Extreme Mass Loss in Low-mass Type Ib/c Supernova Progenitors

Wu, Samantha; Fuller, Jim

doi:10.3847/2041-8213/ac9b3d

Cited by 16 publications

(14 citation statements)

References 47 publications

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“…The progenitors of stripped-envelope SNe could either be stripped by binary partners, or they could be very massive stars with strong winds, and progenitor detections in several bands might allow us to distinguish between these two scenarios. Wu & Fuller (2022) predict that late nuclear burning stages trigger mass loss and brightening for stripped stars. Such events would boost the detection rate for these progenitors and offer direct information about the processes in their stellar cores.…”

Section: Discussionmentioning

confidence: 99%

Search for Supernova Progenitor Stars with ZTF and LSST

Strotjohann,

Ofek,

Gal-Yam

et al. 2023

ApJ

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The direct detection of core-collapse supernova (SN) progenitor stars is a powerful way of probing the last stages of stellar evolution. However, detections in archival Hubble Space Telescope images are limited to about one detection per year. Here, we explore whether we can increase the detection rate by using data from ground-based wide-field surveys. Due to crowding and atmospheric blurring, progenitor stars can typically not be identified in preexplosion images alone. Instead, we combine many pre-SN and late-time images to search for the disappearance of the progenitor star. As a proof of concept, we implement our search of ZTF data. For a few hundred images, we achieve limiting magnitudes of ∼23 mag in the g and r bands. However, no progenitor stars or long-lived outbursts are detected for 29 SNe within z ≤ 0.01, and the ZTF limits are typically several magnitudes less constraining than detected progenitors in the literature. Next, we estimate progenitor detection rates for the Legacy Survey of Space and Time (LSST) with the Vera C. Rubin telescope by simulating a population of nearby SNe. The background from bright host galaxies reduces the nominal LSST sensitivity by, on average, 0.4 mag. Over the 10 yr survey, we expect the detection of ∼50 red supergiant progenitors and several yellow and blue supergiants. The progenitors of Type Ib and Ic SNe will be detectable if they are brighter than −4.7 or −4.0 mag in the LSST i band, respectively. In addition, we expect the detection of hundreds of pre-SN outbursts depending on their brightness and duration.

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Section: Discussionmentioning

confidence: 99%

Search for Supernova Progenitor Stars with ZTF and LSST

Strotjohann,

Ofek,

Gal-Yam

et al. 2023

ApJ

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show abstract

“…Tauris et al (2015) found that the maximum mass-loss rate of ultra-stripped helium stars in binary systems is close to ∼10 −4 M e yr −1 . More recently, Wu & Fuller (2022) found that mass loss with rates of    --M M 10 yr 4 1 could last for ∼10 4 yr until core collapses of close-binary low-mass helium stars, while extreme mass loss…”

Section: Methodsmentioning

confidence: 99%

A Population Study of the Radio Emission of Fast Blue Optical Transients

Liu

et al. 2023

ApJ

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Despite the fact that the progenitor of fast blue optical transients (FBOTs) is still a subject of debate, FBOTs are sometimes suggested to originate from the core collapse of ultra-stripped stars and be powered by a spinning-down neutron star. Following this consideration, it is expected that the late-time evolution of the progenitor stars can leave important imprints in the circumstellar material (CSM) of FBOTs, due to the strong mass loss of the stars. The interaction of the FBOT ejecta with the CSM can drive a long-lasting shock to generate radio emission, which thus enables us to probe the CSM properties through radio observation although such observations are still rare. Within the framework of the magnetar-powered model, Liu et al. fitted the multi-band optical light curves of 40 FBOTs, and hence, the statistical distributions of the FBOT magnetar and ejecta parameters were obtained. Based on these FBOT population results, we investigate the dependence of the radio emission on the mass-loss rate of the progenitors and evaluate the detectability of radio emission from FBOTs with current and future telescopes. It is found that the distribution of the peak time and peak luminosity of the emission at 8.4 GHz are primarily in the regions of t peak,ν = 102.12±0.63 days and L peak,ν = 1028.73±0.83 erg s−1 Hz−1, respectively. A joint detection of the Zwicky Transient Facility and Very Large Array could achieve success in about 8.7% FBOTs of z ≤ 1. Furthermore, if considering a joint detection of the Chinese Space Station Telescope and the Square Kilometer Array, this rate of success could be increased to about 23.9%.

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“…For a comprehensive introduction on the stellar massloss, please see the review by Smith (2014). Tauris et al (2015) found that the maximum mass-loss rate of ultra-stripped helium stars in binary systems is close to ∼ 10 −4 M yr −1 .More recently, Wu & Fuller (2022) found that mass loss with rates of Ṁ 10 −4 M yr −1 could last for ∼ 10 4 yrs until core collapses of closebinary low-mass helium stars, while extreme mass loss ( Ṁ 10 −2 M yr −1 ) could possibly occur beginning weeks to decades before SN explosions. The CSM interaction of such winds from ultra-stripped stars in binary systems is supposed to be very complicated.…”

Section: Methodsmentioning

confidence: 99%

A Population Study on the Radio Emission of Fast Blue Optical Transients

Liu¹,

Liu²,

Yu³

et al. 2023

Preprint

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Despite the fact that the progenitor of fast blue optical transients (FBOTs) is still up for debate, FBOTs are sometimes suggested to originate from the core-collapse of ultra-stripped stars and be powered by a spinning-down neutron star. Following this consideration, it is expected that the latetime evolution of the progenitor stars can leave important imprints in the circumstellar material (CSM) of the FBOTs, due to the strong mass loss of the stars. The interaction of the FBOT ejecta with the CSM can drive a long-lasting shock to generate radio emission, which thus enables us to probe the CSM properties through radio observation although such observations are still rare. Within the framework of the magnetar-powered model, Liu et al. ( 2022) fitted the multi-band optical light curves of 40 FBOTs and, hence, the statistical distributions of the FBOT magnetar and ejecta parameters were obtained. Based on these FBOT population results, we investigate the dependence of the radio emission on the mass-loss rate of the progenitors and evaluate the detectability of radio emission from FBOTs with current and future telescopes. It is found that the distribution of the peak time and peak luminosity of the emission at 8.4 GHz are primarily in the regions of t peak,ν = 10 2.12±0.63 days and L peak,ν = 10 28.73±0.83 erg s −1 Hz −1 , respectively. A joint detection of the Zwicky Transient Facility and Very Large Array could achieve success in about 8.7% FBOTs of z ≤ 1. Furthermore, if considering a joint observation of the Chinese Space Station Telescope and Square Kilometer Array, this fraction can be increased to about 23.9%.

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Extreme Mass Loss in Low-mass Type Ib/c Supernova Progenitors

Cited by 16 publications

References 47 publications

Search for Supernova Progenitor Stars with ZTF and LSST

Search for Supernova Progenitor Stars with ZTF and LSST

A Population Study of the Radio Emission of Fast Blue Optical Transients

A Population Study on the Radio Emission of Fast Blue Optical Transients

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