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The isotropic radio background and annihilating dark matter

Dan Hooper1,2, Alexander V. Belikov3, Tesla E. Jeltema4, Tim Linden4, Stefano Profumo4, and Tracy R. Slatyer5

  • 1Center for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA
  • 2Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637, USA
  • 3Institut d’Astrophysique de Paris, Unité Mixte de Recherche 7095, CNRS, Université Pierre et Marie Curie, Paris 06, 98 bis boulevard Arago, 75014 Paris, France
  • 4Department of Physics and Santa Cruz Institute for Particle Physics, University of California, 1156 High Street, Santa Cruz, California 95064, USA
  • 5School of Natural Sciences, Institute for Advanced Study, Princeton, New Jersey 08540, USA

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Phys. Rev. D 86, 103003 – Published 5 November, 2012

DOI: https://doi.org/10.1103/PhysRevD.86.103003

Abstract

Observations by the Absolute Radiometer for Cosmology, Astrophysics and Diffuse Emission (ARCADE-2) and other telescopes sensitive to low frequency radiation have revealed the presence of an isotropic radio background with a hard spectral index. The intensity of this observed background is found to exceed the flux predicted from astrophysical sources by a factor of approximately 5–6. In this article, we consider the possibility that annihilating dark matter particles provide the primary contribution to the observed isotropic radio background through the emission of synchrotron radiation from electron and positron annihilation products. For reasonable estimates of the magnetic fields present in clusters and galaxies, we find that dark matter could potentially account for the observed radio excess, but only if it annihilates mostly to electrons and/or muons, and only if it possesses a mass in the range of approximately 5–50 GeV. For such models, the annihilation cross section required to normalize the synchrotron signal to the observed excess is σv≈(0.4–30)×10−26  cm3/s, similar to the value predicted for a simple thermal relic (σv≈3×10−26  cm3/s). We find that in any scenario in which dark matter annihilations are responsible for the observed excess radio emission, a significant fraction of the isotropic gamma-ray background observed by Fermi must result from dark matter as well.

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References (44)

