Search for Supernova Progenitor Stars with ZTF and LSST

Strotjohann, Nora L.; Ofek, Eran O.; Gal-Yam, Avishay; Sollerman, Jesper; Chen, Ping; Yaron, Ofer; Zackay, Barak; Rehemtulla, Nabeel; Gris, Phillipe; Masci, Frank J.; Rusholme, Ben; Purdum, Josiah

doi:10.3847/1538-4357/ad06b6

Cited by 6 publications

(2 citation statements)

References 95 publications

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“…In the era of the Rubin Observatory (Ivezićet al 2019), the number of SN precursors we can detect is expected to dramatically increase, and we may also be able to probe deeper into the dimmer end of the precursor population (e.g., Tsuna et al 2023b;Strotjohann et al 2024). We expect that our framework would be helpful to characterize the origin and diversity of such precursors.…”

Section: Discussionmentioning

confidence: 94%

Bright Supernova Precursors by Outbursts from Massive Stars with Compact Object Companions

Tsuna,

Matsumoto,

et al. 2024

ApJ

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A fraction of core-collapse supernovae (SNe) with signs of interaction with a dense circumstellar matter are preceded by bright precursor emission. While the precursors are likely caused by a mass ejection before core collapse, their mechanism to power energetic bursts—sometimes reaching 1048–1049 erg, which is larger than the binding energies of red supergiant envelopes—is still under debate. Remarkably, such a huge energy deposition should result in an almost complete envelope ejection and hence a strong sign of interaction, but the observed SNe with precursors show in fact typical properties among the interacting SNe. More generally, the observed luminosity of 1040−1042 erg s−1 is shown to be challenging for a single SN progenitor. To resolve these tensions, we propose a scenario where the progenitor is in a binary system with a compact object (CO) and an outburst from the star leads to a super-Eddington accretion onto the CO. We show that for sufficiently short separations outbursts with moderate initial kinetic energies of 1046–1047 erg can be energized by the accreting CO so that their radiative output can be consistent with the observed precursors. We discuss the implications of our model in relation to CO binaries detectable with Gaia and gravitational-wave detectors.

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Section: Discussionmentioning

confidence: 94%

Bright Supernova Precursors by Outbursts from Massive Stars with Compact Object Companions

Tsuna,

Matsumoto,

et al. 2024

ApJ

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“…The Nancy Gray Roman Space Telescope (Roman; Spergel et al 2015) is also expected to explore the transient sky with its wide-field infrared capabilities. The resulting light curve sample will enable detailed studies of the distribution of explosion properties (e.g., Goldberg & Bildsten 2020;Barker et al 2023), and how they map onto progenitor star (e.g., Podsiadlowski et al 1992;Crowther 2007;Smartt 2009;Zapartas et al 2017;Renzo et al 2019;Strotjohann et al 2023) and host galaxy properties (e.g., Foley & Mandel 2013;Baldeschi et al 2020;Gagliano et al 2023). However, in addition to the expected abundance of garden variety SNe, such large samples will inevitably reveal anomalous events (e.g., Villar et al 2021) that offer potential insights into rare but important event classes.…”

Section: Introductionmentioning

confidence: 99%

The Effects of r-Process Enrichment in Hydrogen-rich Supernovae

Patel,

Goldberg,

Renzo

et al. 2024

ApJ

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Core-collapse supernovae (SNe) are candidate sites for rapid neutron capture process (r-process) nucleosynthesis. We explore the effects of enrichment from r-process nuclei on the light curves of hydrogen-rich SNe and assess the detectability of these signatures. We modify the radiation hydrodynamics code, SuperNova Explosion Code, to include the approximate effects of opacity and radioactive heating from r-process elements in the supernova (SN) ejecta. We present models spanning a range of total r-process masses M r and their assumed radial distribution within the ejecta, finding that M r ≳ 10−2 M ⊙ is sufficient to induce appreciable differences in their light curves as compared to ordinary hydrogen-rich SNe (without any r-process elements). The primary photometric signatures of r-process enrichment include a shortening of the plateau phase, coinciding with the hydrogen-recombination photosphere retreating to the r-process-enriched layers, and a steeper post-plateau decline associated with a reddening of the SN colors. We compare our r-process-enriched models to ordinary SNe models and observational data, showing that yields of M r ≳ 10−2 M ⊙ are potentially detectable across several of the metrics used by transient observers, provided that r-process-rich layers are mixed at least halfway to the ejecta surface. This detectability threshold can roughly be reproduced analytically using a two-zone (kilonova-within-an-SN) picture. Assuming that a small fraction of SNe produce a detectable r-process yield of M r ≳ 10−2 M ⊙, and respecting constraints on the total Galactic production rate, we estimate that ≳103–104 SNe need be observed to find one r-enriched event, a feat that may become possible with the Vera Rubin Observatory.

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Towards multi-messenger observations of core-collapse supernovae harbouring choked jets

Zegarelli,

Guetta,

Celli

et al. 2024

A&A

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Context. Over the past decade, choked jets have attracted particular attention as potential sources of high-energy cosmic neutrinos. It is challenging to test this hypothesis because of the missing gamma-ray counterpart. An identification of other electromagnetic signatures is therefore crucial. Extended H envelopes surrounding collapsing massive stars might choke launched jets. In addition, the same progenitors are expected to produce a shock-breakout signal in the ultraviolet (UV) and optical that lasts several days. Early UV radiation in particular carries important information about the presence and nature of choked jets. Aims. While UV observations of core-collapse supernovae have so far been limited, the full potential of observations in this spectral band will soon be transformed by the ULTRASAT satellite mission with its unprecedented field of view. We investigated the detection prospects of choked jet progenitors by ULTRASAT in relation to their visibility in the optical band by the currently operating telescope ZTF. In addition, as choked jets can produce neutrinos via hadronic and photohadronic interactions in choked jets, we also investigated how neutrino observations by existing Cherenkov high-energy neutrino telescopes (e.g. IceCube and KM3NeT) can be used in association with electromagnetic signals from shock-breakout events. Methods. By considering fiducial parameters of the source population and instrument performances, we estimated the maximum redshift up to which ULTRASAT and ZTF are able to detect ultraviolet and optical signals from these explosions, respectively. Furthermore, we discuss coordinated multi-messenger observations using ULTRASAT, ZTF, and high-energy neutrino telescopes. Results. We find that ULTRASAT will double the volume of the sky that is currently visible by ZTF for the same emitting sources. This will enlarge the sample of observed Type II supernovae by ∼60%. For optimised multi-messenger detections, the delay between neutrinos produced at the shock breakout (during the jet propagation inside the stellar envelope) and ULTRASAT observations should be of ∼4 (5) days, with subsequent follow-up by instruments such as ZTF about one week later. We estimate that fewer than 1% of the core-collapse supernovae from red supergiant stars that are detectable in UV with ULTRASAT might host a choked jet and release TeV neutrinos. Electromagnetic and neutrino detections, if accompanied by additional photometric and spectroscopic follow-up with compelling evidence for a relativistic jet launched by the central engine of the source, would suggest that core-collapse supernovae harbouring choked jets are the main contributors to the diffuse astrophysical high-energy neutrino flux.

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Search for Supernova Progenitor Stars with ZTF and LSST

Cited by 6 publications

References 95 publications

Bright Supernova Precursors by Outbursts from Massive Stars with Compact Object Companions

Bright Supernova Precursors by Outbursts from Massive Stars with Compact Object Companions

The Effects of r-Process Enrichment in Hydrogen-rich Supernovae

Towards multi-messenger observations of core-collapse supernovae harbouring choked jets

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