Shock Cooling and Possible Precursor Emission in the Early Light Curve of the Type II SN 2023ixf
Author
Hosseinzadeh, G.
Farah, J.
Shrestha, M.
Sand, D.J.
Dong, Y.
Brown, P.J.
Bostroem, K.A.
Valenti, S.

Jha, S.W.
Andrews, J.E.
Arcavi, I.

Haislip, J.
Hiramatsu, D.
Hoang, E.
Howell, D.A.
Janzen, D.
Jencson, J.E.
Kouprianov, V.
Lundquist, M.
McCully, C.

Meza, Retamal, N.E.
Modjaz, M.
Newsome, M.
Gonzalez, E.P.
Pearson, J.
Pellegrino, C.
Ravi, A.P.
Reichart, D.E.
Smith, N.
Terreran, G.
Vinkó, J.
Affiliation
Steward Observatory, University of ArizonaIssue Date
2023-08-14
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American Astronomical SocietyCitation
Griffin Hosseinzadeh et al 2023 ApJL 953 L16Journal
Astrophysical Journal LettersRights
© 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
We present the densely sampled early light curve of the Type II supernova (SN) 2023ixf, first observed within hours of explosion in the nearby Pinwheel Galaxy (Messier 101; 6.7 Mpc). Comparing these data to recently updated models of shock-cooling emission, we find that the progenitor likely had a radius of 410 ± 10 R ⊙. Our estimate is model dependent but consistent with a red supergiant. These models provide a good fit to the data starting about 1 day after the explosion, despite the fact that the classification spectrum shows signatures of circumstellar material around SN 2023ixf during that time. Photometry during the first day after the explosion, provided almost entirely by amateur astronomers, does not agree with the shock-cooling models or a simple power-law rise fit to data after 1 day. We consider the possible causes of this discrepancy, including precursor activity from the progenitor star, circumstellar interaction, and emission from the shock before or after it breaks out of the stellar surface. The very low luminosity (−11 mag > M > −14 mag) and short duration of the initial excess lead us to prefer a scenario related to prolonged emission from the SN shock traveling through the progenitor system. © 2023. The Author(s). Published by the American Astronomical Society.Note
Open access journalISSN
2041-8205Version
Final Published Versionae974a485f413a2113503eed53cd6c53
10.3847/2041-8213/ace4c4
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Except where otherwise noted, this item's license is described as © 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.