Outline Introduction Fitting the gCe in the Nmssm GCE solutions with H, being the SM-like Higgs boson Solution -the bb annihilation channel Solution ll- the hua, annihilation channel Solution lll -the wtw-annihilation channel GCE solutions with H, being the SM-like higgs boson Solution v-the h,a, annihilation channel Solution V- the h,A, annihilation channel Explore the gCe solutions in future experiments ● Summary
Outline 11 • Summary • Introduction • Fitting the GCE in the NMSSM • Explore the GCE solutions in future experiments • GCE solutions with H2 being the SM-like Higgs boson • GCE solutions with H1 being the SM-like Higgs boson • Solution I - the 𝑏𝑏ത annihilation channel • Solution II - the H1A1 annihilation channel • Solution III - the W +W — annihilation channel • Solution IV - the H1A1 annihilation channel • Solution V – the H2A1 annihilation channel
Introduction Dark Matter Annihilation and ndirect Detection Indirect Dark Matter searches HE DM MAGIC Fermi LAT M (o)a3×10-26cm3s-1 EGRET Integra WMAP From Weniger's talk Planck B-field Searching WIMPs , Weakly Interacting Fermi LAT Massive Particles ATIC Compatible with observed relic density due to self- annihilation in early icecube Universe SuperK Still annihilate today → contribute to cosmic From Christoph Weniger's talk
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Introduction Fermi-laT and dark atter ndirect Detection 日June11,2008 From Fermi colla boration' s talk Fermi Gamma-ray Space Telescope on a delta ii rocket shuttle toward s 550 km to orbit Earth every 95 min a Bigger and better successor to the EgRET (Energetic Gamma Ray Exp. Telescope) Operational from 1991-2000 u Fermi includes two scientific instruments Large Area Telescope(LAT) Gamma-ray Burst Monitor(GBM) u Fermi is mainly a gamma-ray telescope, but is a good electron and positron detector too
Introduction 13
Introduction Spatial residuals with New Cut a010-6 NFW. 71.2 nner Galaxy Galactic Center After the cut on CTBCORE. An apparent north/south asymmetry previously noted in the extended (inner Galaxy) excess is removed. The new preferred slope is y=1. 26 in the inner Galaxy analysis, Y=1. 1-1.2 in the Galactic Center. The spectra measured in different regions are more consistent, especially at low energies. The low-energy spectrum becomes harder Daylan et aL. (1402. 6703)
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Introduction DM coupling to SM induces y interactions Parton shower hadronization Adapted from D Zepp PITPOS
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