Cosmic Supernova Neutrino and Gamma-Ray Backgrounds in the MeV Regime

Abstract

Cosmic multimessenger backgrounds include relic diffuse components created in the early universe and contributions from individual sources. Here, we study both type Ia supernovae (SNe Ia) and core-collapse supernovae (CCSNe) contributions to the diffuse neutrino and gamma-ray backgrounds in the MeV regime referred to as DSNB and DSGB respectively. We show that the diffuse SN Ia background is 106 times lower (for ν ¯ e ) than the CCSN background making it negligible. Our predicted DSNB ν ¯ e flux at earth in the 19.3–32 MeV regime is 0.36 ν cm−2 s−1. We also find that the DSNB flux in the energy range from 11.3 to 32 MeV varies by +29% with a change in the SFRD model from Madau & Fragos which yielded a minimum predicted flux, to the extragalactic background light reconstruction model (maximum predicted flux). The diffuse SN Ia gamma-ray background and its dependence on the progenitor supernova delay time distribution are also evaluated. Furthermore, we address the origin of the CGB (Cosmic Gamma-ray Background) in the 0.1–7 MeV regime by adding contributions from sources such as SNe Ia, CCSNe, radio-quiet Active Galactic Nuclei, Flat spectrum radio quasars (FSRQs) and Neutron star—neutron star mergers. We find that our modeled background (including uncertainties) matches the observed CGB above 1.0 MeV, but is a factor ≈2 lower than the observed flux in the 0.1–1.0 MeV range, highlighting the need for future MeV missions to establish the CGB spectrum more reliably, and to possibly identify additional sources or even source classes in the underexplored MeV band.

Contribution of Neutrino-dominated Accretion Flows to the Cosmic MeV Neutrino Background

“…Until now, the most studied contribution to the CMNB has been the diffuse SN neutrino background (DSNB). Over the years, the predictions of the DSNB have improved steadily (see, e.g., Horiuchi et al 2009Horiuchi et al , 2018Horiuchi et al , 2021Lunardini 2009;Galais et al 2010;Nakazato 2013;Nakazato et al 2015;Yüksel & Kistler 2015;Møller et al 2018;Abe et al 2021;Kresse et al 2021;Li et al 2021;Tabrizi & Horiuchi 2021;Ashida & Nakazato 2022;de Gouvêa et al 2022;Ekanger et al 2022Ekanger et al , 2024Libanov & Sharofeev 2022;Anandagoda et al 2023;Ashida et al 2023); and for the related reviews, see Ando & Sato (2004), Beacom (2010), Lunardini (2016), Vitagliano et al (2020), andSuliga (2022). Compared to the DSNB, very few works focus on the DNNB.…”

Diffuse Neutrino Flux Based on the Rates of Core-collapse Supernovae and Black Hole Formation Deduced from a Novel Galactic Chemical Evolution Model

“…In particular, neutrinos from the core collapse of massive stars over cosmic history have accumulated to form the diffuse supernova neutrino background (DSNB), or they are referred to as supernova relic neutrinos, and they are expected to provide knowledge of not only collapsing stars, but also cosmic chemical evolution, etc. Impacts of physical and astrophysical factors on the DSNB have been studied actively in many theoretical works (e.g., Totani & Sato 1995;Totani et al 1996;Hartmann & Woosley 1997;Malaney 1997;Kaplinghat et al 2000;Ando et al 2003;Horiuchi et al 2009Horiuchi et al , 2018Horiuchi et al , 2021Lunardini 2009;Galais et al 2010;Nakazato 2013;Nakazato et al 2015;Mathews et al 2020;Kresse et al 2021;Tabrizi & Horiuchi 2021;Ashida & Nakazato 2022;Ekanger et al 2022;Ziegler et al 2022;Anandagoda et al 2023;Aoyama et al 2023). In the experimental field, an observation of the DSNB flux has yet to be accomplished; however, a recent search at the Super-Kamiokande (SK) water Cherenkov detector has excluded some optimistic models and placed upper bounds on the DSNB e n ¯flux close to many theoretical predictions, within a factor of 10 (Abe et al 2021).…”

Stellar Neutrino Emission across the Mass–Metallicity Plane

“…Ongoing stellar neutrino searches aim to detect pre-supernova neutrinos, which allow new tests of stellar and neutrino physics (e.g., Brocato et al 1998;Odrzywolek et al 2004;Kutschera et al 2009;Odrzywolek 2009;Patton et al 2017aPatton et al , 2017bKato et al 2017Kato et al , 2020aYusof et al 2021;Kosmas et al 2022) and enable an early alert of an impending CC supernova to the electromagnetic and gravitational-wave communities Mukhopadhyay et al 2020;Al Kharusi et al 2021). They also aim to explore the diffuse supernova neutrino background (Bisnovatyi-Kogan & Seidov 1984;Krauss et al 1984;Hartmann & Woosley 1997;Ando & Sato 2004;Porciani et al 2004;Horiuchi et al 2009;Beacom 2010;Anandagoda et al 2020;Suliga 2022;Anandagoda et al 2023) and neutrinos from the helium-core nitrogen flash (Serenelli & Fukugita 2005), compact object mergers (Kyutoku & Kashiyama 2018;Lin & Lunardini 2020), tidal disruptions of stars (Lunardini & Winter 2017;Reusch et al 2022;Winter & Lunardini 2023), and pulsational pair-instability supernovae (Leung et al 2020). Farag et al (2020) introduced the idea of a neutrino Hertzsprung-Russell diagram (νHRD) with a sparse grid of models.…”