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Resolving the explosion of supernova 2023ixf in Messier 101 within its complex circumstellar environment

Fuente: arXiv

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Bibliographic Details
Main Authors:	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., Ami, S. Ben, Aubert, M., Badash, A., Bloom, J. S., Brown, P. J., De, K., Dimitriadis, G., Fransson, C., Fremling, C., Hinds, K., Horesh, A., Johansson, J. P., Kasliwal, M. M., Kulkarni, S. R., Kushnir, D., Martin, C., Matuzewski, M., McGurk, R. C., Miller, A. A., Morag, J., Neil, J. D., Nugent, P. E., Post, R. S., Prusinski, N. Z., Qin, Y., Raichoor, A., Riddle, R., Rowe, M., Rusholme, B., Sfaradi, I., Sjoberg, K. M., Soumagnac, M., Stein, R. D., Strotjohann, N. L., Terwel, J. H., Wasserman, T., Wise, J., Wold, A., Yan, L., Zhang, K.
Format:	Preprint
Published:	2023
Subjects:	High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics
Online Access:	Acceder al recurso
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_version_	1866916178866208768
author	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. Ami, S. Ben Aubert, M. Badash, A. Bloom, J. S. Brown, P. J. De, K. Dimitriadis, G. Fransson, C. Fremling, C. Hinds, K. Horesh, A. Johansson, J. P. Kasliwal, M. M. Kulkarni, S. R. Kushnir, D. Martin, C. Matuzewski, M. McGurk, R. C. Miller, A. A. Morag, J. Neil, J. D. Nugent, P. E. Post, R. S. Prusinski, N. Z. Qin, Y. Raichoor, A. Riddle, R. Rowe, M. Rusholme, B. Sfaradi, I. Sjoberg, K. M. Soumagnac, M. Stein, R. D. Strotjohann, N. L. Terwel, J. H. Wasserman, T. Wise, J. Wold, A. Yan, L. Zhang, K.
author_facet	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. Ami, S. Ben Aubert, M. Badash, A. Bloom, J. S. Brown, P. J. De, K. Dimitriadis, G. Fransson, C. Fremling, C. Hinds, K. Horesh, A. Johansson, J. P. Kasliwal, M. M. Kulkarni, S. R. Kushnir, D. Martin, C. Matuzewski, M. McGurk, R. C. Miller, A. A. Morag, J. Neil, J. D. Nugent, P. E. Post, R. S. Prusinski, N. Z. Qin, Y. Raichoor, A. Riddle, R. Rowe, M. Rusholme, B. Sfaradi, I. Sjoberg, K. M. Soumagnac, M. Stein, R. D. Strotjohann, N. L. Terwel, J. H. Wasserman, T. Wise, J. Wold, A. Yan, L. Zhang, K.
contents	Observing a supernova explosion shortly after it occurs can reveal important information about the physics of stellar explosions and the nature of the progenitor stars of supernovae (SNe). When a star with a well-defined edge explodes in vacuum, the first photons to escape from its surface appear as a brief shock-breakout flare. The duration of this flare can extend to at most a few hours even for nonspherical breakouts from supergiant stars, after which the explosion ejecta should expand and cool. Alternatively, for stars exploding within a distribution of sufficiently dense optically thick circumstellar material, 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 heating. The difficulty in detecting SN explosions promptly after the event has so far limited data regarding supergiant stellar explosions mostly to serendipitous observations that, owing to the lack of 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 observations of SN 2023ixf in the nearby galaxy M101, covering the early days of the event. Using UV spectroscopy from the Hubble Space Telescope (HST) as well as a comprehensive set of additional multiwavelength observations, we trace the photometric and spectroscopic evolution of the event and are able to temporally resolve the emergence and evolution of the SN emission.
format	Preprint
id	arxiv_https___arxiv_org_abs_2310_10727
institution	arXiv
publishDate	2023
record_format	arxiv
spellingShingle	Resolving the explosion of supernova 2023ixf in Messier 101 within its complex circumstellar environment 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. Ami, S. Ben Aubert, M. Badash, A. Bloom, J. S. Brown, P. J. De, K. Dimitriadis, G. Fransson, C. Fremling, C. Hinds, K. Horesh, A. Johansson, J. P. Kasliwal, M. M. Kulkarni, S. R. Kushnir, D. Martin, C. Matuzewski, M. McGurk, R. C. Miller, A. A. Morag, J. Neil, J. D. Nugent, P. E. Post, R. S. Prusinski, N. Z. Qin, Y. Raichoor, A. Riddle, R. Rowe, M. Rusholme, B. Sfaradi, I. Sjoberg, K. M. Soumagnac, M. Stein, R. D. Strotjohann, N. L. Terwel, J. H. Wasserman, T. Wise, J. Wold, A. Yan, L. Zhang, K. High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics Observing a supernova explosion shortly after it occurs can reveal important information about the physics of stellar explosions and the nature of the progenitor stars of supernovae (SNe). When a star with a well-defined edge explodes in vacuum, the first photons to escape from its surface appear as a brief shock-breakout flare. The duration of this flare can extend to at most a few hours even for nonspherical breakouts from supergiant stars, after which the explosion ejecta should expand and cool. Alternatively, for stars exploding within a distribution of sufficiently dense optically thick circumstellar material, 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 heating. The difficulty in detecting SN explosions promptly after the event has so far limited data regarding supergiant stellar explosions mostly to serendipitous observations that, owing to the lack of 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 observations of SN 2023ixf in the nearby galaxy M101, covering the early days of the event. Using UV spectroscopy from the Hubble Space Telescope (HST) as well as a comprehensive set of additional multiwavelength observations, we trace the photometric and spectroscopic evolution of the event and are able to temporally resolve the emergence and evolution of the SN emission.
title	Resolving the explosion of supernova 2023ixf in Messier 101 within its complex circumstellar environment
topic	High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics
url	https://arxiv.org/abs/2310.10727