Type II supernovae from the Carnegie Supernova Project-I

Martínez, Laureano; Bersten, Melina C.; Anderson, J. P.; Hamuy, M.; González–Gaitán, S.; Förster, F.; Orellana, M.; Stritzinger, M. D.; Phillips, M. M.; Gutiérrez, C. P.; Burns, Christopher R.; Contreras, C.; Jaeger, Thomas de; Ertini, K.; Folatelli, G.; Galbany, L.; Hoêflich, P.; Hsiao, E. Y.; Morrell, N.; Pessi, P. J.; Suntzeff, Nicholas B.

doi:10.1051/0004-6361/202142076

Cited by 34 publications

(27 citation statements)

References 164 publications

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“…Morozova et al 2018;Förster et al 2018;Eldridge et al 2019;Ricks & Dwarkadas 2019;Martinez & Bersten 2019;Martinez et al 2020;Utrobin et al 2021). Recently, Martinez et al (2022) presented results from hydrodynamical modelling to 53 SNe II, finding a maximum initial mass of 21.3 M ⊙ . A third alternative method to infer Mi is by comparing late-time spectra with nebular spectra models (e.g.…”

Section: ; O'mentioning

confidence: 99%

“…This relation depends on the stellar evolution model adopted in each work. Morozova et al (2018) and Martinez et al (2020Martinez et al ( , 2022) reported Mi values inferred by fitting hydrodynamical models to SN data. Morozova et al (2018) used multiband light-curve models generated with the SNEC code (Morozova et al 2015), while Martinez et al (2020Martinez et al ( , 2022 used bolometric light curves and expansion velocity curves calculated with the model of Bersten et al (2011).…”

Section: Comparison With Initial Masses From Modelsmentioning

confidence: 99%

“…Morozova et al (2018) and Martinez et al (2020Martinez et al ( , 2022) reported Mi values inferred by fitting hydrodynamical models to SN data. Morozova et al (2018) used multiband light-curve models generated with the SNEC code (Morozova et al 2015), while Martinez et al (2020Martinez et al ( , 2022 used bolometric light curves and expansion velocity curves calculated with the model of Bersten et al (2011). In addition, 19 SNe used in the present study have Mi estimates computed by comparing late-time spectra with spectral models generated with the SUMO code (Jerkstrand et al 2011(Jerkstrand et al , 2012.…”

Section: Comparison With Initial Masses From Modelsmentioning

confidence: 99%

“…These SNe, along with the reported µ, E host B−V , and Mi values are collected in Table 10. Morozova et al (2018), Martinez et al (2020Martinez et al ( , 2022, and the SUMO code adopted non-rotating RSGs models with solar composition and Mi between 9 and 25 M ⊙ as progenitors. Specifically, Morozova et al (2018) and the SUMO code used RSG models computed with the KEPLER code (e.g.…”

Section: Comparison With Initial Masses From Modelsmentioning

confidence: 99%

“…Specifically, Morozova et al (2018) and the SUMO code used RSG models computed with the KEPLER code (e.g. Woosley et al 2002), while Martinez et al (2020Martinez et al ( , 2022 computed RSG models using the MESA code (e.g. Farmer et al 2016).…”

Section: Comparison With Initial Masses From Modelsmentioning

confidence: 99%

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Luminosity distribution of Type II supernova progenitors

Rodríguez

2022

Preprint

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I present progenitor luminosities (L) for a sample of 112 Type II supernovae (SNe II), computed directly from progenitor photometry and the bolometric correction technique, or indirectly from empirical correlations between progenitor luminosity and [O i] λλ6300, 6364 line luminosity at 350 d since explosion, 56 Ni mass, or absolute V -band magnitude at 50 d since explosion. To calibrate these correlations, I use twelve SNe II with progenitor luminosities measured from progenitor photometry. I find that the correlations mentioned above are strong and statistically significant, and allow to estimate progenitor luminosities to a precision between 20 and 24 per cent. I correct the SN sample for selection bias and define a subsample of 112 SNe II with progenitor luminosities between log(L/L ⊙ ) = 4.6 dex, corresponding to the completeness limit of the corrected sample, and the maximum observed progenitor luminosity of log(L/L ⊙ ) = 5.091 dex. The luminosity distribution for this subsample is statistically consistent with those for red supergiants (RSGs) in LMC, SMC, M31, and M33 with 4.6 ≤ log(L/L ⊙ ) ≤ 5.091. This supports that SN II progenitors correspond to RSGs. The conspicuous absence of SN II progenitors with log(L/L ⊙ ) > 5.1 dex with respect to what is observed in RSG luminosity distributions, known as the RSG problem, is significant at a 5.2 ± 0.5 σ level.

