Multi-TeV dark matter density in the inner Milky Way halo: spectral and dynamical constraints

被引:5
作者
Zuriaga-Puig, Jaume [1 ,2 ]
Gammaldi, Viviana [1 ,2 ]
Gaggero, Daniele [3 ]
Lacroix, Thomas [4 ]
Sanchez-Conde, M. A. [1 ,2 ]
机构
[1] IFT UAM CSIC, Inst Fis Teor, Calle Nicolas Cabrera 13-15,Campus Cantoblanco, E-28049 Madrid, Spain
[2] Univ Autonoma Madrid, Dept Fis Teor, Modulo 15, E-28049 Madrid, Spain
[3] INFN, Sez Pisa, Polo Fibonacci Largo B Pontecorvo 3, I-56127 Pisa, Italy
[4] 5 B Rue Francisque Jomard, F-69600 Oullins, France
关键词
dark matter theory; gamma ray theory; galaxy morphology; GALACTIC-CENTER; ANNIHILATION;
D O I
10.1088/1475-7516/2023/11/063
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We develop a comprehensive study of the gamma-ray flux observed by the High Energy Stereoscopic System (H.E.S.S.) in 5 regions of the Galactic Center (GC). Motivated by previous works on a possible Dark Matter (DM) explanation for the TeV cut-off observed by H.E.S.S. in the innermost similar to 15 pc of the Galaxy, we aim to constrain the DM distribution up to a radius of similar to 450 pc from the GC. In this region, the benchmark approach (e.g. cosmological simulations and Galactic dynamics studies) fails to produce a strong prediction of the DM profile. Within our proof-of-concept analysis, we use DRAGON to model the diffuse background emission and determine upper limits on the density distribution of thermal multi-TeV Weakly Interactive Massive Particles (WIMPs), compatible with the observed gamma-ray flux. The results are in agreement with the hypothesis of an enhancement of the DM density in the GC with respect to the benchmark Navarro-Frenk-White (NFW) profile (-y = 1) and allow us to exclude profiles with an inner slope cuspier than-y greater than or similar to 1.3. We also investigate the possibility that such an enhancement could be related to the existence of a DM spike associated with the supermassive black hole Sgr A* at the GC. We find out that the existence of an adiabatic DM spike smoothed by the scattering off of WIMPs by the bulge stars may be consistent with the observed gamma-ray flux if the spike forms on an underlying generalized NFW profile with gamma less than or similar to 0.8, corresponding to a spike slope of gamma sp-star = 1.5 and spike radius of Rsp-stars similar to 25-30 pc. Instead, in the extreme case of the instantaneous growth of the black hole, the underlying profile could have up to gamma similar to 1.2, a corresponding gamma sp-inst = 1.4 and Rsp-inst similar to 15-25 pc. Finally, the results of our analysis of the total DM mass enclosed within the S2 orbit (updated with new GRAVITY data) are less stringent than the spectral analysis. Our work aims to guide future studies of the GC region, with both current and next generation of telescopes. In particular, the next Cherenkov Telescope Array will be able to scan the GC region with improved flux sensitivity and angular resolution.
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