论文标题

ICECUBE高能量开始事件样本:描述和通量表征7。5年

The IceCube high-energy starting event sample: Description and flux characterization with 7.5 years of data

论文作者

Abbasi, R., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Alispach, C., Alves Jr., A. A., Amin, N. M., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Argüelles, C., Axani, S., Bai, X., V., A. Balagopal, Barbano, A., Barwick, S. W., Bastian, B., Basu, V., Baum, V., Baur, S., Bay, R., Beatty, J. J., Becker, K. -H., Tjus, J. Becker, Bellenghi, C., BenZvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Böser, S., Botner, O., Böttcher, J., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Bron, S., Brostean-Kaiser, J., Burgman, A., Busse, R. S., Campana, M. A., Chen, C., Chirkin, D., Choi, S., Clark, B. A., Clark, K., Classen, L., Coleman, A., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., De Clercq, C., DeLaunay, J. J., Dembinski, H., Deoskar, K., De Ridder, S., Desai, A., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Dharani, S., Diaz, A., Díaz-Vélez, J. C., Dujmovic, H., Dunkman, M., DuVernois, M. A., Dvorak, E., Ehrhardt, T., Eller, P., Engel, R., Evans, J., Evenson, P. A., Fahey, S., Fazely, A. R., Fiedlschuster, S., Fienberg, A. T., Filimonov, K., Finley, C., Fischer, L., Fox, D., Franckowiak, A., Friedman, E., Fritz, A., Fürst, P., Gaisser, T. K., Gallagher, J., Ganster, E., Garrappa, S., Gerhardt, L., Ghadimi, A., Glauch, T., Glüsenkamp, T., Goldschmidt, A., Gonzalez, J. G., Goswami, S., Grant, D., Grégoire, T., Griffith, Z., Griswold, S., Gündüz, M., Haack, C., Hallgren, A., Halliday, R., Halve, L., Halzen, F., Minh, M. Ha, Hanson, K., Hardin, J., Haungs, A., Hauser, S., Hebecker, D., Helbing, K., Henningsen, F., Hickford, S., Hignight, J., Hill, C., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Huber, T., Hultqvist, K., Hünnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jansson, M., Japaridze, G. S., Jeong, M., Jones, B. J. P., Joppe, R., Kang, D., Kang, W., Kang, X., Kappes, A., Kappesser, D., Karg, T., Karl, M., Karle, A., Katori, T., Katz, U., Kauer, M., Kellermann, M., Kelley, J. L., Kheirandish, A., Kim, J., Kin, K., Kintscher, T., Kiryluk, J., Klein, S. R., Koirala, R., Kolanoski, H., Köpke, L., Kopper, C., Kopper, S., Koskinen, D. J., Koundal, P., Kovacevich, M., Kowalski, M., Krings, K., Krückl, G., Kulacz, N., Kurahashi, N., Kyriacou, A., Gualda, C. Lagunas, Lanfranchi, J. L., Larson, M. J., Lauber, F., Lazar, J. P., Leonard, K., Leszczyńska, A., Li, Y., Liu, Q. R., Lohfink, E., Mariscal, C. J. Lozano, Lu, L., Lucarelli, F., Ludwig, A., Luszczak, W., Lyu, Y., Ma, W. Y., Madsen, J., Mahn, K. B. M., Makino, Y., Mallik, P., Mancina, S., Mandalia, S., Mariş, I. C., Maruyama, R., Mase, K., McNally, F., Meagher, K., Medina, A., Meier, M., Meighen-Berger, S., Merz, J., Micallef, J., Mockler, D., Momenté, G., Montaruli, T., Moore, R. W., Morse, R., Moulai, M., Naab, R., Nagai, R., Naumann, U., Necker, J., Neer, G., Nguyen, L. V., Niederhausen, H., Nisa, M. U., Nowicki, S. C., Nygren, D. R., Pollmann, A. Obertacke, Oehler, M., Olivas, A., O'Sullivan, E., Pandya, H., Pankova, D. V., Park, N., Parker, G. K., Paudel, E. N., Peiffer, P., Heros, C. Pérez de los, Philippen, S., Pieloth, D., Pieper, S., Pizzuto, A., Plum, M., Popovych, Y., Porcelli, A., Rodriguez, M. Prado, Price, P. B., Przybylski, G. T., Raab, C., Raissi, A., Rameez, M., Rawlins, K., Rea, I. C., Rehman, A., Reimann, R., Renschler, M., Renzi, G., Resconi, E., Reusch, S., Rhode, W., Richman, M., Riedel, B., Robertson, S., Roellinghoff, G., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Cantu, D. Rysewyk, Safa, I., Herrera, S. E. Sanchez, Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Sarkar, S., Satalecka, K., Scharf, M., Schaufel, M., Schieler, H., Schlunder, P., Schmidt, T., Schneider, A., Schneider, J., Schröder, F. G., Schumacher, L., Sclafani, S., Seckel, D., Seunarine, S., Shefali, S., Silva, M., Smithers, B., Snihur, R., Soedingrekso, J., Soldin, D., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Strotjohann, N. L., Stuttard, T., Sullivan, G. W., Taboada, I., Tenholt, F., Ter-Antonyan, S., Tilav, S., Tischbein, F., Tollefson, K., Tomankova, L., Tönnis, C., Toscano, S., Tosi, D., Trettin, A., Tselengidou, M., Tung, C. F., Turcati, A., Turcotte, R., Turley, C. F., Twagirayezu, J. P., Ty, B., Unger, E., Elorrieta, M. A. Unland, Vandenbroucke, J., van Eijk, D., van Eijndhoven, N., Vannerom, D., van Santen, J., Verpoest, S., Vraeghe, M., Walck, C., Wallace, A., Wandkowsky, N., Watson, T. B., Weaver, C., Weindl, A., Weiss, M. J., Weldert, J., Wendt, C., Werthebach, J., Weyrauch, M., Whelan, B. J., Whitehorn, N., Wiebe, K., Wiebusch, C. H., Williams, D. R., Wolf, M., Wood, T. R., Woschnagg, K., Wrede, G., Wulff, J., Xu, X. W., Xu, Y., Yanez, J. P., Yoshida, S., Yuan, T., Zhang, Z.

