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Testing dark matter warmness and quantity via the reduced relativistic gas model

Julio C. Fabris1, Ilya L. Shapiro2, and A. M. Velasquez-Toribio1

  • 1Departamento de Física—CCE, Universidade Federal do Espírito Santo Vitória, CEP: 29060-900, ES, Brazil
  • 2Departamento de Física—ICE, Universidade Federal de Juiz de Fora, CEP: 36036-330, MG, Brazil

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Phys. Rev. D 85, 023506 – Published 6 January, 2012

DOI: https://doi.org/10.1103/PhysRevD.85.023506

Abstract

We use the framework of a recently proposed model of reduced relativistic gas to obtain the bounds for Ω’s of dark matter and dark energy (in the present case, a cosmological constant), taking into consideration an arbitrary warmness of dark matter. An equivalent equation of state has been used by Sakharov to predict the oscillations in the matter power spectrum. Two kinds of tests are accounted for in what follows, namely, the ones coming from the dynamics of the conformal factor of the homogeneous and isotropic metric and also the ones based on linear cosmic perturbations. The reduced relativistic gas model demonstrated its high effectiveness, permitting to explore a large volume in the space of mentioned parameters in a rather economic way. Taking together the results of such tests as supernova type Ia (Union2 sample), H(z), cosmic microwave background (R factor), baryon acoustic oscillation, and large-scale structure data (2dFGRS data), we confirm that ΛCDM is the most favored model. At the same time, for the 2dFGRS data alone we found that an alternative model with a very small quantity of dark matter is also viable. This output is potentially relevant in view of the fact that the large-scale structure data is the only test which cannot be affected by the possible quantum contributions to the low-energy gravitational action.

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References (42)

  1. A. G. Riess et al., Astron. J. 116, 1009 (1998); 699, 539 (2009); S. Perlmutter, Astrophys. J. 517, 565 (1999).
  2. S. Hannestad, Int. J. Mod. Phys. A 21, 1938 (2006).
  3. S. Weinberg, Rev. Mod. Phys. 61, 1 (1989).
  4. I. L. Shapiro and J. Solà, J. High Energy Phys. 02 (2002) 006.
  5. E. Kolb and M. Turner, The Very Early Universe (Addison-Wesley, Reading, MA, 1994); J. Binney and S. Tremaine, Galactic Dynamics (Princeton University, Princeton, NJ, 1988).
  6. S. Dodelson, Modern Cosmology (Academic, New York, 2003).
  7. J. A. Tyson, G. P. Kochanski, and I. P. Dell’Antonio, Astrophys. J. 498, L107 (1998).
  8. A. Pinzke, C. Pfrommer, and L. Bergstrom, Phys. Rev. D 84, 123509 (2011).
  9. J. L. Tinker, Astrophys. J. 688, 709 (2008).
  10. I. A. Yegorova, A. Pizzella, and P. Salucci, arXiv:1106.5105 [Astron. Astrophys. (to be published)].
  11. S. Dodelson and L. M. Widrow, Phys. Rev. Lett. 72, 17 (1994).
  12. S. Colombi, S. Dodelson, and L. M. Widrow, Astrophys. J. 458, 1 (1996).
  13. G. de Berredo-Peixoto, I. L. Shapiro, and F. Sobreira, Mod. Phys. Lett. A 20, 2723 (2005).
  14. J. C. Fabris, I. L. Shapiro, and F. Sobreira, J. Cosmol. Astropart. Phys. 02 (2009) 001.
  15. L. P. Grishchuk, arXiv:1106.5205.
  16. A. D. Sakharov, Zh. Eksp. Teor. Fiz. 49, 345 (1965) [Sov. Phys. JETP 22, 241 (1966)].
  17. J. R. Bond and A. S. Szalay, Astrophys. J. 274, 443 (1983).
  18. Z. Haiman, R. Barkana, and J. P. Ostriker, arXiv:astro-ph/0103050.
  19. P. Bode, J. P. Ostriker, and N. Turok, Astrophys. J. 556, 93 (2001).
  20. R. Barkana, Z. Haiman, and J. P. Ostriker, arXiv:astro-ph/0102304.
  21. I. L. Shapiro, J. Solà, and H. Štefančić, J. Cosmol. Astropart. Phys. 01 (2005) 012.
  22. J. Grande, J. Solà, J. C. Fabris, and I. L. Shapiro, Classical Quantum Gravity 27, 105004 (2010).
  23. C. Farina, W. J. M. Kort-Kamp, S. Mauro, and I. L. Shapiro, Phys. Rev. D 83, 124037 (2011).
  24. D. C. Rodrigues, P. S. Letelier, and I. L. Shapiro, J. Cosmol. Astropart. Phys. 04 (2010) 020;
  25. J. C. Fabris, I. L. Shapiro, and J. Solà, J. Cosmol. Astropart. Phys. 02 (2007) 016.
  26. J. M. Bardeen, J. R. Bond, N. Kaiser, and A. S. Szalay, Astrophys. J. 304, 15 (1986).
  27. P. Bode, J. P. Ostriker, and N. Turok, Astrophys. J. 556, 93 (2001).
  28. M. Viel, J. Lesgourgues, M. G. Haehnelt, S. Matarrese, and A. Riotto, Phys. Rev. D 71, 063534 (2005); Phys. Rev. Lett. 97, 071301 (2006).
  29. E. Komatsu et al., Astrophys. J. Suppl. Ser. 192, 18 (2011).
  30. S. Nesseris and L. Perivolaropoulos, J. Cosmol. Astropart. Phys. 01 (2007) 018.
  31. D. L. Eisenstein et al. (SDSS Collaboration) Astrophys. J. 633, 560 (2005).
  32. R. Jimenez, L. Verde, T. Treu, and D. Stern, Astrophys. J. 593, 622 (2003).
  33. J. Simon, L. Verde, and R. Jimenez, Phys. Rev. D 71, 123001 (2005).
  34. D. Stern, R. Jimenez, L. Verde, M. Kamionkowski, and S. A. Stanford, J. Cosmol. Astropart. Phys. 2 (2010) 008.
  35. E. Gaztanaga, A. Cabre, and L. Hui, Mon. Not. R. Astron. Soc. 399, 1663 (2009).
  36. R. Amanullah et al., Astrophys. J. 716, 712 (2010).
  37. R. Kessler et al., Astrophys. J. 185, 32 (2009).
  38. M. Kowalski et al., Astrophys. J. 686, 749 (2008).
  39. S. Cole et al., Mon. Not. R. Astron. Soc. 362, 505 (2005); Astrophys. J. 549, 669 (2001); W. J. Percival et al. (2dFGRS Team Collaboration), Mon. Not. R. Astron. Soc. 337, 1068 (2002).
  40. H. J. de Vega and N. G. Sanchez, Int. J. Mod. Phys. A 26, 1057 (2011); H. J. de Vega, P. Salucci, and N. G. Sanchez, arXiv:1004.1908.
  41. R. K. de Naray and T. Kaufmann, Mon. Not. R. Astron. Soc. 414, 3617 (2011); A. Del Popolo, 408, 1808 (2010); F. Donato et al., 397, 1169 (2009); G. Ogiya and M. Mori, arXiv:1106.2864 [Astrophys. J. Lett. (to be published)].
  42. V. R. Eke, J. F. Navarro, and M. Steinmetz, Astrophys. J. 554, 114 (2001).

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Phys. Rev. D 85, 023506– Published 6 January, 2012
  • Received 17 May 2011

© 2012 American Physical Society

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