The complex circumstellar environment of supernova 2023ixf

E. A. Zimmerman; I. Irani; P. Chen; A. Gal-Yam; S. Schulze; D. A. Perley; J. Sollerman; A. V. Filippenko; T. Shenar; O. Yaron; S. Shahaf; R. J. Bruch; E. O. Ofek; A. De Cia; T. G. Brink; Y. Yang; S. S. Vasylyev; S. Ben Ami; M. Aubert; A. Badash; J. S. Bloom; P. J. Brown; K. De; G. Dimitriadis; C. Fransson; C. Fremling; K. Hinds; A. Horesh; J. P. Johansson; M. M. Kasliwal; S. R. Kulkarni; D. Kushnir; C. Martin; M. Matuzewski; R. C. McGurk; A. A. Miller; J. Morag; J. D. Neil; P. E. Nugent; R. S. Post; N. Z. Prusinski; Y. Qin; A. Raichoor; R. Riddle; M. Rowe; B. Rusholme; I. Sfaradi; K. M. Sjoberg; M. Soumagnac; R. D. Stein; N. L. Strotjohann; J. H. Terwel; T. Wasserman; J. Wise; A. Wold; L. Yan; K. Zhang

doi:10.1038/s41586-024-07116-6

The complex circumstellar environment of supernova 2023ixf

E. A. Zimmerman^*, I. Irani, P. Chen, A. Gal-Yam, S. Schulze, D. A. Perley, J. Sollerman, A. V. Filippenko, T. Shenar, O. Yaron, S. Shahaf, R. J. Bruch, E. O. Ofek, A. De Cia, T. G. Brink, Y. Yang, S. S. Vasylyev, S. Ben Ami, M. Aubert, A. BadashJ. S. Bloom, P. J. Brown, K. De, G. Dimitriadis, C. Fransson, C. Fremling, K. Hinds, A. Horesh, J. P. Johansson, M. M. Kasliwal, S. R. Kulkarni, D. Kushnir, C. Martin, M. Matuzewski, R. C. McGurk, A. A. Miller, J. Morag, J. D. Neil, P. E. Nugent, R. S. Post, N. Z. Prusinski, Y. Qin, A. Raichoor, R. Riddle, M. Rowe, B. Rusholme, I. Sfaradi, K. M. Sjoberg, M. Soumagnac, R. D. Stein, N. L. Strotjohann, J. H. Terwel, T. Wasserman, J. Wise, A. Wold, L. Yan, K. Zhang

^*Corresponding author for this work

Physics and Astronomy

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Abstract

The early evolution of a supernova (SN) can reveal information about the environment and the progenitor star. When a star explodes in vacuum, the first photons to escape from its surface appear as a brief, hours-long shock-breakout flare^1,2, followed by a cooling phase of emission. However, for stars exploding within a distribution of dense, optically thick circumstellar material (CSM), the first photons escape from the material beyond the stellar edge and the duration of the initial flare can extend to several days, during which the escaping emission indicates photospheric heating³. Early serendipitous observations^2,4 that lacked ultraviolet (UV) data were unable to determine whether the early emission is heating or cooling and hence the nature of the early explosion event. Here we report UV spectra of the nearby SN 2023ixf in the galaxy Messier 101 (M101). Using the UV data as well as a comprehensive set of further multiwavelength observations, we temporally resolve the emergence of the explosion shock from a thick medium heated by the SN emission. We derive a reliable bolometric light curve that indicates that the shock breaks out from a dense layer with a radius substantially larger than typical supergiants.

Original language	English (US)
Pages (from-to)	759-762
Number of pages	4
Journal	Nature
Volume	627
Issue number	8005
DOIs	https://doi.org/10.1038/s41586-024-07116-6
State	Published - Mar 28 2024

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Zimmerman, E. A., Irani, I., Chen, P., Gal-Yam, A., Schulze, S., Perley, D. A., Sollerman, J., Filippenko, A. V., Shenar, T., Yaron, O., Shahaf, S., Bruch, R. J., Ofek, E. O., De Cia, A., Brink, T. G., Yang, Y., Vasylyev, S. S., Ben Ami, S., Aubert, M., ... Zhang, K. (2024). The complex circumstellar environment of supernova 2023ixf. Nature, 627(8005), 759-762. https://doi.org/10.1038/s41586-024-07116-6

