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Gamma-ray emission from warm WIMP annihilation. Qiang Yuan Institute of High Energy Physics Collaborated with Xiaojun Bi, Yixian Cao, Jie Liu, Liang Gao, Pengfei Yin & Xinmin Zhang (arXiv:1203.5636) KITPC cosmology month 2012-09-05. Outline. Introduction of cold/warm dark matter - PowerPoint PPT Presentation
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Gamma-ray emission from warm WIMP annihilation
Qiang YuanInstitute of High Energy Physics
Collaborated with Xiaojun Bi, Yixian Cao, Jie Liu, Liang Gao, Pengfei Yin & Xinmin Zhang
(arXiv:1203.5636)
KITPC cosmology month2012-09-05
Outline
• Introduction of cold/warm dark matter
• Gamma-ray emission of warm WIMP based on numerical simulations
• Conclusion
Bottom-up structure formation pattern instead of top-down pattern (fragmentation): cold dark matter
Structure evolution: cold dark matter
Springel et al. (2006) Nature
CDM simulation vs. galaxy survey
How cold is dark matter?
The coldness of dark matter depends on the free-streaming scale during the formation of structures
• Hot dark matter (eV neutrinos) that washes out fluctuations on cluster scale (10 Mpc/h)
• Warm dark matter (sterile neutrinos) that washes out fluctuations on galaxy scale (1 Mpc/h)
• Cold dark matter that has effectively zero thermal velocity
From Jing’s Nanjing talk (2012)
How cold is dark matter: matter power spectrum
Tegmark et al. (2004)
WDM
CDM
How cold is dark matter: number of satellites
Jing (2001)
How cold is dark matter: circular velocity of Milky Way satellites
Lovell et al. (2012)
How cold is dark matter: velocity width function of galaxies (ALFALFA survey)
Papastergis et al. (2011)
How cold is dark matter: central density of dwarf galaxies
S. Shao’s talk on Friday
Burkert (1995)
Observational summary
• Large scale structures are very close to CDM
• At (sub-)galactic scales, many discrepancies between observations and CDM expected (abundance, density profile, velocity profile)
• WDM can better explain the observations
Detection of WDM particles?
• Traditionally, WDM is light (e.g., sterile neutrinos)
• Most of DM experiments are dedicated on WIMPs; it is fatal if DM is warm and light
• Nevertheless, if non-thermally produced, WIMPs could also be warm (Jeannerot et al., 1999; Lin et al., 2001; Bi et al. 2009)
• Another feature of non-thermal WIMPs is that larger annihilation cross section (compared with 3×10-26 cm3 s) is plausible
• DM particles are produced through decay of very heavy particles (e.g., from cosmic string) and carry very large initial momentum
• Large initial momentum will correspond to a large free-streaming length
Non-thermal warm WIMP
Matter power spectrum
2 keV WDM
NTDMrc=10-
7
Outline
• Introduction of cold/warm dark matter
• Gamma-ray emission of warm WIMP based on numerical simulations
• Conclusion
Simulations
2keV WDMLovell et al. (2012)
CDM: AquariusSpringel et al. (2008)
(Sub-)halo density profile
• Core in the center
• Core size is anti-correlated with halo mass
• For Milky-Way halo, CDM and WDM profiles are identical within resolution
Subhalo statistics
M vs. L≡∫2dV M vs. F≡L/d2
Spatial skymaps: CDM
Spatial skymaps: WDM
Two supersymmetric benchmark models
Total skymaps with diffuse background (E>10 GeV)
Detectability comparison
Impact on direct detection
• Velocity distribution?
• Nucleon-DM scattering cross section?
Conclusion
• Subhalos are less abundant for WDM, resulting a very flat subhalo luminosity function
• It is currently difficult to detect either the cold or warm WIMPs, but the detectability of warm WIMP can be in principle better than cold WIMP due to a potentially larger cross section
• For DM indirect search strategy, the Galactic center may be prior to dwarf galaxies for warm WIMP scenario (different from that for cold WIMPs)
Thank youThank you