Diffuse supernova neutrino background is detectable in Super-Kamiokande

By S. Horiuchi, J. Beacom, E. Dwek. 2008

161 citations recorded by the source corpus.

The diffuse supernova neutrino background (DSNB) provides an immediate opportunity to study the emission of MeV thermal neutrinos from core-collapse supernovae. The DSNB is a powerful probe of stellar and neutrino physics, provided that the core-collapse rate is large enough and that its uncertainty is small enough. To assess the important physics enabled by the DSNB, we start with the cosmic star formation history of Hopkins and Beacom (2006) and confirm its normalization and evolution by cross-checks with the supernova rate, extragalactic background light, and stellar mass density. We find a sufficient core-collapse rate with small uncertainties that translate into a variation of {+-}40% in the DSNB event spectrum. Considering thermal neutrino spectra with effective temperatures between 4-6 MeV, the predicted DSNB is within a factor 4-2 below the upper limit obtained by Super-Kamiokande in 2003. Furthermore, detection prospects would be dramatically improved with a gadolinium-enhanced Super-Kamiokande: the backgrounds would be significantly reduced, the fluxes and uncertainties converge at the lower threshold energy, and the predicted event rate is 1.2-5.6 events yr{sup -1} in the energy range 10-26 MeV. These results demonstrate the imminent detection of the DSNB by Super-Kamiokande and its exciting prospects for studying stellar and neutrino physics.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8311e5ea465308c741e9e1af1464b444c734d0ce

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Citations in the corpus

Neutrino coherent scattering rates at direct dark matter detectors (2009, result): “The core-collapse rate is derived from the star-formation rate and stellar initial mass function; the calculations in the paper follow the recent results of Horiuchi et al [16].”
ROLE OF LINE-OF-SIGHT COSMIC-RAY INTERACTIONS IN FORMING THE SPECTRA OF DISTANT BLAZARS IN TeV GAMMA RAYS AND HIGH-ENERGY NEUTRINOS (2010, background): “A number of models fall in this range (Salamon & Stecker 1998; Kneiske et al. 2002, 2004; Stecker et al. 2007; Franceschini et al. 2008; Horiuchi et al. 2009; Primack et al. 2009; Gilmore et al. 2009; Razzaque et al. 2009; Finke et al. 2010).”
Galactic Searches for Dark Matter (2012, background): “These include Solar neutrinos, atmospheric neutrinos, and diffuse supernova neutrinos (Horiuchi et al., 2009; Beacom, 2010).”
THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, methodology): “We summarize the findings of Horiuchi et al. (2009) here.”
Revisiting the SN1987A gamma-ray limit on ultralight axion-like particles (2014, background): “Similar to the diffuse supernova neutrino background (DSNB) [76], the existence of axions and ALPs would lead to the presence of a diffuse supernova axion background (DSAB), and to a diffuse supernova ALP background (DSALPB), respectively [77].”
What can be learned from a future supernova neutrino detection (2017, background): “[210] lists the Fermi-Dirac temperatures for almost a dozen”
ACCELERATING COMPACT OBJECT MERGERS IN TRIPLE SYSTEMS WITH THE KOZAI RESONANCE: A MECHANISM FOR “PROMPT” TYPE Ia SUPERNOVAE, GAMMA-RAY BURSTS, AND OTHER EXOTICA (2010, background): “Similarly, the massive star birthrate, which is ap- 1 Alfred P. Sloan Fellow proximately equal to the Type-II supernova rate,∼ 105 Gpc−3 yr−1 (e.g., Horiuchi et al. 2009), is∼ 20− 600 times larger than the NS-NS merger rate (Kalogera et al. 2001, 2004ab; O’Shaughnessy et al. 2008).”
The extragalactic background light and the gamma-ray opacity of the universe (2012, background): “The total EBL intensity can therefore be used to derive an estimate of the supernova rate and the resulting flux of supernova neutrinos (Horiuchi et al., 2009; Beacom, 2010).”