The Diffuse Supernova Neutrino Background

Beacom, J. F.

doi:10.1146/annurev.nucl.010909.083331

Cited by 293 publications

(304 citation statements)

References 119 publications

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“…The evolution of the cosmic SFR density suggested by these measurements are well fitted by a power law ρ SFR = ρ SFR (0)(1 + z) 4.5 ± 0.7 , while if we consider also the other results of recent emission line surveys for the SFR density over 0 ≤ z ≤ 1.5 the evolution is given by ρ SFR = ρ SFR (0)(1 + z) 3.4 ± 0.4 (Hopkins & Beacom 2006;Horiuchi et al 2009;Dale et al 2010). The evolution with redshift of the volumetric CC SN rate can be fitted with a power law (1 + z) 3.6 (Botticella et al 2008;Bazin et al 2009) so the CC SN rate evolution seems to be consistent with that of SFR in a wide range of redshift but there is a problem in the normalisation (Hopkins & Beacom 2006;Botticella et al 2008;Beacom 2010;Horiuchi et al 2011). We also emphasise that the prediction of the stellar mass density based on the integrated SFH also exceeds the observed value at the present epoch by a factor of two and remains systematically higher with cosmic time evolution 5 (Wilkins et al 2008).…”

Section: Comparison Of Sfr Indicatorsmentioning

confidence: 90%

“…Horiuchi et al (2011) adopted a SFR density of 0.017 M Mpc −3 yr −1 for H 0 = 73 km s −1 Mpc −1 that becomes 0.018 M Mpc −3 yr −1 H 0 = 75 km s −1 Mpc −1 obtaining a CC SN rate of 1.5 × 10 −4 Mpc −3 yr −1 . The luminosity density estimate j B is independent of the SFR measurements used by Beacom (2010) and Horiuchi et al (2011).…”

Section: Appendix C: CC Sn Rate Per Unit Luminosity and Massmentioning

confidence: 99%

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A comparison between star formation rate diagnostics and rate of core collapse supernovae within 11 Mpc

Botticella

Smartt

Kennicutt

et al. 2012

A&A

124

135

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Aims. The core collapse supernova rate provides a strong lower limit for the star formation rate (SFR). Progress in using it as a cosmic SFR tracer requires some confidence that it is consistent with more conventional SFR diagnostics in the nearby Universe. This paper compares standard SFR measurements based on Hα, far ultraviolet (FUV) and total infrared (TIR) galaxy luminosities with the observed core collapse supernova rate in the same galaxy sample. The comparison can be viewed from two perspectives. Firstly, by adopting an estimate of the minimum stellar mass to produce a core collapse supernova one can determine a SFR from supernova numbers. Secondly, the radiative SFR can be assumed to be robust and then the supernova statistics provide a constrain on the minimum stellar mass for core collapse supernova progenitors. Methods. The novel aspect of this study is that Hα, FUV and TIR luminosities are now available for a complete galaxy sample within the local 11 Mpc volume and the number of discovered supernovae in this sample within the last 13 years is high enough to perform a meaningful statistical comparison. We exploit the multi-wavelength dataset from 11 HUGS, a volume-limited survey designed to provide a census of SFR in the Local Volume. There are 14 supernovae discovered in this sample of galaxies within the last 13 years. Although one could argue that this may not be complete, it is certainly a robust lower limit. Results. Assuming a lower limit for core collapse of 8 M (as proposed by direct detections of SN progenitor stars and white dwarf progenitors), the core-collapse supernova rate matches the SFR from the FUV luminosity. However, the SFR based on Hα luminosity is lower than these two estimates by a factor of nearly 2. If we assume that the FUV or Hα based luminosities are a true reflection of the SFR, we find that the minimum mass for core collapse supernova progenitors is 8 ± 1 M and 6 ± 1 M , respectively. Conclusions. The estimate of the minimum mass for core collapse supernova progenitors obtained exploiting FUV data is in good agreement with that from the direct detection of supernova progenitors. The concordant results by these independent methods point toward a constraint of 8 ± 1 M on the lower mass limit for progenitor stars of core collapse supernovae.

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Section: Comparison Of Sfr Indicatorsmentioning

confidence: 90%

Section: Appendix C: CC Sn Rate Per Unit Luminosity and Massmentioning

confidence: 99%

A comparison between star formation rate diagnostics and rate of core collapse supernovae within 11 Mpc

Botticella

Smartt

Kennicutt

et al. 2012

A&A

124

135

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show abstract

“…Most of the elements involved in a comprehensive prediction of the SRN flux are now fairly well known [32] SK 1497+794+562 Days (e.g. initial mass functions, cosmic star formation history, Hubble expansion, etc.…”

Section: B Typical Sn ν Emission Limitmentioning

confidence: 99%

Supernova relic neutrino search at super-Kamiokande

Bays¹,

Iida²,

Abe³

et al. 2012

Phys. Rev. D

198

293

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A new Super-Kamiokande (SK) search for Supernova Relic Neutrinos (SRNs) was conducted using 2853 live days of data. Sensitivity is now greatly improved compared to the 2003 SK result, which placed a flux limit near many theoretical predictions. This more detailed analysis includes a variety of improvements such as increased efficiency, a lower energy threshold, and an expanded data set. New combined upper limits on SRN flux are between 2.8 and 3.0νe cm −2 s −1 > 16 MeV total positron energy (17.3 MeV Eν).

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“…The DSNB flux is a convolution of the core-collapse supernova rate as a function of redshift with the neutrino spectrum per supernova; for a recent review of the predicted DSNB flux see Beacom [25]. The DSNB spectra have a similar form to a Fermi-Dirac spectrum with temperatures in the range 3-8 MeV.…”

Section: B Atmospheric Neutrinosmentioning

confidence: 99%

Readout strategies for directional dark matter detection beyond the neutrino background

et al. 2015

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The search for weakly interacting massive particles (WIMPs) by direct detection faces an encroaching background due to coherent neutrino-nucleus scattering. As the sensitivity of these experiments improves, the question of how to best distinguish a dark matter signal from neutrinos will become increasingly important. A proposed method of overcoming this so-called "neutrino floor" is to utilize the directional signature that both neutrino and dark matter induced recoils possess. We show that directional experiments can indeed probe WIMP-nucleon cross-sections below the neutrino floor with little loss in sensitivity due to the neutrino background. In particular we find at low WIMP masses (around 6 GeV) the discovery limits for directional detectors penetrate below the non-directional limit by several orders of magnitude. For high WIMP masses (around 100 GeV), the non-directional limit is overcome by a factor of a few. Furthermore we show that even for directional detectors which can only measure 1-or 2-dimensional projections of the 3-dimensional recoil track, the discovery potential is only reduced by a factor of 3 at most. We also demonstrate that while the experimental limitations of directional detectors, such as sense recognition and finite angular resolution, have a detrimental effect on the discovery limits, it is still possible to overcome the ultimate neutrino background faced by non-directional detectors.PACS numbers: 95.35.+d; 95.85.Pw

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The Diffuse Supernova Neutrino Background

Cited by 293 publications

References 119 publications

A comparison between star formation rate diagnostics and rate of core collapse supernovae within 11 Mpc

A comparison between star formation rate diagnostics and rate of core collapse supernovae within 11 Mpc

Supernova relic neutrino search at super-Kamiokande

Readout strategies for directional dark matter detection beyond the neutrino background

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