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Section: ; O'mentioning

confidence: 99%

Section: Comparison With Initial Masses From Modelsmentioning

confidence: 99%

Section: Comparison With Initial Masses From Modelsmentioning

confidence: 99%

Section: Comparison With Initial Masses From Modelsmentioning

confidence: 99%

Section: Comparison With Initial Masses From Modelsmentioning

confidence: 99%

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Luminosity distribution of Type II supernova progenitors

Rodríguez

2022

Preprint

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Interplay between neutrino kicks and hydrodynamic kicks of neutron stars and black holes

Janka,

Kresse

2024

Astrophys Space Sci

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Neutron stars (NSs) are observed with high space velocities and elliptical orbits in binaries. The magnitude of these effects points to natal kicks that originate from asymmetries during the supernova (SN) explosions. Using a growing set of long-time 3D SN simulations with the Prometheus-Vertex code, we explore the interplay of NS kicks that are induced by asymmetric neutrino emission and by asymmetric mass ejection. Anisotropic neutrino emission can arise from a large-amplitude dipolar convection asymmetry inside the proto-NS (PNS) termed LESA (Lepton-number Emission Self-sustained Asymmetry) and from aspherical accretion downflows around the PNS, which can lead to anisotropic neutrino emission (absorption/scattering) with a neutrino-induced NS kick roughly opposite to (aligned with) the kick by asymmetric mass ejection. In massive progenitors, hydrodynamic kicks can reach up to more than 1300 km s−1, whereas our calculated neutrino kicks reach (55–140) km s−1 (estimated upper bounds of (170–265) km s−1) and only ∼(10–50) km s−1, if LESA is the main cause of asymmetric neutrino emission. Therefore, hydrodynamic NS kicks dominate in explosions of high-mass progenitors, whereas LESA-induced neutrino kicks dominate for NSs born in low-energy SNe of the lowest-mass progenitors, when these explode nearly spherically. Our models suggest that the Crab pulsar with its velocity of ∼160 km s−1, if born in the low-energy explosion of a low-mass, single-star progenitor, should have received a hydrodynamic kick in a considerably asymmetric explosion. Black holes, if formed by the collapse of short-lived PNSs and solely kicked by anisotropic neutrino emission, obtain velocities of only some km s−1.

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Type II supernovae from the Carnegie Supernova Project-I

Martínez

Anderson

Bersten

et al. 2022

A&A

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Type II supernovae (SNe II) show great photometric and spectroscopic diversity which is attributed to the varied physical characteristics of their progenitor and explosion properties. In this study, the third of a series of papers where we analyse a large sample of SNe II observed by the Carnegie Supernova Project-I, we present correlations between their observed and physical properties. Our analysis shows that explosion energy is the physical property that correlates with the highest number of parameters. We recover previously suggested relationships between the hydrogen-rich envelope mass and the plateau duration, and find that more luminous SNe II with higher expansion velocities, faster declining light curves, and higher 56 Ni masses are consistent with higher energy explosions. In addition, faster declining SNe II (usually called SNe IIL) are also compatible with more concentrated 56 Ni in the inner regions of the ejecta. Positive trends are found between the initial mass, explosion energy, and 56 Ni mass. While the explosion energy spans the full range explored with our models, the initial mass generally arises from a relatively narrow range. Observable properties were measured from our grid of bolometric LC and photospheric velocity models to determine the effect of each physical parameter on the observed SN II diversity. We argue that explosion energy is the physical parameter causing the greatest impact on SN II diversity, that is, assuming the non-rotating solar-metallicity single-star evolution as in the models used in this study. The inclusion of pre-SN models assuming higher mass loss produces a significant increase in the strength of some correlations, particularly those between the progenitor hydrogen-rich envelope mass and the plateau and optically thick phase durations. These differences clearly show the impact of having different treatments of stellar evolution, implying that changes in the assumption of standard single-star evolution are necessary for a complete understanding of SN II diversity.

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Type II supernovae from the Carnegie Supernova Project-I

Cited by 34 publications

References 164 publications

Luminosity distribution of Type II supernova progenitors

Luminosity distribution of Type II supernova progenitors

Interplay between neutrino kicks and hydrodynamic kicks of neutron stars and black holes

Type II supernovae from the Carnegie Supernova Project-I

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