Relative frequencies of supernovae types: dependence on host galaxy magnitude, galactocentric radius, and local metallicity

Boissier, S.; Prantzos, Nikos

doi:10.1051/0004-6361/200811234

Cited by 81 publications

(130 citation statements)

References 46 publications

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“…The ratio of Type Ia to CC SNe in our sample is 0.44 +0.04 −0.03 , which is close to 0.40 ± 0.04 in Boissier & Prantzos (2009) and 0.40 ± 0.08 obtained from the local SNe sample of Smartt et al (2009). The N Ibc /NII ratio in our study is 0.36 +0.04 −0.03 , which is similar to 0.31 ± 0.04 in Boissier & Prantzos (2009) …”

Section: Resultssupporting

confidence: 87%

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Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Hakobyan¹,

Nazaryan²,

Adibekyan³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the relative frequencies of different supernova (SN) types in spirals with various morphologies and in barred or unbarred galaxies. We use a well-defined and homogeneous sample of spiral host galaxies of 692 SNe from the Sloan Digital Sky Survey in different stages of galaxy-galaxy interaction and activity classes of nucleus. We propose that the underlying mechanisms shaping the number ratios of SNe types can be interpreted within the framework of interaction-induced star formation, in addition to the known relations between morphologies and stellar populations. We find a strong trend in behaviour of the N Ia /N CC ratio depending on host morphology, such that early spirals include more Type Ia SNe. The N Ibc /N II ratio is higher in a broad bin of early-type hosts. The N Ia /N CC ratio is nearly constant when changing from normal, perturbed to interacting galaxies, then declines in merging galaxies, whereas it jumps to the highest value in post-merging/remnant galaxies. In contrast, the N Ibc /N II ratio jumps to the highest value in merging galaxies and slightly declines in post-merging/remnant subsample. The interpretation is that the star formation rates and morphologies of galaxies, which are strongly affected in the final stages of interaction, have an impact on the number ratios of SNe types. The N Ia /N CC (N Ibc /N II ) ratio increases (decreases) from star-forming to active galactic nuclei (AGN) classes of galaxies. These variations are consistent with the scenario of an interaction-triggered starburst evolving into AGN during the later stages of interaction, accompanied with the change of star formation and transformation of the galaxy morphology into an earlier type.

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Section: Resultssupporting

confidence: 87%

“…The result is in agreement with that of Boissier & Prantzos (2009). However, in both cases, the differences are not significant.…”

Section: Dependence Of Relative Frequencies Of Sne Types On Host Morpsupporting

confidence: 90%

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Hakobyan¹,

Nazaryan²,

Adibekyan³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…At solar metallicity, in case 1, the present models give ratios well within the range of the observed values determined by Boissier & Prantzos (2009). Indeed, one sees that the present single-star models may explain the greatest part of the observed number of Type Ibc (normalised to the number of Type II SNe).…”

Section: Comparisons With Observationssupporting

confidence: 85%

Grids of stellar models with rotation

Georgy

Ekström

Meynet

et al. 2012

A&A

305

364

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Context. In recent years, many very interesting observations have appeared concerning the positions of Wolf-Rayet (WR) stars in the Hertzsprung-Russell diagram (HRD), the number ratios of WR stars, the nature of Type Ibc supernova (SN) progenitors, long and soft gamma ray bursts (LGRB), and the frequency of these various types of explosive events. These observations represent key constraints on massive star evolution. Aims. We study, in the framework of the single-star evolutionary scenario, how rotation modifies the evolution of a given initial mass star towards the WR phase and how it impacts the rates of Type Ibc SNe. We also discuss the initial conditions required to obtain collapsars and LGRB. Methods. We used a recent grid of stellar models computed with and without rotation to make predictions concerning the WR populations and the frequency of different types of core-collapse SNe. Current rotating models were checked to provide good fits to the following features: solar luminosity and radius at the solar age, main-sequence width, red-giant and red-supergiant (RSG) positions in the HRD, surface abundances, and rotational velocities. Results. Rotating stellar models predict that about half of the observed WR stars and at least half of the Type Ibc SNe may be produced through the single-star evolution channel. Rotation increases the duration of the WNL and WNC phases, while reducing those of the WNE and WC phases, as was already shown in previous works. Rotation increases the frequency of Type Ic SNe. The upper mass limit for Type II-P SNe is ∼19.0 M for the non rotating models and ∼16.8 M for the rotating ones. Both values agree with observations. Moreover, present rotating models provide a very good fit to the progenitor of SN 2008ax. We discuss future directions of research for further improving the agreement between the models and the observations. We conclude that the mass-loss rates in the WNL and RSG phases are probably underestimated at present. We show that up to an initial mass of 40 M , a surface magnetic field inferior to about 200 G may be sufficient to produce some braking. Much lower values are needed at the red supergiant stage. We suggest that the presence/absence of any magnetic braking effect may play a key role in questions regarding rotation rates of young pulsars and the evolution leading to LGRBs.

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“…This has already been discussed extensively in Georgy et al (2012), which determined the relative rates of the different core-collapse SN types and compared to the observational sample from Boissier & Prantzos (2009). Here we revisit this topic, given that two relatively large samples of observational core-collapse SN data have been recently released (Smith et al 2011a, hereafter S11, andEldridge et al 2013, hereafter E13).…”

Section: The Core-collapse Sn Fraction From Single Starsmentioning

confidence: 91%

Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death

Groh

Meynet

Georgy

et al. 2013

A&A

193

223

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We investigate the fundamental properties of core-collapse supernova (SN) progenitors from single stars at solar metallicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of M ini = 20−120 M with atmospheric and wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at the pre-SN stage. For models with M ini = 9−20 M , we supplement our analysis using publicly available MARCS model atmospheres of RSGs to estimate their synthetic photometry. We employ well-established observational criteria of spectroscopic classification and find that, depending on their initial mass and rotation, massive stars end their lives as red supergiants (RSG), yellow hypergiants (YHG), luminous blue variables (LBV), and Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we obtained the following types of SN progenitors:, and RSGs (9 ≤ M ini ≤ 18 M ). For non-rotating models, we found spectral types WO1-, and RSGs (9 ≤ M ini ≤ 20 M ). Our rotating models indicate that SN IIP progenitors are all RSG, SN IIL/b progenitors are 56% LBVs and 44% YHGs, SN Ib progenitors are 96% WN10-11 and 4% WOs, and SN Ic progenitors are all WO stars. We find that the most massive and luminous SN progenitors are not necessarily the brightest ones in a given filter, since this depends on their luminosity, temperature, wind density, and the way the spectral energy distribution compares to a filter bandpass. We find that SN IIP progenitors (RSGs) are bright in the RIJHK S filters and faint in the UB filters. SN IIL/b progenitors (LBVs and YHGs), and SN Ib progenitors (WNs) are relatively bright in optical/infrared filters, while SN Ic progenitors (WOs) are faint in all optical filters. We argue that SN Ib and Ic progenitors from single stars should be undetectable in the available pre-explosion images with the current magnitude limits, in agreement with observational results.

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Relative frequencies of supernovae types: dependence on host galaxy magnitude, galactocentric radius, and local metallicity

Cited by 81 publications

References 46 publications

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Grids of stellar models with rotation

Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death

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