The 50–100 pc scale parent stellar populations of Type II supernovae and limitations of single star evolution models

Schady, P.; Eldridge, J. J.; Anderson, J. P.; Chen, Ting-Wan; Galbany, L.; Kuncarayakti, H.; Xiao, Lin

doi:10.1093/mnras/stz2843

Cited by 18 publications

(25 citation statements)

References 126 publications

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“…However, other observational studies have suggested that the upper mass limit for SN-II progenitors should be considerably lower (e.g. Smartt 2015;Davies & Beasor 2018;Schady et al 2019), and other chemical evolution models have been successful in reproducing Milky Way constraints without requiring enrichment from stars above ∼ 25 − 50 M (e.g. Kobayashi & Nakasato 2011;Côté et al 2017).…”

Section: A Reduced Maximum Sn-ii Progenitor Massmentioning

confidence: 99%

L-GALAXIES 2020: The evolution of radial metallicity profiles and global metallicities in disc galaxies

Yates

Henriques

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a modified version of the L-Galaxies 2020 semi-analytic model of galaxy evolution, which includes significantly increased direct metal enrichment of the circumgalactic medium (CGM) by supernovae (SNe). These more metal-rich outflows do not require increased mass-loading factors, in contrast to some other galaxy evolution models. This modified L-Galaxies 2020 model is able to simultaneously reproduce the gas-phase metallicity (Zg) and stellar metallicity (Z*) radial profiles observed in nearby disc galaxies by MaNGA and MUSE, as well as the observed mass – metallicity relations for gas and stars at z = 0 and their evolution back to z ∼ 2 − 3. A direct CGM enrichment fraction of ∼90 per cent for SNe-II is preferred. We find that massive disc galaxies have slightly flatter Zg profiles than their lower-mass counterparts in L-Galaxies 2020, due to more efficient enrichment of their outskirts via inside-out growth and metal-rich accretion. Such a weak, positive correlation between stellar mass and Zg profile slope is also seen in our MaNGA-DR15 sample of 571 star-forming disc galaxies, although below ${\rm log}_{10}{(M_{*}/{\rm M_\odot} )}{}\sim {}10.0$ this observational result is strongly dependent on the metallicity diagnostic and morphological selection chosen. In addition, a lowered maximum SN-II progenitor mass of 25 M⊙, reflecting recent theoretical and observational estimates, can also provide a good match to observed Zg and Z* profiles at z = 0 in L-Galaxies 2020. However, this model version fails to reproduce an evolution in Zg at fixed mass over cosmic time, or the magnesium abundances observed in the intracluster medium (ICM).

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Section: A Reduced Maximum Sn-ii Progenitor Massmentioning

confidence: 99%

L-GALAXIES 2020: The evolution of radial metallicity profiles and global metallicities in disc galaxies

Yates

Henriques

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…For nearby, spatially resolved galaxies, especially those for which integral field spectroscopy (IFS) observations are available, local properties can provide an extra channel from which to inform the host study (e.g. Thöne et al 2014;Krühler et al 2017a;Galbany et al 2018;Schady et al 2019). Local properties are typically analogues of the global properties, but are derived from a region smaller than the entire host galaxy, and are used to provide a more accurate representation of the properties of the particular stellar population from which the progenitor was born (e.g.…”

Section: Introductionmentioning

confidence: 99%

Supernova host galaxies in the dark energy survey: I. Deep coadds, photometry, and stellar masses

Wiseman¹,

Smith²,

Childress³

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The 5-yr Dark Energy Survey Supernova Programme (DES-SN) is one of the largest and deepest transient surveys to date in terms of volume and number of supernovae. Identifying and characterizing the host galaxies of transients plays a key role in their classification, the study of their formation mechanisms, and the cosmological analyses. To derive accurate host galaxy properties, we create depth-optimized coadds using single-epoch DES-SN images that are selected based on sky and atmospheric conditions. For each of the five DES-SN seasons, a separate coadd is made from the other four seasons such that each SN has a corresponding deep coadd with no contaminating SN emission. The coadds reach limiting magnitudes of order ∼27 in g band, and have a much smaller magnitude uncertainty than the previous DES-SN host templates, particularly for faint objects. We present the resulting multiband photometry of host galaxies for samples of spectroscopically confirmed type Ia (SNe Ia), core-collapse (CCSNe), and superluminous (SLSNe) as well as rapidly evolving transients (RETs) discovered by DES-SN. We derive host galaxy stellar masses and probabilistically compare stellar-mass distributions to samples from other surveys. We find that the DES spectroscopically confirmed sample of SNe Ia selects preferentially fewer high-mass hosts at high-redshift compared to other surveys, while at low redshift the distributions are consistent. DES CCSNe and SLSNe hosts are similar to other samples, while RET hosts are unlike the hosts of any other transients, although these differences have not been disentangled from selection effects.