@article{904cb9826c31478b8fc140de023e2fb2,

title = "The complex circumstellar environment of supernova 2023ixf",

abstract = "The early evolution of a supernova (SN) can reveal information about the environment and the progenitor star. When a star explodes in vacuum, the first photons to escape from its surface appear as a brief, hours-long shock-breakout flare1,2, followed by a cooling phase of emission. However, for stars exploding within a distribution of dense, optically thick circumstellar material (CSM), the first photons escape from the material beyond the stellar edge and the duration of the initial flare can extend to several days, during which the escaping emission indicates photospheric heating3. Early serendipitous observations2,4 that lacked ultraviolet (UV) data were unable to determine whether the early emission is heating or cooling and hence the nature of the early explosion event. Here we report UV spectra of the nearby SN 2023ixf in the galaxy Messier 101 (M101). Using the UV data as well as a comprehensive set of further multiwavelength observations, we temporally resolve the emergence of the explosion shock from a thick medium heated by the SN emission. We derive a reliable bolometric light curve that indicates that the shock breaks out from a dense layer with a radius substantially larger than typical supergiants.",

author = "Zimmerman, {E. A.} and I. Irani and P. Chen and A. Gal-Yam and S. Schulze and Perley, {D. A.} and J. Sollerman and Filippenko, {A. V.} and T. Shenar and O. Yaron and S. Shahaf and Bruch, {R. J.} and Ofek, {E. O.} and {De Cia}, A. and Brink, {T. G.} and Y. Yang and Vasylyev, {S. S.} and {Ben Ami}, S. and M. Aubert and A. Badash and Bloom, {J. S.} and Brown, {P. J.} and K. De and G. Dimitriadis and C. Fransson and C. Fremling and K. Hinds and A. Horesh and Johansson, {J. P.} and Kasliwal, {M. M.} and Kulkarni, {S. R.} and D. Kushnir and C. Martin and M. Matuzewski and McGurk, {R. C.} and Miller, {A. A.} and J. Morag and Neil, {J. D.} and Nugent, {P. E.} and Post, {R. S.} and Prusinski, {N. Z.} and Y. Qin and A. Raichoor and R. Riddle and M. Rowe and B. Rusholme and I. Sfaradi and Sjoberg, {K. M.} and M. Soumagnac and Stein, {R. D.} and Strotjohann, {N. L.} and Terwel, {J. H.} and T. Wasserman and J. Wise and A. Wold and L. Yan and K. Zhang",

note = "Publisher Copyright: {\textcopyright} The Author(s), under exclusive licence to Springer Nature Limited 2024.",

year = "2024",

month = mar,

day = "28",

doi = "10.1038/s41586-024-07116-6",

language = "English (US)",

volume = "627",

pages = "759--762",

journal = "Nature",

issn = "0028-0836",

publisher = "Nature Publishing Group",

number = "8005",

}

Zimmerman, EA, Irani, I, Chen, P, Gal-Yam, A, Schulze, S, Perley, DA, Sollerman, J, Filippenko, AV, Shenar, T, Yaron, O, Shahaf, S, Bruch, RJ, Ofek, EO, De Cia, A, Brink, TG, Yang, Y, Vasylyev, SS, Ben Ami, S, Aubert, M, Badash, A, Bloom, JS, Brown, PJ, De, K, Dimitriadis, G, Fransson, C, Fremling, C, Hinds, K, Horesh, A, Johansson, JP, Kasliwal, MM, Kulkarni, SR, Kushnir, D, Martin, C, Matuzewski, M, McGurk, RC, Miller, AA, Morag, J, Neil, JD, Nugent, PE, Post, RS, Prusinski, NZ, Qin, Y, Raichoor, A, Riddle, R, Rowe, M, Rusholme, B, Sfaradi, I, Sjoberg, KM, Soumagnac, M, Stein, RD, Strotjohann, NL, Terwel, JH, Wasserman, T, Wise, J, Wold, A, Yan, L & Zhang, K 2024, 'The complex circumstellar environment of supernova 2023ixf', Nature, vol. 627, no. 8005, pp. 759-762. https://doi.org/10.1038/s41586-024-07116-6

TY - JOUR

T1 - The complex circumstellar environment of supernova 2023ixf

AU - Zimmerman, E. A.

