We explore the possibility that the astrophysical neutrinos are produced in $pp$-interactions with a gas cloud near the source acting as a beam dump, which is sufficiently dense to significantly attenuate the associated gamma-ray flux through pair-production on this gas. In this way, such sources could potentially supply the astrophysical neutrino flux whilst avoiding the existing constraints on the non-blazar contribution to the extragalactic gamma-ray background. After defining our model, we implement a Monte Carlo simulation and apply this to different scenarios. First, we investigate a set of active galaxies which exhibit signs of obscuration. We find that, currently, the expected neutrino flux from these objects in our model is below the existing exclusion limits, but can already constrain the amount of protons accelerated in such sources. Second, we investigate the diffuse neutrino flux generated by a population of obscured sources. We find that such a population can indeed alleviate the tension with the extragalactic background light. We discuss the possibility that ultra-luminous infrared galaxies represent such a source class.
High-energy neutrinos from shocked circumnuclear material around optically-bright and infrared-only tidal disruption events
Fermi National Accelerator Laboratory（费米国家加速器实验室）；University of Chicago（芝加哥大学）；NSF-Simons AI Institute for the Sky (SkAI)（NSF-西蒙斯天空人工智能研究所）；Tohoku University（东北大学）；The University of Tokyo（东京大学）
Correlation Between Hard X-Ray and Cosmic Neutrino Sources: From Obscured AGN to Blazars
ELTE Eötvös Loránd University（厄特沃什·罗兰大学）；HUN-REN Research Centre for Astronomy and Earth Sciences（匈牙利研究与教育网络地球科学与天文学研究中心）；Ruhr University Bochum（波鸿鲁尔大学）；University of Florida（佛罗里达大学）；University of Geneva（日内瓦大学）；Universidad Diego Portales（迭戈·波特莱斯大学）；Chalmers University of Technology（查尔姆斯理工大学）；University of Wisconsin, Madison（威斯康星大学麦迪逊分校）
Neutrinos from hidden ultraluminous X-ray sources in the Galaxy
Instituto Argentino de Radioastronomía (CCT La Plata, CONICET（阿根廷射电天文研究所）；CICPBA（拉普拉塔国立大学天文与地球物理学院）；UNLP)（马德普拉塔物理研究所）；Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata（马德普拉塔国立大学理学院物理系）；Instituto de Investigaciones Físicas de Mar del Plata (IFIMAR – CONICET)；Departamento de Física, Facultad de Ciencias Exactas y Naturales, Universidad Nacional de Mar del Plata
High-Energy Neutrino Emission in NGC1068 driven by Turbulent Magnetic Reconnection
Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG-USP), Universidade de São Paulo（圣保罗大学地球物理与大气科学学院）；Centro Brasileiro de Pesquisas Físicas (CBPF)（巴西物理研究中心）
Assessing the Relative Importance of Neutrino Matter Interaction Channels in Post-Merger Remnant of Binary Neutron Stars
University of New Hampshire（新罕布什尔大学）；Cornell University（康奈尔大学）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；California Institute of Technology（加州理工学院）
Search for Point-Like Sources of Ultra-High Energy Neutrinos at the Pierre Auger Observatory and Improved Limit on the Diffuse Flux of Tau Neutrinos
皮埃尔·俄歇天文台的表面探测器阵列可以探测到能量在10^17 eV到10^20 eV之间的中微子，这些中微子来自于+55度以南和-65度以北的天空中的点状源。人们已经对大气中各种中微子相互作用（下行中微子）和地壳中τ中微子相互作用产生的τ轻子衰变（掠地中微子）产生的高度倾斜的大范围空气簇射进行了研究。截至2010年5月31日，在数据中没有发现候选中微子。这相当于全表面探测器阵列在掠地通道中的等效曝光时间约为3.5年，在下行通道中的等效曝光时间约为2年。导出了τ中微子扩散通量的一个改进的上限。从点源的中微子通量的上限已被推导出作为源decompensate的函数。假设来自点状源的中微子通量k_PS E ^-2为微分，则90% C. L。通过对掠地中微子和下行中微子的研究，在很宽的磁偏角范围内分别得到了k_PS的上限值约为5 x 10 ^-7和2.5 x 10 ^-6 GeV cm ^-2 s ^-1。
