Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf
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Published:2023-10-01
Issue:1
Volume:956
Page:L5
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ISSN:2041-8205
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Container-title:The Astrophysical Journal Letters
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language:
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Short-container-title:ApJL
Author:
Bostroem K. AzaleeORCID, Pearson JeniveveORCID, Shrestha ManishaORCID, Sand David J.ORCID, Valenti StefanoORCID, Jha Saurabh W.ORCID, Andrews Jennifer E.ORCID, Smith NathanORCID, Terreran GiacomoORCID, Green Elizabeth, Dong 董 Yize 一泽ORCID, Lundquist MichaelORCID, Haislip JoshuaORCID, Hoang Emily T.ORCID, Hosseinzadeh GriffinORCID, Janzen DarylORCID, Jencson Jacob E.ORCID, Kouprianov VladimirORCID, Paraskeva EmmyORCID, Meza Retamal Nicolas E.ORCID, Reichart Daniel E.ORCID, Arcavi IairORCID, Bonanos Alceste Z.ORCID, Coughlin Michael W.ORCID, Dobson Ross, Farah JosephORCID, Galbany LluísORCID, Gutiérrez ClaudiaORCID, Hawley SuzanneORCID, Hebb LeslieORCID, Hiramatsu DaichiORCID, Howell D. AndrewORCID, Iijima Takashi, Ilyin IlyaORCID, Jhass Kiran, McCully CurtisORCID, Moran SeanORCID, Morris Brett M.ORCID, Mura Alessandra C.ORCID, Müller-Bravo Tomás E.ORCID, Munday James, Newsome MeganORCID, Pabst Maria Th.ORCID, Ochner PaoloORCID, Gonzalez Estefania PadillaORCID, Pastorello AndreaORCID, Pellegrino CraigORCID, Piscarreta LaraORCID, Ravi Aravind P.ORCID, Reguitti AndreaORCID, Salo LauraORCID, Vinkó JózsefORCID, de Vos Kellie, Wheeler J. C.ORCID, Williams G. GrantORCID, Wyatt SamuelORCID
Abstract
Abstract
We present the optical spectroscopic evolution of SN 2023ixf seen in subnight cadence spectra from 1.18 to 15 days after explosion. We identify high-ionization emission features, signatures of interaction with material surrounding the progenitor star, that fade over the first 7 days, with rapid evolution between spectra observed within the same night. We compare the emission lines present and their relative strength to those of other supernovae with early interaction, finding a close match to SN 2020pni and SN 2017ahn in the first spectrum and SN 2014G at later epochs. To physically interpret our observations, we compare them to CMFGEN models with confined, dense circumstellar material around a red supergiant (RSG) progenitor from the literature. We find that very few models reproduce the blended N iii (λλ4634.0,4640.6)/C iii (λλ4647.5,4650.0) emission lines observed in the first few spectra and their rapid disappearance thereafter, making this a unique diagnostic. From the best models, we find a mass-loss rate of 10−3–10−2
M
⊙ yr−1, which far exceeds the mass-loss rate for any steady wind, especially for an RSG in the initial mass range of the detected progenitor. These mass-loss rates are, however, similar to rates inferred for other supernovae with early circumstellar interaction. Using the phase when the narrow emission features disappear, we calculate an outer dense radius of circumstellar material R
CSM,out ≈ 5 × 1014 cm, and a mean circumstellar material density of ρ = 5.6 × 10−14 g cm−3. This is consistent with the lower limit on the outer radius of the circumstellar material we calculate from the peak Hα emission flux, R
CSM,out ≳ 9 × 1013 cm.
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
6 articles.
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