AU - Irani, I.

AU - Chen, P.

AU - Gal-Yam, A.

AU - Schulze, S.

AU - Perley, D. A.

AU - Sollerman, J.

AU - Filippenko, A. V.

AU - Shenar, T.

AU - Yaron, O.

AU - Shahaf, S.

AU - Bruch, R. J.

AU - Ofek, E. O.

AU - De Cia, A.

AU - Brink, T. G.

AU - Yang, Y.

AU - Vasylyev, S. S.

AU - Ben Ami, S.

AU - Aubert, M.

AU - Badash, A.

AU - Bloom, J. S.

AU - Brown, P. J.

AU - De, K.

AU - Dimitriadis, G.

AU - Fransson, C.

AU - Fremling, C.

AU - Hinds, K.

AU - Horesh, A.

AU - Johansson, J. P.

AU - Kasliwal, M. M.

AU - Kulkarni, S. R.

AU - Kushnir, D.

AU - Martin, C.

AU - Matuzewski, M.

AU - McGurk, R. C.

AU - Miller, A. A.

AU - Morag, J.

AU - Neil, J. D.

AU - Nugent, P. E.

AU - Post, R. S.

AU - Prusinski, N. Z.

AU - Qin, Y.

AU - Raichoor, A.

AU - Riddle, R.

AU - Rowe, M.

AU - Rusholme, B.

AU - Sfaradi, I.

AU - Sjoberg, K. M.

AU - Soumagnac, M.

AU - Stein, R. D.

AU - Strotjohann, N. L.

AU - Terwel, J. H.

AU - Wasserman, T.

AU - Wise, J.

AU - Wold, A.

AU - Yan, L.

AU - Zhang, K.

PY - 2024/3/28

Y1 - 2024/3/28

N2 - The early evolution of a supernova (SN) can reveal information about the environment and the progenitor star. When a star explodes in vacuum, the first photons to escape from its surface appear as a brief, hours-long shock-breakout flare1,2, followed by a cooling phase of emission. However, for stars exploding within a distribution of dense, optically thick circumstellar material (CSM), the first photons escape from the material beyond the stellar edge and the duration of the initial flare can extend to several days, during which the escaping emission indicates photospheric heating3. Early serendipitous observations2,4 that lacked ultraviolet (UV) data were unable to determine whether the early emission is heating or cooling and hence the nature of the early explosion event. Here we report UV spectra of the nearby SN 2023ixf in the galaxy Messier 101 (M101). Using the UV data as well as a comprehensive set of further multiwavelength observations, we temporally resolve the emergence of the explosion shock from a thick medium heated by the SN emission. We derive a reliable bolometric light curve that indicates that the shock breaks out from a dense layer with a radius substantially larger than typical supergiants.

AB - The early evolution of a supernova (SN) can reveal information about the environment and the progenitor star. When a star explodes in vacuum, the first photons to escape from its surface appear as a brief, hours-long shock-breakout flare1,2, followed by a cooling phase of emission. However, for stars exploding within a distribution of dense, optically thick circumstellar material (CSM), the first photons escape from the material beyond the stellar edge and the duration of the initial flare can extend to several days, during which the escaping emission indicates photospheric heating3. Early serendipitous observations2,4 that lacked ultraviolet (UV) data were unable to determine whether the early emission is heating or cooling and hence the nature of the early explosion event. Here we report UV spectra of the nearby SN 2023ixf in the galaxy Messier 101 (M101). Using the UV data as well as a comprehensive set of further multiwavelength observations, we temporally resolve the emergence of the explosion shock from a thick medium heated by the SN emission. We derive a reliable bolometric light curve that indicates that the shock breaks out from a dense layer with a radius substantially larger than typical supergiants.

UR - http://www.scopus.com/inward/record.url?scp=85188894094&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85188894094&partnerID=8YFLogxK

U2 - 10.1038/s41586-024-07116-6

DO - 10.1038/s41586-024-07116-6

M3 - Article

C2 - 38538936

AN - SCOPUS:85188894094

SN - 0028-0836

VL - 627

SP - 759

EP - 762

JO - Nature

JF - Nature

IS - 8005

ER -

The complex circumstellar environment of supernova 2023ixf

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