Review of uncertainties in the cosmic supernova relic neutrino background

Mathews, Grant J.; Boccioli, Luca; Hidaka, Jun; Kajino, Toshitaka

doi:10.1142/s0217732320300116

Cited by 12 publications

(9 citation statements)

References 86 publications

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“…6 The neutrino fluxes from CCSNe can be changed by assumptions that include an approximation of gas motions around the progenitor core and a choice of the equation of state. 7 A systematic uncertainty of the neutrino flux raised by the assumptions is estimated to be ∼50% (private communications with K. Kotake; see also Mathews et al 2020). We include the systematic uncertainty in our model calculations, and show the contours of the forecast in Figure 5.…”

Section: Neutrino Fluxes Measured In the Futurementioning

confidence: 97%

Stellar Initial Mass Function (IMF) Probed with Supernova Rates and Neutrino Background: Cosmic-average IMF Slope Is ≃2–3 Similar to the Salpeter IMF

Aoyama

Ouchi

Harikane

2023

ApJ

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The stellar initial mass function (IMF) is expressed by ϕ(m) ∝ m − α with the slope α, and known as a poorly constrained but very important function in studies of star and galaxy formation. There are no sensible observational constraints on the IMF slopes beyond the Milky Way and nearby galaxies. Here we combine two sets of observational results, (1) cosmic densities of core-collapse supernova (CCSN) explosion rates and (2) cosmic far-UV radiation (and infrared reradiation) densities, which are sensitive to massive (≃8–50 M ⊙) and moderately massive (≃2.5–7 M ⊙) stars, respectively, and constrain the IMF slope at m > 1 M ⊙ with a freedom of redshift evolution. Although no redshift evolution is identified beyond the uncertainties, we find that the cosmic-average IMF slope at z = 0 is α = 1.8–3.2 at the 95% confidence level that is comparable with the Salpeter IMF, α = 2.35, which marks the first constraint on the cosmic-average IMF. We show a forecast for the Nancy Grace Roman Space Telescope supernova survey that will provide significantly strong constraints on the IMF slope with δ α ≃ 0.5 over z = 0–2. Moreover, as for an independent IMF probe instead of (1), we suggest to use diffuse supernovae neutrino background (DSNB), relic neutrinos from CCSNe. We expect that the Hyper-Kamiokande neutrino observations over 20 yr will improve the constraints on the IMF slope and the redshift evolution significantly better than those obtained today, if the systematic uncertainties of DSNB production physics are reduced in the future numerical simulations.

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Section: Neutrino Fluxes Measured In the Futurementioning

confidence: 97%

Stellar Initial Mass Function (IMF) Probed with Supernova Rates and Neutrino Background: Cosmic-average IMF Slope Is ≃2–3 Similar to the Salpeter IMF

Aoyama

Ouchi

Harikane

2023

ApJ

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“…In the case of the failed SN, the time-integrated neutrino spectrum depends on the maximum mass of the proto-NS because neutrinos are emitted until a BH formation (Sumiyoshi et al 2006). In the previous studies (Lunardini 2009;Nakazato et al 2015;Mathews et al 2020), the EOS dependence is taken into account only for the component of the failed SN. In the present study, we also consider the EOS dependence for the SN with a NS.…”

Section: Formulation Of the Srn Fluxmentioning

confidence: 99%

Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos

Ashida¹,

Nakazato

2022

ApJ

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Core collapse of massive stars leads to different fates for various physical factors, which gives different spectra of the emitted neutrinos. We focus on the supernova relic neutrinos (SRNs) as a probe to investigate the stellar collapse fate. We present the SRN fluxes and event rate spectra at a detector for three resultant states after stellar core collapse, the typical mass neutron star, the higher mass neutron star, or the failed supernova forming a black hole, based on different nuclear equations of state. Then possible SRN fluxes are formed as mixtures of the three components. We also show the expected sensitivities at the next-generation water-based Cherenkov detectors, SK-Gd and Hyper-Kamiokande, as constraining the mixture fractions. This study provides a practical example of extracting astrophysical constraints through SRN measurement.

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“…The neutrino fluxes from CCSNe can be changed by assumptions that include an approximation of gas motions around the progenitor core and a choice of the equation of state 3 . A systematic uncertainty of the neutrino flux raised by the assumptions is estimated to be ∼ 50% (private communications with K. Kotake, see also Mathews et al (2020)). We include the systematic uncertainty into our model calculations, and show the contours of the forecast in Figure 5.…”

Section: Neutrino Fluxes Measured In the Futurementioning

confidence: 99%

Stellar Initial Mass Function (IMF) Probed with Supernova Rates and Neutrino Background: Cosmic Average IMF Slope is $\simeq 2-3$ Similar to the Salpeter IMF

Aoyama¹,

Ouchi²,

Harikane³

2021

Preprint

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The stellar initial mass function (IMF) is expressed by φ(m) ∝ m −α with the slope α, and known as the poorly-constrained but very important function in studies of star and galaxy formation. There are no sensible observational constraints on the IMF slopes beyond Milky Way and nearby galaxies. Here we combine two sets of observational results, 1) cosmic densities of core-collapse supernova explosion (CCSNe) rates and 2) cosmic far ultraviolet radiation (and infrared re-radiation) densities, which are sensitive to massive (≃ 8 − 50 M ⊙ ) and moderately massive (≃ 2.5 − 7 M ⊙ ) stars, respectively, and constrain the IMF slope at m > 1 M ⊙ with a freedom of redshift evolution. Although no redshift evolution is identified beyond the uncertainties, we find that the cosmic average IMF slope at z = 0 is α = 1.8 − 3.2 at the 95% confidence level that is comparable with the Salpeter IMF, α = 2.35, which marks the first constraint on the cosmic average IMF. We show a forecast for the Nancy Grace Roman Space Telescope supernova survey that will provide significantly strong constraints on the IMF slope with δα ≃ 0.5 over z = 0 − 2. Moreover, as for an independent IMF probe instead of 1), we suggest to use diffuse supernovae neutrino background (DSNB), relic neutrinos from CCSNe. We expect that the Hyper-Kamiokande neutrino observations over 20 years will improve the constraints on the IMF slope and the redshift evolution significantly better than those obtained today, if the systematic uncertainties of DSNB production physics are reduced in the future numerical simulations.

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Review of uncertainties in the cosmic supernova relic neutrino background

Cited by 12 publications

References 86 publications

Stellar Initial Mass Function (IMF) Probed with Supernova Rates and Neutrino Background: Cosmic-average IMF Slope Is ≃2–3 Similar to the Salpeter IMF

Stellar Initial Mass Function (IMF) Probed with Supernova Rates and Neutrino Background: Cosmic-average IMF Slope Is ≃2–3 Similar to the Salpeter IMF

Exploring the Fate of Stellar Core Collapse with Supernova Relic Neutrinos

Stellar Initial Mass Function (IMF) Probed with Supernova Rates and Neutrino Background: Cosmic Average IMF Slope is $\simeq 2-3$ Similar to the Salpeter IMF

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