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tokens: of SNe IIn at distances 22Mpc (40Mpc) is () 3 within 8yr in the Northern Sky (top panel in Fig. 9 ). During the period of 20102016, three SNe IIn were detected in the Northern Sky at a mean distance of 29Mpc (Table 3 ). Stacking of their neutrino signal could place stronger constraints on p than the diffuse neutrino flux by a factor of . Table 3. List of SNe IIn detected within 40Mpc over a period of 8yr (20082015). Notes. a Time of maximum optical light. b Available radio light curve. No radio observations exist for the rest of the sources. (1): Arbour Boles ( 2008 ); Botticella etal. ( 2009 ); Brown etal. ( 2014 ); (2): Chandra Soderberg ( 2008 ); (3): Maza etal. ( 2009 ); Fraser etal. ( 2013 ); Potashov etal. ( 2013 ); Mauerhan etal. ( 2013b ); Pastorello etal. ( 2013 ); Graham etal. ( 2014 ); Margutti etal. ( 2014 ); Brown etal. ( 2014 ); Fraser etal. ( 2015 ); (4): Nakano, Yusa Kadota ( 2009 ); (5): de Jaeger etal. ( 2015 ); Stritzinger etal. ( 2011 ); (6): Prieto Seth ( 2011 ); (7): Pastorello etal. ( 2011 ); Humphreys etal. ( 2012 ); Mauerhan etal. ( 2013c ); Brown etal. ( 2014 ); Ofek etal. ( 2014c ); (8): Antezana etal. ( 2013 ); (9): http://www.cbat.eps.harvard.edu/unconf/followups/J14041297-0938168.html ; (10): http://nesssi.cacr.caltech.edu/catalina/current.html ; (11): Terreran etal. ( 2016 ); Denisenko etal. ( 2014 ); (12): Elias-Rosa etal. ( 2015 , 2016 ); (13): Childress etal. ( 2015 ); (14): Zhang Wang ( 2015 ); (15): Masi etal. ( 2015 ); Challis etal. ( 2015 ); (16): Mauerhan etal. ( 2015 , 2017 ); Kankare etal. ( 2015 ). Neutrino production in pp collisions is accompanied by the injection of relativistic electronpositron pairs in the post-shock region and the production of GeV -ray photons via the decay of neutral pions. The first systematic search for -ray emission in Fermi -LATdata from the ensemble of 147 SNe IIn exploding in a dense CSM was recently presented by Ackermann etal. ( 2015 ). No significant excess above the background was found leading to model-independent -ray flux upper limits. These -ray non-detections constrained the ratio of the -ray to optical luminosity in the range 0.011. These can, in principle, be translated to limits on p . However, due to the uncertainty in the escaping fraction of -rays, no stringent limits could be placed on the proton acceleration efficiency. 4.3 IceCube neutrinos in coincidence with SNe IIn? Table 3 shows the detected SNe IIn in the local Universe (i.e. within a distance D L 40Mpc). Out of the 29 high-energy muon neutrinos detected in the Northern Sky above 200 TeV (Aartsen etal. 2016d ), none is found to be in spatial or temporal coincidence with these SNe IIn. However, one cascade-like event 4 from the 4-yr HESE IceCube sample (The IceCube Collaboration etal. 2015 ) was detected on MJD 55798.63, i.e. t 1.13 d after the peak of the SN2011fh optical light curve, with an angular offset of 712. 5 The coincident rate of SNe IIn in the local Universe ( z 0.1) during the time