论文摘要

Icecube中微子天文台已经确定了天体物理起源的高能量全天气中微子通量的存在。这一发现是使用在检测器的基准区域中相互作用的事件进行的,该事件被活跃的否决权围绕,重建能量以上超过60 TEV,通常称为高能量开始事件样本,或者是HESE。我们通过额外的4。5年的数据,更新的冰川冰模型和改进的系统治疗来重新审视对HESE样本的分析。本文详细介绍了样本,报告了最新的天体中微子通量测量结果,并提供了对天体中性中微子的来源搜索。我们提供了这些观察结果与文献中提出的特定各向同性通量模型以及通用幂律样情况的兼容性。假设$ν_e:ν_μ:ν_τ= 1:1:1 $,以及中微子和抗神经酸酯的同等通量,我们发现天体中微子中微子光谱与不间断的功率定律相吻合,具有$ {2.87}^2.87}^{+0.20} $ 60} $ 60} $ $ 0.19的优先光谱指数 间隔。

The IceCube Neutrino Observatory has established the existence of a high-energy all-sky neutrino flux of astrophysical origin. This discovery was made using events interacting within a fiducial region of the detector surrounded by an active veto and with reconstructed energy above 60 TeV, commonly known as the high-energy starting event sample, or HESE. We revisit the analysis of the HESE sample with an additional 4.5 years of data, newer glacial ice models, and improved systematics treatment. This paper describes the sample in detail, reports on the latest astrophysical neutrino flux measurements, and presents a source search for astrophysical neutrinos. We give the compatibility of these observations with specific isotropic flux models proposed in the literature as well as generic power-law-like scenarios. Assuming $ν_e:ν_μ:ν_τ=1:1:1$, and an equal flux of neutrinos and antineutrinos, we find that the astrophysical neutrino spectrum is compatible with an unbroken power law, with a preferred spectral index of ${2.87}^{+0.20}_{-0.19}$ for the $68.3\%$ confidence interval.

扫码加入交流群

加入微信交流群

微信交流群二维码

扫码加入学术交流群,获取更多资源