATION; TELESCOPE;

EID: 0041697316     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.66.083006     Document Type: Article

References (58)

1. G. Jungman, M. Kamionkowski, and K. Griest, Phys. Rep. 267, 195 (1996).
2. J. Ellis, T. Falk, G. Ganis, and K.A. Olive, Phys. Rev. D 62, 075010 (2000).
3. V. Berezinsky, A.V. Gurevich, and K.P. Zybin, Phys. Lett. B 294, 221 (1992).
4. V. Berezinsky, A. Bottino, and G. Mignola, Phys. Lett. B 325, 136 (1994).
5. P. Gondolo and J. Silk, Phys. Rev. Lett. 83, 1719 (1999).
6. P. Gondolo, Phys. Lett. B 494, 181 (2000).
7. G. Bertone, G. Sigl, and J. Silk, Mon. Not. R. Astron. Soc. 326, 799 (2001).
8. L. Bergström, J. Edsjö, P. Gondolo, and P. Ullio, Phys. Rev. D 59, 043506 (1999).
9. C. Calcáneo-Roldán and B. Moore, Phys. Rev. D 62, 123005 (2000).
10. R. Aloisio, P. Blasi, and A.V. Olinto, astro-ph/0206036.
11. P. Blasi, A.V. Olinto, and C. Tyler, astro-ph/0202049.
12. C. Tyler, Phys. Rev. D 66, 023504 (2002).
13. D. Merritt and M. Milosavljevic, in “DARK 2002: 4th International Heidelberg Conference on Dark Matter in Astro and Particle Physics, Cape Town, South Africa, 2002,” edited by H. V. Klapdor-Kleingrothaus and R. Viollier, astro-ph/0205140.
14. S. Ghigna, B. Moore, F. Governato, G. Lake, T. Quinn, and J. Stadel, Mon. Not. R. Astron. Soc. 300, 146 (1998).
15. B. Moore, S. Ghigna, F. Governato, G. Lake, T. Quinn, J. Stadel, and P. Tozzi, Astrophys. J. Lett. 524, L19 (1999).
16. A. Klypin, A.V. Kravtsov, O. Valenzuela, and F. Prada, Astrophys. J. 522, 82 (1999).
17. A. Tasitsiomi, astro-ph/0205464.
18. V.V. Vassiliev et al., 26th International Cosmic Ray Conference, Salt Lake City, 1999, Vol. 5, p. 299, http://veritas.sao.arizona.edu
19. W. Hofmann, GeV-TeV Gamma Ray Astrophysics Workshop: Towards a Major Atmospheric Cherenkov Detector VI, edited by Brenda L. Dingus, Michael H. Salamon, and David B. Kieda, AIP Conf. Proc. No.515 (AIP, Melville, NY, 2000), p. 492.
20. M. Martinez, Ref. 18, p. 219.
21. M. Mori, et al., Ref. 19, p. 485.
22. A.S. Font, J.F. Navarro, J. Stadel, and T. Quinn, Astrophys. J. Lett. 563, L1 (2001).
23. I.R. Walker, J.C. Mihos, and L. Hernquist, Astrophys. J. 460, 121 (1996).
24. H. Velazquez and S.D.M. White, Mon. Not. R. Astron. Soc. 304, 254 (1999).
25. P. Blasi and R.K. Sheth, Phys. Lett. B 486, 233 (2000).
26. G. Lake, Nature (London) 346, 39 (1990).
27. L. Bergström, J. Edsjö, P. Gondolo, and P. Ullio, Phys. Rev. D 59, 043506 (1999).
28. J.F. Navarro, C.S. Frenk, and S.D.M. White, Astrophys. J. 462, 563 (1996).
29. A. Klypin, A.V. Kravtsov, J. Bullock, and J.R. Primack, Astrophys. J. 554, 903 (2001).
30. J.E. Taylor and J.F. Navarro, Astrophys. J. 563, 483 (2001).
31. J.F. Navarro, astro-ph/0110680.
32. J. Binney and S. Tremaine, Galactic Dynamics (Princeton University Press, Princeton, NJ, 1998), p. 452.
33. Similar is the conclusion with respect to the mass, (Formula presented) that appears in Eq. (8). Namely, for the distances from the galactic center that are relevant here, both profiles yield similar results.
34. More generally, for an (Formula presented) behavior of the density profile at the center, the contribution of the core to the flux scales as (Formula presented) which implies a sensitive dependence on (Formula presented) for (Formula presented) assuming of course that (Formula presented) Note, however, that the behavior of the density profile at intermediate distances (Formula presented) might also be important in some cases in determining the overall dependence of the flux on (Formula presented)
35. E.A. Baltz, C. Briot, P. Salati, R. Taillet, and J. Silk, Phys. Rev. D 61, 023514 (1999).
36. L. Bergström, J. Edsjö, and C. Gunnarsson, Phys. Rev. D 63, 083515 (2001).
37. J. Edsjö and P. Gondolo, Phys. Rev. D 56, 1879 (1997).
38. DARKSUSY, http://www.physto.se/∼edsjo/dark susy; P. Gondolo, J. Edsjö, L. Bergström, P. Ullio, and E. A. Baltz (in preparation).
39. L. Bergström and P. Gondolo, Astropart. Phys. 5, 263 (1996).
40. L. Bergström and P. Ullio, Nucl. Phys. B504, 27 (1997).
41. P. Ullio and L. Bergström, Phys. Rev. D 57, 1962 (1998).
42. M. Drees, M.M. Nojiri, D.P. Roy, and Y. Yamada, Phys. Rev. D 56, 276 (1997).
43. S. Heinemeyer, W. Hollik, and G. Weiglein, Phys. Lett. B 455, 179 (1999);http://www-itp.physik.uni-karlsruhe.de/feynhiggs/
44. P. Gondolo and G. Gelmini, Nucl. Phys. B360, 145 (1991).
45. J.A. Peacock, Cosmological Physics, (Cambridge University Press, Cambridge, England, 1999), Sec. 3.2.
46. A.G. Reiss et al., Astrophys. J. 116, 1009 (1998).
47. S. Perlmutter et al., Astrophys. J. 517, 565 (1999).
48. C.T. Hill, Nucl. Phys. B224, 469 (1983).
49. C.T. Hill, D.N. Schramm, and T.P. Walker, Phys. Rev. D 36, 1007 (1987).
50. For simplicity, from that point on we will use the term cross section to denote the thermally averaged product of the cross section times the relative velocity.
51. In fact, the low (good) VERITAS resolution—which renders the nearest clumps resolved—has been a crucial factor in determining our strategy, namely, the use of individual clumps rather than of all-sky maps that might be more appropriate in the case of numerous, unresolved clumps, as most clumps would appear when observed via instruments of higher (worse) angular resolution, e.g., GLAST.
52. L. Bergström, P. Ullio, and J.H. Buckley, Astropart. Phys. 9, 137 (1998).
53. M.S. Longair, High Energy Astrophysics (Cambridge University Press, Cambridge, England, 1992).
54. P. Sreekumar et al., Astrophys. J. 494, 523 (1998).
55. S.D. Hunter et al., Astrophys. J. 481, 205 (1997).
56. L. Bergström, J. Edsjö, and C. Gunnarsson, Phys. Rev. D 63, 083515 (2001).
57. N. Gehrels and P. Michelson, Astropart. Phys. 11, 277 (1999).
58. Other weaker dependencies exist as, for example, via Eqs. (7) and (21).