A search is made for neutrino-induced muons from Cyg X-3, Her X-1, LMC X-4, Vela X-1, Geminga (= 2CG 195+4), the Crab Nebula, Cen A, 3C 273, SS 433, and the center of our Galaxy using a large underground ring-imaging water Cerenkov detector. For this study, the detector is used to measure the track direction of upward-going muons (energy >2 GeV) produced by neutrino interactions in the surrounding rock. The measured flux is 2.41±0.21×10-13cm-2s-1sr-1 for zenith angles greater than 98°. This overall rate is consistent with that expected from ordinary cosmic-ray interactions with Earth's atmosphere, which is calculated to be 2.36±0.12 (statistical) ±0.35 (systematic) ×10-13cm-2sr-1. Upper limits are placed on the incident neutrino flux and luminosity of each object based on detailed computer simulations of the detector's effective area, efficiency, and energy threshold.
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Svoboda et al. (1987) studied this question.