搜索使用Anita的第三次飞行，寻找与天体物理源相关的超高能源中微子

论文标题

搜索使用Anita的第三次飞行，寻找与天体物理源相关的超高能源中微子

A search for ultrahigh-energy neutrinos associated with astrophysical sources using the third flight of ANITA

论文作者

Deaconu, C., Batten, L., Allison, P., Banerjee, O., Beatty, J. J., Belov, K., Besson, D. Z., Binns, W. R., Bugaev, V., Cao, P., Chen, C. H., Chen, P., Chen, Y., Clem, J. M., Connolly, A., Cremonesi, L., Dailey, B., Dowkontt, P. F., Fox, B. D., Gordon, J. W. H., Gorham, P. W., Hast, C., Hill, B., Hsu, S. Y., Huang, J. J., Hughes, K., Hupe, R., Israel, M. H., Liewer, K. M., Liu, T. C., Ludwig, A. B., Macchiarulo, L., Matsuno, S., McBride, K., Miki, C., Mulrey, K., Nam, J., Naudet, C., Nichol, R. J., Novikov, A., Oberla, E., Prohira, S., Prechelt, R., Rauch, B. F., Ripa, J., Roberts, J. M., Romero-Wolf, A., Rotter, B., Russell, J. W., Saltzberg, D., Seckel, D., Schoorlemmer, H., Shiao, J., Stafford, S., Stockham, J., Stockham, M., Strutt, B., Sutherland, M. S., Varner, G. S., Vieregg, A. G., Wang, N., Wang, S. H., Wissel, S. A.

论文摘要

南极冲动瞬态天线（ANITA）长持续气球实验对南极冰盖中超高能量（E> 10^{18} EV）中微子的相互作用敏感。 Anita的第三次飞行持续了22天，始于2014年12月。我们开发了一种方法，可以在空间和时间上与Anita数据中的潜在源类别相吻合。该方法应用于几个来源类别：TXS 0506+056 Blazar和NGC 1068，这是IceCube确定的第一个潜在的TEV Neutrino来源，由Fermi All-Sky-Kyky差异分析报告的高能量Blazars，gamma-ray-ray usbers and Gamma-ray usbers and supernovae报道。在五个源类中的搜索中，一名候选人被确定为与SN 2015D相关联，尽管没有统计学意义。我们继续在源类上放置上限。我们进一步评论了这种方法对更敏感的未来工具的潜在应用。

The ANtarctic Impulsive Transient Antenna (ANITA) long-duration balloon experiment is sensitive to interactions of ultra high-energy (E > 10^{18} eV) neutrinos in the Antarctic ice sheet. The third flight of ANITA, lasting 22 days, began in December 2014. We develop a methodology to search for energetic neutrinos spatially and temporally coincident with potential source classes in ANITA data. This methodology is applied to several source classes: the TXS 0506+056 blazar and NGC 1068, the first potential TeV neutrino sources identified by IceCube, flaring high-energy blazars reported by the Fermi All-Sky Variability Analysis, gamma-ray bursts, and supernovae. Among searches within the five source classes, one candidate was identified as associated with SN 2015D, although not at a statistically significant level. We proceed to place upper limits on the source classes. We further comment on potential applications of this methodology to more sensitive future instruments.

下载PDF全文

下载文献需遵守相关版权规定

论文标题