No velocity-kicks are required to explain large-distance offsets of Ca-rich supernovae and short-GRBs

Perets, Hagai B.; Beniamini, Paz

doi:10.1093/mnras/stab794

Cited by 21 publications

(18 citation statements)

References 65 publications

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“…An independent constraint comes from short GRBs. The offset distribution of those GRBs relative to the centers of their host galaxies is found to be fully consistent with the underlying distribution of stellar material in the host galaxies (Perets & Beniamini 2021). This strongly suggests that the effects of kicks are subdominant in determining the merger locations of BNS.…”

Section: Conclusion and Discussionsupporting

confidence: 59%

Evidence for r-process Delay in Very Metal-poor Stars

Tarumi

Hotokezaka²,

Beniamini³

2021

ApJL

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The abundances of r-process elements of very metal-poor stars capture the history of the r-process enrichment in the early stage of star formation in a galaxy. Currently, various types of astrophysical sites including neutron star mergers (NSMs), magneto-rotational supernovae, and collapsars, are suggested as the origin of r-process elements. The time delay between the star formation and the production of r-process elements is the key to distinguish these scenarios, with the caveat that the diffusion of r-process elements in the interstellar medium may induce the delay in r-process enrichment because r-process events are rare. Here we study the observed Ba abundance data of very metal-poor stars as the tracer of the early enrichment history of r-process elements. We find that the gradual increase of [Ba/Mg] with [Fe/H], which is remarkably similar among the Milky Way and classical dwarfs, Requires a significant time delay (100 Myr-1 Gyr) of r-process events from star formation rather than the diffusion-induced delay. We stress that this conclusion is robust to the assumption regarding s-process contamination in the Ba abundances because the sources with no delay would overproduce Ba at very low metallicities, even without the contribution from the s-process. Therefore, we conclude that sources with a delay, possibly NSMs, are the origins of r-process elements.

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Section: Conclusion and Discussionsupporting

confidence: 59%

Evidence for r-process Delay in Very Metal-poor Stars

Tarumi

Hotokezaka²,

Beniamini³

2021

ApJL

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“…They were initially classified into Type Ib SNe because of the strong He features in their optical spectra but were later found to have different characteristics of low luminosity, fast temporal evolution, large Ca to O line ratios in nebular phase, and show a tendency to occur in the outskirts of galaxies. Such large offsets have been explained by in situ low-mass stars or runaway binary mergers (but see Perets & Beniamini 2021). This group of SNe was first called Ca-rich gap transients because its luminosity lies in the gap between novae and ordinary SNe (Kasliwal et al 2012;Taubenberger 2017).…”

Section: Introductionmentioning

confidence: 99%

Spatially Resolved X-Ray Study of Supernova Remnant G306.3–0.9 with Unusually High Calcium Abundance

Weng

Zhou

Chen

et al. 2022

ApJ

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G306.3–0.9 is an asymmetric Galactic supernova remnant (SNR), whose progenitor has been thought to be a Type Ia supernova (SN), but its high Ca abundance appears inconsistent with the Type Ia origin. Hoping to uncover the reason for its asymmetry and the origin of this SNR, we performed a spatially resolved X-ray spectroscopic analysis of XMM-Newton and Chandra observation data. We divided the SNR into 13 regions and analyzed the spectra using two-temperature models (0.2 keV + 1 keV). Compared to the southwestern regions, the northeastern regions have higher metal abundances and a lower gas density. This suggests that the asymmetric morphology results from the nonuniform ambient environment. We found that neither Type Ia nor core-collapse SN models can account for the abnormally high abundance ratios of Ar/Si, Ca/Si, or the shape of the abundance curve. A comparison with the Ca-rich transient models suggests that G306.3–0.9 is likely to be the first identified Galactic Ca-rich transient remnant, although the theoretical production of element S is lower. We also note that the conclusion for the SNR’s origin relies on the measured abundance ratios and existing nucleosynthesis models. Between two groups of Ca-rich transient explosion models, we prefer the He shell detonation for an accreting white dwarf, rather than the merger of a white dwarf and a neutron star.

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“…To date, there has been considerable effort to constrain potential progenitor systems of Ca-rich transients using host galaxy information (see, e.g., Yuan et al 2013;Lunnan et al 2017a;Shen et al 2019;Perets & Beniamini 2021). Here we further these efforts by presenting a comprehensive analysis of the host galaxies of all reported and suspected Ca-rich transients using publicly available photometry and the parametric and nonparametric models in the advanced stellar inference Python package prospector (Leja et al 2017;Johnson et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Physical Properties of the Host Galaxies of Ca-rich Transients

Dong,

Milisavljevic,

Leja

et al. 2022

Preprint

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Calcium-rich (Ca-rich) transients are a new class of supernovae (SNe) that are known for their comparatively rapid evolution, modest peak luminosities, and strong nebular calcium emission lines. Currently, the progenitor systems of Ca-rich transients remain unknown. Although they exhibit spectroscopic properties not unlike core-collapse Type Ib/c SNe, nearly half are found in the outskirts of their host galaxies that are predominantly elliptical, suggesting a closer connection to the older stellar populations of SNe Ia. In this paper, we present a compilation of publicly available multiwavelength observations of all known and/or suspected host galaxies of Ca-rich transients ranging from FUV to IR, and use these data to characterize their stellar populations with prospector. We estimate several galaxy parameters including integrated star formation rate, stellar mass, metallicity, and age. For nine host galaxies, the observations are sensitive enough to obtain nonparametric star formation histories, from which we recover SN rates and estimate probabilities that the Ca-rich transients in each of these host galaxies originated from a core-collapse vs. Type Ia-like explosion. Our work supports the notion that the population of Ca-rich transients do not come exclusively from core-collapse explosions, and must either be only from white dwarf stars or a mixed population of white dwarf stars with other channels, potentially including massive star explosions. Additional photometry and explosion site spectroscopy of larger samples of Ca-rich host galaxies will improve these estimates and better constrain the ratio of white dwarf vs. massive star progenitors of Ca-rich transients.

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No velocity-kicks are required to explain large-distance offsets of Ca-rich supernovae and short-GRBs

Cited by 21 publications

References 65 publications

Evidence for r-process Delay in Very Metal-poor Stars

Evidence for r-process Delay in Very Metal-poor Stars

Spatially Resolved X-Ray Study of Supernova Remnant G306.3–0.9 with Unusually High Calcium Abundance

Physical Properties of the Host Galaxies of Ca-rich Transients

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