Search for gamma-ray lines in the Galaxy with DAMPE
- Autori: Alemanno F.; An Q.; Azzarello P.; Barbato F.C.T.; Bernardini P.; Bi X.J.; Cai M.S.; Casilli E.; Catanzani E.; Chang J.; Chen D.Y.; Chen J.L.; Chen Z.F.; Cui M.Y.; Cui T.S.; Cui Y.X.; Dai H.T.; De Benedittis A.; De Mitri I.; de Palma F.; Deliyergiyev M.; Di Santo M.; Ding Q.; Dong T.K.; Dong Z.X.; Donvito G.; Droz D.; Duan J.L.; Duan K.-K.; D'Urso D.; Fan R.R.; Fan Y.Z.; Fang K.; Fang F.; Feng C.Q.; Feng L.; Fusco P.; Gao M.; Gargano F.; Gong K.; Gong Y.Z.; Guo D.Y.; Guo J.H.; Han S.X.; Hu Y.M.; Huang G.S.; Huang X.Y.; Huang Y.Y.; Ionica M.; Jiang W.; Kong J.; Kotenko A.; Kyratzis D.; Lei S.J.; Li W.H.; Li W.L.; Li X.; Li X.Q.; Liang Y.M.; Liu C.M.; Liu H.; Liu J.; Liu S.B.; Liu Y.; Loparco F.; Luo C.N.; Ma M.; Ma P.X.; Ma T.; Ma X.Y.; Marsella G.; Mazziotta M.N.; Mo D.; Niu X.Y.; Pan X.; Parenti A.; Peng W.X.; Peng X.Y.; Perrina C.; Qiao R.; Rao J.N.; Ruina A.; Salinas M.M.; Shang G.Z.; Shen W.H.; Shen Z.-Q.; Shen Z.T.; Silveri L.; Song J.X.; Stolpovskiy M.; Su H.; Su M.; Sun H.R.; Sun Z.Y.; Surdo A.; Teng X.J.; Tykhonov A.; Wang H.; Wang J.Z.; Wang L.G.; Wang S.; Wang S.X.; Wang X.L.; Wang Y.; Wang Y.F.; Wang Y.Z.; Wei D.M.; Wei J.J.; Wei Y.F.; Wu D.; Wu J.; Wu L.B.; Wu S.S.; Wu X.; Xia Z.Q.; Xu E.H.; Xu H.T.; Xu Z.H.; Xu Z.-L.; Xu Z.Z.; Xue G.F.; Yang H.B.; Yang P.; Yang Y.Q.; Yao H.J.; Yu Y.H.; Yuan G.W.; Yuan Q.; Yue C.; Zang J.J.; Zhang F.; Zhang S.X.; Zhang W.Z.; Zhang Y.; Zhang Y.J.; Zhang Y.L.; Zhang Y.P.; Zhang Y.Q.; Zhang Z.; Zhang Z.Y.; Zhao C.; Zhao H.Y.; Zhao X.F.; Zhou C.Y.; Zhu Y.
- Anno di pubblicazione: 2022
- Tipologia: Contributo in atti di convegno pubblicato in rivista
- OA Link: http://hdl.handle.net/10447/613256
Abstract
DArk Matter Particle Explorer (DAMPE) has a great potential in the search of monochromatic and sharp gamma-ray structures in GeV-TeV range thanks to its good energy resolution. In this work, we search for gamma-ray line structures using 5.0 years of DAMPE data. To improve the sensitivity, we develop two types of data sets and adopt the signal-to-noise ratio optimized regions of interest (ROIs) for different DM density profiles. No line signals or candidates, including those located at 133 GeV and 43 GeV, are found between 10 GeV and 300 GeV in the Galaxy. Therefore we calculate the 95% confidence level constraints on the velocity-averaged cross section for χχ → γγ and the decay lifetime for χ → γν with systematic uncertainties included. Our constraints on DM parameters are mostly comparable to the Fermi-LAT 5.8-yr results. The lower limit for DM decay lifetime below 100 GeV are better than that of Fermi-LAT.