[Okc-wp4] EO meeting: 16th of June

[Ana Sagués Carracedo]

Here the link to the recording of the meeting: https://stockholmuniversity.box.com/s/3mzdkzc0ww6et2h4ific7ori6cg433ns

Thank you so much Wynn for a great talk and discussion.

Bests,
Ana

On 9 Jun 2022, at 13:36, Ana Sagués Carracedo <ana.sagues-carracedo at fysik.su.se<mailto:ana.sagues-carracedo at fysik.su.se>> wrote:

Dear all,

our next and last Extreme Object meeting before the summer break will be held next Thursday, 16th of April, at 13:15 (CET). The speaker is Wynn Jacobson-Galan a fellow researcher from Berkeley visiting us in Stockholm next week.

The meeting will be held in hybrid mode at the Albano 3:6228 - Mega room. Some directions for those that have never been in the Mega room, it is located in Nordita (floor 6 house 3), if you enter from the door on the right of the elevator it is just there. I will be a little in advance to set up the room, and I can open the door for people with no access.

To join the meeting online:
https://stockholmuniversity.zoom.us/j/65883589027?pwd=RGxJOUVQWmNtMlZFMUIwaHRabkExdz09

Meeting ID: 658 8358 9027



Title: Watching a Star Explode with the Young Supernova Experiment

Abstract: We present multi-wavelength observations of supernova (SN) 2020tlf, the first normal type II-P/L SN with confirmed precursor emission, as detected by the Young Supernova Experiment (YSE) transient survey. The detected pre-explosion emission for ~130 days prior to SN is consistent with either a super-Eddington progenitor wind or a wave-driven eruption. Soon after discovery, “flash” spectroscopy of SN 2020tlf revealed prominent narrow emission lines from shock-ionized circumstellar material (CSM) shed in progenitor mass-loss episodes in the final months before explosion. Following classification, SN 2020tlf was observed in a thorough multi-wavelength follow-up campaign in UV/optical/IR, radio and X-ray bands out to a +300 days after explosion. The nebular phase spectra of SN 2020tlf constrain the possible mass of the red supergiant progenitor to 10-12 Msun. Finally, we present radiative transfer modeling of the SN light curve and spectral evolution, which reveals that the progenitor star had an extended envelope, detached CSM and a heightened mass loss rate. We will discuss how the progenitor and CSM properties of SN 2020tlf fits within the phase space of the small but growing number of SNe with “flash” spectroscopy and pre-explosion eruptions. Furthermore, we will discuss the physical processes capable of producing such luminous precursor emission in a red supergiant in the final year(s) before explosion.




Kind regards,
Ana Sagués Carracedo & Haakon Andresen



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