提示来自Antares银河山脊的TEV中微子发射

论文标题

提示来自Antares银河山脊的TEV中微子发射

Hint for a TeV neutrino emission from the Galactic Ridge with ANTARES

论文作者

Albert, A., Alves, S., André, M., Ardid, M., Ardid, S., Aubert, J. -J., Aublin, J., Baret, B., Basa, S., Becherini, Y., Belhorma, B., Bendahman, M., Benfenati, F., Bertin, V., Biagi, S., Bissinger, M., Boumaaza, J., Bouta, M., Bouwhuis, M. C., Brânzaş, H., Bruijn, R., Brunner, J., Busto, J., Caiffi, B., Calvo, D., Campion, S., Capone, A., Caramete, L., Carenini, F., Carr, J., Carretero, V., Celli, S., Cerisy, L., Chabab, M., Chau, T. N., Moursli, R. Cherkaoui El, Chiarusi, T., Circella, M., Coelho, J. A. B., Coleiro, A., Coniglione, R., Coyle, P., Creusot, A., Díaz, A. F., De Martino, B., Distefano, C., Di Palma, I., Domi, A., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., van Eeden, T., van Eijk, D., Hedri, S. El, Khayati, N. El, Enzenhöfer, A., Fasano, M., Fermani, P., Ferrara, G., Filippini, F., Fusco, L., Gagliardini, S., García, J., Oliver, C. Gatius, Gay, P., Geißelbrecht, N., Glotin, H., Gozzini, R., Ruiz, R. Gracia, Graf, K., Guidi, C., Haegel, L., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hernández-Rey, J. J., Hößl, J., Hofestädt, J., Huang, F., Illuminati, G., James, C. W., Jisse-Jung, B., de Jong, M., de Jong, P., Kadler, M., Kalekin, O., Katz, U., Kouchner, A., Kreykenbohm, I., Kulikovskiy, V., Lahmann, R., Lamoureux, M., Lazo, A., Lefèvre, D., Leonora, E., Levi, G., Stum, S. Le, Lopez-Coto, D., Loucatos, S., Maderer, L., Manczak, J., Marcelin, M., Margiotta, A., Marinelli, A., Martínez-Mora, J. A., Migliozzi, P., Moussa, A., Muller, R., Nauta, L., Navas, S., Neronov, A., Nezri, E., Fearraigh, B. Ó, Păun, A., Păvălaş, G. E., Perrin-Terrin, M., Pestel, V., Piattelli, P., Poirè, C., Popa, V., Pradier, T., Randazzo, N., Real, D., Reck, S., Riccobene, G., Romanov, A., Sánchez-Losa, A., Saina, A., Greus, F. Salesa, Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Savchenko, D., Schnabel, J., Schumann, J., Schüssler, F., Seneca, J., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Tingay, S. J., Vallage, B., Vannoye, G., Van Elewyck, V., Viola, S., Vivolo, D., Wilms, J., Zavatarelli, S., Zegarelli, A., Zornoza, J. D., Zúñiga, J.

论文摘要

银河系内部的星际介质中宇宙射线质子，原子核和电子的相互作用产生了银河脊的$γ$ ray通量。如果$γ$ ray的发射由质子和核相互作用主导，则预期与$γ$ - ray磁通相媲美的中微子通量将从同一天空区域中。 Antares中微子望远镜收集的数据用于限制1-100 TEV能量范围内银河脊的中微子通量。在分析中考虑了作为轨道和淋浴的重建的中微子事件，并且选择了用于搜索该区域过剩的选择。 <30°$，$ | b | <2°$。使用具有相似天空覆盖的区域区域估算搜索区域的预期背景。中微子信号源自光谱索引范围从$γ_ν= 1 $到$ 4 $的幂律光谱。拟合观察到的能量分布以限制脊的中微子发射。信号区域中的能量分布与背景期望在$ \ sim 96 \％$置信水平不一致。轻度过度超过背景与具有频谱索引$ 2.45^{+0.22} _ { - 0.34} $的中微子通量一致，$ 2.45^{+0.22} $和Flux归一化$DN_ν/DE_ν/DE_ν= 4.0^{+2.7} \ text {cm}^{ - 2} \ text {s}^{ - 1} \ text {sr}^{ - 1} $在40 tev参考能量。如果从银河脊中观察到的$γ$ ray通量中的大部分频率源于宇宙射线质子和核与幂律频谱的相互作用，则这种通量与预期的中微子信号一致。

Interactions of cosmic ray protons, atomic nuclei, and electrons in the interstellar medium in the inner part of the Milky Way produce a $γ$-ray flux from the Galactic Ridge. If the $γ$-ray emission is dominated by proton and nuclei interactions, a neutrino flux comparable to the $γ$-ray flux is expected from the same sky region. Data collected by the ANTARES neutrino telescope are used to constrain the neutrino flux from the Galactic Ridge in the 1-100 TeV energy range. Neutrino events reconstructed both as tracks and showers are considered in the analysis and the selection is optimized for the search of an excess in the region $|l| < 30°$, $|b| < 2°$. The expected background in the search region is estimated using an off-zone region with similar sky coverage. Neutrino signal originating from a power-law spectrum with spectral index ranging from $Γ_ν=1$ to $4$ is simulated in both channels. The observed energy distributions are fitted to constrain the neutrino emission from the Ridge. The energy distributions in the signal region are inconsistent with the background expectation at $\sim 96\%$ confidence level. The mild excess over the background is consistent with a neutrino flux with a power law with a spectral index $2.45^{+0.22}_{-0.34}$ and a flux normalization $dN_ν/dE_ν= 4.0^{+2.7}_{-2.0} \times 10^{-16} \text{GeV}^{-1} \text{cm}^{-2} \text{s}^{-1} \text{sr}^{-1}$ at 40 TeV reference energy. Such flux is consistent with the expected neutrino signal if the bulk of the observed $γ$-ray flux from the Galactic Ridge originates from interactions of cosmic ray protons and nuclei with a power-law spectrum extending well into the PeV energy range.

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