摘要We evaluate the spin-independent elastic dark matter-nucleon scattering cross section in the framework of the simple singlet fermionic dark matter extension of the standard model and constrain the model parameter space with the following considerations: (i) new dark matter measurement, in which, apart from WMAP and CDMS, the results from the XENON experiment are also used in constraining the model; (ii) new fitted value of the quark fractions in nucleons, in which the updated value of fTs from the recent lattice simulation is much smaller than the previous one and may reduce the scattering rate significantly; (iii) new dark matter annihilation channels, in which the scenario where top quark and Higgs pairs produced by dark matter annihilation was not included in the previous works. We find that unlike in the minimal supersymmetric standard model, the cross section is just reduced by a factor of about 1/4 and dark matter lighter than 100 GeV is not favored by the WMAP, CDMS and XENON experiments.
Abstract：We evaluate the spin-independent elastic dark matter-nucleon scattering cross section in the framework of the simple singlet fermionic dark matter extension of the standard model and constrain the model parameter space with the following considerations: (i) new dark matter measurement, in which, apart from WMAP and CDMS, the results from the XENON experiment are also used in constraining the model; (ii) new fitted value of the quark fractions in nucleons, in which the updated value of fTs from the recent lattice simulation is much smaller than the previous one and may reduce the scattering rate significantly; (iii) new dark matter annihilation channels, in which the scenario where top quark and Higgs pairs produced by dark matter annihilation was not included in the previous works. We find that unlike in the minimal supersymmetric standard model, the cross section is just reduced by a factor of about 1/4 and dark matter lighter than 100 GeV is not favored by the WMAP, CDMS and XENON experiments.
[1] Bennett C L et al [WMAP Collaboration] 2003 Astrophys. J. Suppl. 148 1
Spergel D N et al [WMAP Collaboration] 2003 Astrophys. J. Suppl. 148 175
Hinshaw G et al [WMAP Collaboration] 2009 Astrophys. J. Suppl. 180 225
[2] Ahmed Z et al [The CDMS-II Collaboration] 2010 Science 327 1619
[3] Aprile E et al [XENON100 Collaboration] 2011 arXiv:1104.2549 [astro-ph.CO]
[4] Jungman G, Kamionkowski M and Griest K 1996 Phys. Rept. 267 195
Bertone G, Hooper D and Silk J 2005 Phys. Rept. 405 279
Wang W W et al 2009 J. High Energy Phys. 0911 053
[5] Cheng H C, Feng J L and Matchev K T 2002 Phys. Rev. Lett. 89 211301
Servant G and Tait T M P 2003 Nucl. Phys. B 650 391
[6] Zhu S H 2007 Chin. Phys. Lett. 24 381
[7] Kim Y G and Lee K Y 2007 Phys. Rev. D 75 115012
[8] Kim Y G, Lee K Y and Shin S 2008 J. High Energy Phys. 0805 100
[9] Lee K Y, Kim Y G and Shin S 2008 arXiv:0809.2745 [hep-ph]
[10] Kim Y G and Shin S 2009 J. High Energy Phys. 0905 036
[11] Ettefaghi M M 2009 Phys. Rev. D 79 065022
[12] Ellis J R, Ferstl A and Olive K A 2000 Phys. Lett. B 481 304
[13] Cao J, Hikasa K -i, Wang W W, Yang J M and Yu L -X 2010 Phys. Rev. D 82 051701
Cao J, Hikasa K -i, Wang W W, Yang J M and Yu L -X 2010 J. High Energy Phys. 1007 044
[14] Nihei T et al 2002 J. High Energy Phys. 0203 031
[15] Kolb E W and Turner M 1990 The Early Universe (Boulder: Westview Press)
[16] Nihei T and Sasagawa M 2004 Phys. Rev. D 70 055011
[17] Hisano J, Ishiwata K and Nagata N 2010 Phys. Rev. D 82 115007
[18] Bottino A, Donato F, Mignola G, Scopel S, Belli P and Incicchitti A 1997 Phys. Lett. B 402 113
[19] Djouadi A, Kalinowski J and Spira M 1998 Comput. Phys. Commun. 108 56
2011, Vol. 28 