  1. D. J. Fixsen, A. Kogut, S. Levin, M. Limon, P. Lubin, P. Mirel, M. Seiffert, J. Singal et al., arXiv:0901.0555.
  2. M. Seiffert, D. J. Fixsen, A. Kogut, S. M. Levin, M. Limon, P. M. Lubin, P. Mirel, J. Singal et al., arXiv:0901.0559.
  3. R. S. Roger, C. H. Costain, T. L. Landecker, and C. M. Swerdlyk, Astron. Astrophys. Suppl. Ser. 137, 7 (1999).
  4. A. E. Guzman, J. May, H. Alvarez, and K. Maeda, Astron. Astrophys. 525, A138 (2011).
  5. C. G. T. Haslam et al., Astron. Astrophys. 100, 209 (1981).
  6. P. Reich and W. Reich, Astron. Astrophys. Suppl. Ser. 63, 205 (1986).
  7. A. Kogut, D. J. Fixsen, S. M. Levin, M. Limon, P. M. Lubin, P. Mirel, M. Seiffert, J. Singal et al., Astrophys. J. 734, 4 (2011).
  8. J. Singal, L. Stawarz, A. Lawrence, and V. Petrosian, Mon. Not. R. Astron. Soc. 409, 1172 (2010).
  9. T. Vernstrom, D. Scott, and J. Wall, arXiv:1102.0814.
  10. M. Gervasi, A. Tartari, M. Zannoni, G. Boella, and G. Sironi, arXiv:0803.4138.
  11. P. P. Ponente, Y. Ascasibar, and J. M. Diego, Mon. Not. R. Astron. Soc. 418, 691 (2011).
  12. B. C. Lacki, Astrophys. J. 729, L1 (2011).
  13. N. Fornengo, R. Lineros, M. Regis, and M. Taoso, Phys. Rev. Lett. 107, 271302 (2011).
  14. N. Fornengo, R. Lineros, M. Regis, and M. Taoso, J. Cosmol. Astropart. Phys. 03 (2012) 033; M. Regis, Proc. Sci. EPS-HEP2011 (2011) 062.
  15. D. P. Finkbeiner, arXiv:0409027; D. Hooper, D. P. Finkbeiner, and G. Dobler, Phys. Rev. D 76, 083012 (2007); T. Linden, S. Profumo, and B. Anderson, 82, 063529 (2010); N. Fornengo, R. A. Lineros, M. Regis, and M. Taoso, J. Cosmol. Astropart. Phys. 01 (2012) 005.
  16. M. Regis and P. Ullio, Phys. Rev. D 78, 043505 (2008); R. Aloisio, P. Blasi, and A. V. Olinto, J. Cosmol. Astropart. Phys. 05 (2004) 007; C. Boehm, J. Silk, and T. Ensslin, arXiv:1008.5175.
  17. T. Linden, D. Hooper, and F. Yusef-Zadeh, Astrophys. J. 741, 95 (2011).
  18. S. Colafrancesco, S. Profumo, and P. Ullio, Astron. Astrophys. 455, 21 (2006).
  19. E. A. Baltz and L. Wai, Phys. Rev. D 70, 023512 (2004); P. Blasi, A. V. Olinto, and C. Tyler, Astropart. Phys. 18, 649 (2003); B. B. Siffert, A. Limone, E. Borriello, G. Longo, and G. Miele, Mon. Not. R. Astron. Soc. 410, 2463 (2011).
  20. S. Profumo and T. E. Jeltema, J. Cosmol. Astropart. Phys. 07 (2009) 020.
  21. A. V. Belikov and D. Hooper, Phys. Rev. D 81, 043505 (2010).
  22. J. F. Navarro, C. S. Frenk, and S. D. M. White, Astrophys. J. 462, 563 (1996); 490, 493 (1997).
  23. O. Y. Gnedin, D. Ceverino, N. Y. Gnedin, A. A. Klypin, A. V. Kravtsov, R. Levine, D. Nagai, and G. Yepes, arXiv:1108.5736.
  24. K.-H. Chae, A. V. Kravtsov, J. A. Frieman, and M. Bernardi, arXiv:1202.2716.
  25. J. S. Bullock, T. S. Kolatt, Y. Sigad, R. S. Somerville, A. V. Kravtsov, A. A. Klypin, J. R. Primack, and A. Dekel, Mon. Not. R. Astron. Soc. 321, 559 (2001).
  26. J. C. Munoz-Cuartas, A. V. Maccio, S. Gottlober, and A. A. Dutton, arXiv:1007.0438.
  27. J. S. Bullock, T. S. Kolatt, Y. Sigad, R. S. Somerville, A. V. Kravtsov, A. A. Klypin, J. R. Primack, and A. Dekel, Mon. Not. R. Astron. Soc. 321, 559 (2001).
  28. M. Kamionkowski, S. M. Koushiappas, and M. Kuhlen, Phys. Rev. D 81, 043532 (2010).
  29. J. Diemand, M. Kuhlen, P. Madau, M. Zemp, B. Moore, D. Potter, and J. Stadel, Nature (London) 454, 735 (2008); J. Diemand, M. Zemp, B. Moore, J. Stadel, M. Carolloand , Mon. Not. R. Astron. Soc. 364, 665 (2005).
  30. L. Gao, C. S. Frenk, A. Jenkins, V. Springel, and S. D. M. White, Mon. Not. R. Astron. Soc. 419, 1721 (2012); L. Gao, J. F. Navarro, C. S. Frenk, A. Jenkins, V. Springel, and S. D. M. White, 425, 2169 (2012).
  31. J. F. Navarro, E. Hayashi, C. Power, A. R. Jenkins, C. S. Frenk, S. D. M. White, V. Springel, J. Stadel, T. R. Quinnand , Mon. Not. R. Astron. Soc. 349, 1039 (2004); V. Springel, J. Wang, M. Vogelsberger, A. Ludlow, A. Jenkins, A. Helmi, J. F. Navarro, C. S. Frenk, and S. D. M. White, 391, 1685 (2008).
  32. K. Dolag, S. Schindler, F. Govoni, and L. Feretti, Astron. Astrophys. 378, 777 (2001); F. Govoni and L. Feretti, Int. J. Mod. Phys. D 13, 1549 (2004); J. Donnert, K. Dolag, H. Lesch, and E. Muller, Mon. Not. R. Astron. Soc. 392, 1008 (2009); A. Bonafede, L. Feretti, M. Murgia, F. Govoni, G. Giovannini, D. Dallacasa, K. Dolag, and G. B. Taylor, arXiv:1002.0594; T. E. Jeltema and S. Profumo, Astrophys. J. 728, 53 (2011); T. E. Clarke, P. P. Kronberg, and H. Boehringer, 547, L111 (2001); G. B. Taylor, A. C. Fabian, and S. W. Allen, Mon. Not. R. Astron. Soc. 334, 769 (2002); J. A. Eilek and F. N. Owen, Astrophys. J. 567, 202 (2002); C. Ferrari, F. Govoni, S. Schindler, A. M. Bykov, and Y. Rephaeli, Space Sci. Rev. 134, 93 (2008).
  33. R. Crocker, D. I. Jones, F. Melia, J. Ott, and R. J. Protheroe, Nature (London) 463, 65 (2010); R. Crocker, D. I. Jones, F. Aharonian, C. J. Law, F. Melia, and J. Ott, Mon. Not. R. Astron. Soc. 411, L11 (2011).
  34. T. G. Arshakian, R. Beck, M. Krause, D. Sokolff, and R. Stepanov, arXiv:0909.3001.
  35. A. A. Abdo et al. (The Fermi-LAT Collaboration), Phys. Rev. Lett. 104, 101101 (2010).
  36. C. Arina and M. H. G. Tytgat, J. Cosmol. Astropart. Phys. 01 (2011) 011.
  37. The Fermi-LAT Collaboration, Phys. Rev. Lett. 107, 241302 (2011); A. Geringer-Sameth and S. M. Koushiappas, 107, 241303 (2011).
  38. A. A. Abdo et al. (Fermi-LAT Collaboration), J. Cosmol. Astropart. Phys. 04 (2010) 014.
  39. M. Ackerman et al. (The Fermi-LAT Collaboration), Phys. Rev. D 85, 083007 (2012).
  40. D. Hooper and T. Linden, Phys. Rev. D 84, 123005 (2011); D. Hooper and L. Goodenough, Phys. Lett. B 697, 412 (2011).
  41. D. Hooper and T. Linden, Phys. Rev. D 83, 083517 (2011).
  42. R. Bernabei, P. Belli, F. Cappella et al., Eur. Phys. J. C 67, 39 (2010).
  43. C. E. Aalseth, P. S. Barbeau, J. Colaresi, J. I. Collar, J. Diaz Leon, J. E. Fast, N. Fields, T. W. Hossbach et al., Phys. Rev. Lett. 107, 141301 (2011); C. E. Aalseth et al. (CoGeNT Collaboration), 106, 131301 (2011).
  44. G. Angloher, M. Bauer, I. Bavykina, A. Bento, C. Bucci, C. Ciemniak, G. Deuter, F. von Feilitzsch et al., Eur. Phys. J. C 72, 1971 (2012).

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Phys. Rev. D 86, 103003– Published 5 November, 2012
  • Received 15 August 2012
Article part of CHORUS

© 2012 American Physical Society

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