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arXiv 2302.08784astro-ph.HEastro-ph.COhep-exhep-ph
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用VERITAS观测矮球状星系寻找超重暗物质

Search for Ultraheavy Dark Matter from Observations of Dwarf Spheroidal Galaxies with VERITAS

A. Acharyya, A. Archer, P. Bangale, J. T. Bartkoske, P. Batista, M. Baumgart, W. Benbow, J. H. Buckley, A. Falcone, Q. Feng, J. P. Finley, G. M. Foote, L. Forts… 展开作者

A. Acharyya, A. Archer, P. Bangale, J. T. Bartkoske, P. Batista, M. Baumgart, W. Benbow, J. H. Buckley, A. Falcone, Q. Feng, J. P. Finley, G. M. Foote, L. Fortson, A. Furniss, G. Gallagher, W. F. Hanlon, O. Hervet, J. Hoang, J. Holder, T. B. Humensky, W. Jin, P. Kaaret, M. Kertzman, M. Kherlakian, D. Kieda, T. K. Kleiner, N. Korzoun, F. Krennrich, M. J. Lang, M. Lundy, G. Maier, C. E McGrath, P. Moriarty, S. O'Brien, R. A. Ong, K. Pfrang, M. Pohl, E. Pueschel, J. Quinn, K. Ragan, P. T. Reynolds, E. Roache, N. L. Rodd, J. L. Ryan, I. Sadeh, L. Saha, M. Santander, G. H. Sembroski, R. Shang, M. Splettstoesser, D. Tak, J. V. Tucci, V. V. Vassiliev, D. A. Williams

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10 pages, 7 figures
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摘要：

暗物质是当前宇宙学场景的关键部分，弱相互作用大质量粒子（WIMP）是暗物质的主要候选者。WIMP在其常规参数空间（100 GeV $\lesssim M_χ \lesssim$ 100 TeV）中尚未被检测到，这是目前成像大气切伦科夫望远镜可以达到的质量范围。由于超重暗物质（UHDM; $M_χ \gtrsim$ 100 TeV）已被建议作为一个未充分探索的替代WIMP范式，我们寻找一个间接的暗物质湮灭信号在更高的质量范围（高达30 PeV）与VERITAS伽马射线天文台。通过对四个矮球状星系216小时的观测，我们进行了未分组似然分析。我们没有发现任何证据的$γ$射线信号UHDM湮灭以上的背景波动的任何个别矮星系，也没有一个联合拟合分析，因此限制速度加权湮灭截面UHDM的暗物质粒子质量之间的1 TeV和30 PeV。我们还对复合UHDM颗粒的允许半径设置了限制。

英文摘要：

Dark matter is a key piece of the current cosmological scenario, with weakly interacting massive particles (WIMPs) a leading dark matter candidate. WIMPs have not been detected in their conventional parameter space (100 GeV $\lesssim M_χ \lesssim$ 100 TeV), a mass range accessible with current Imaging Atmospheric Cherenkov Telescopes. As ultraheavy dark matter (UHDM; $M_χ \gtrsim$ 100 TeV) has been suggested as an under-explored alternative to the WIMP paradigm, we search for an indirect dark matter annihilation signal in a higher mass range (up to 30 PeV) with the VERITAS gamma-ray observatory. With 216 hours of observations of four dwarf spheroidal galaxies, we perform an unbinned likelihood analysis. We find no evidence of a $γ$-ray signal from UHDM annihilation above the background fluctuation for any individual dwarf galaxy nor for a joint-fit analysis, and consequently constrain the velocity-weighted annihilation cross section of UHDM for dark matter particle masses between 1 TeV and 30 PeV. We additionally set constraints on the allowed radius of a composite UHDM particle.

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