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“…As the local rate of SNe is low, the same technique has been used for SN remnants too (Maoz & Badenes 2010;Jennings et al 2014;Maund 2017;Díaz-Rodríguez et al 2018;Auchettl et al 2019). Several other studies investigate the association of SN II with star-forming regions, through observations of nebular emission lines of the SN environment (e.g., Anderson et al 2012;Habergham et al 2014;Xiao et al 2018;Kuncarayakti et al 2018;Schady et al 2019), thus also providing an estimate of the initial mass of the progenitor star. This technique has been also used to other stellar objects, like Luminous Blue Variables that may be progenitors of type IIn SNe.…”

Section: Predicted Discrepancy Of Inferred Initial Masses Of Type II Sn Progenitors Between Different Observational Methodsmentioning

confidence: 99%

“…Part of the sample has been presented in Schady et al (2019), where they used Hα emission lines in the surrounding region as an age tracer. They show that this method is highly sensitive to the modeling of the stellar environment, because binary prod- Notes.…”

Section: Predicted Discrepancy Of Inferred Initial Masses Of Type II Sn Progenitors Between Different Observational Methodsmentioning

confidence: 99%

“…They show that this method is highly sensitive to the modeling of the stellar environment, because binary prod- Notes. (a) Hα emission by Schady et al (2019), similar value to Kuncarayakti et al (2018). Should be considered not valid according to Schady et al (2019), thus are not shown in Fig.…”

Section: Predicted Discrepancy Of Inferred Initial Masses Of Type II Sn Progenitors Between Different Observational Methodsmentioning

confidence: 99%

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Effect of binary evolution on the inferred initial and final core masses of hydrogen-rich, Type II supernova progenitors

Zapartas

Mink

Justham

et al. 2020

A&A

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The majority of massive stars, which are the progenitors of core-collapse supernovae (SNe), are found in close binary systems. In a previous work, we modeled the fraction of hydrogen-rich, Type II SN progenitors whose evolution is affected by mass exchange with their companion, finding this to be between ≈1/3 and 1/2 for most assumptions. Here we study in more depth the impact of this binary history of Type II SN progenitors on their final pre-SN core mass distribution, using population synthesis simulations. We find that binary star progenitors of Type II SNe typically end their life with a larger core mass than they would have had if they had lived in isolation because they gained mass or merged with a companion before their explosion. The combination of the diverse binary evolutionary paths typically leads to a marginally shallower final core mass distribution. In discussing our results in the context of the red supergiant problem, that is, the reported lack of detected high luminosity progenitors, we conclude that binary evolution does not seem to significantly affect the issue. This conclusion is quite robust against our variations in the assumptions of binary physics. We also predict that inferring the initial masses of Type II SN progenitors by “age-dating” their surrounding environment systematically yields lower masses compared to methods that probe the pre-SN core mass or luminosity. A robust discrepancy between the inferred initial masses of a SN progenitor from those different techniques could indicate an evolutionary history of binary mass accretion or merging.

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The 50–100 pc scale parent stellar populations of Type II supernovae and limitations of single star evolution models

Cited by 18 publications

References 126 publications

L-GALAXIES 2020: The evolution of radial metallicity profiles and global metallicities in disc galaxies

L-GALAXIES 2020: The evolution of radial metallicity profiles and global metallicities in disc galaxies

Supernova host galaxies in the dark energy survey: I. Deep coadds, photometry, and stellar masses

Effect of binary evolution on the inferred initial and final core masses of hydrogen-rich, Type II supernova progenitors

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