The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves: I. Signatures of H/He-free interaction in the first four months

H. Kuncarayakti; J. Sollerman; L. Izzo; K. Maeda; S. Yang; S. Schulze; C. R. Angus; M. Aubert; K. Auchettl; M. Della Valle; L. Dessart; K. Hinds; E. Kankare; M. Kawabata; P. Lundqvist; T. Nakaoka; D. Perley; S. I. Raimundo; N. L. Strotjohann; K. Taguchi; Y. Z. Cai; P. Charalampopoulos; Q. Fang; M. Fraser; C. P. Gutiérrez; R. Imazawa; T. Kangas; K. S. Kawabata; R. Kotak; T. Kravtsov; K. Matilainen; S. Mattila; S. Moran; I. Murata; I. Salmaso; J. P. Anderson; C. Ashall; E. C. Bellm; S. Benetti; K. C. Chambers; T. W. Chen; M. Coughlin; F. De Colle; C. Fremling; L. Galbany; A. Gal-Yam; M. Gromadzki; S. L. Groom; A. Hajela; C. Inserra; M. M. Kasliwal; A. A. Mahabal; A. Martin-Carrillo; T. Moore; T. E. Müller-Bravo; M. Nicholl; F. Ragosta; R. L. Riddle; Y. Sharma; S. Srivastav; M. D. Stritzinger; A. Wold; D. R. Young

doi:10.1051/0004-6361/202346526

The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves: I. Signatures of H/He-free interaction in the first four months

H. Kuncarayakti, J. Sollerman, L. Izzo, K. Maeda, S. Yang, S. Schulze, C. R. Angus, M. Aubert, K. Auchettl, M. Della Valle, L. Dessart, K. Hinds, E. Kankare, M. Kawabata, P. Lundqvist, T. Nakaoka, D. Perley, S. I. Raimundo, N. L. Strotjohann, K. TaguchiY. Z. Cai, P. Charalampopoulos, Q. Fang, M. Fraser, C. P. Gutiérrez, R. Imazawa, T. Kangas, K. S. Kawabata, R. Kotak, T. Kravtsov, K. Matilainen, S. Mattila, S. Moran, I. Murata, I. Salmaso, J. P. Anderson, C. Ashall, E. C. Bellm, S. Benetti, K. C. Chambers, T. W. Chen, M. Coughlin, F. De Colle, C. Fremling, L. Galbany, A. Gal-Yam, M. Gromadzki, S. L. Groom, A. Hajela, C. Inserra, M. M. Kasliwal, A. A. Mahabal, A. Martin-Carrillo, T. Moore, T. E. Müller-Bravo, M. Nicholl, F. Ragosta, R. L. Riddle, Y. Sharma, S. Srivastav, M. D. Stritzinger, A. Wold, D. R. Young

Physics and Astronomy (Twin Cities)

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Abstract

We report on our study of the supernova (SN) 2022xxf based on observations obtained during the first four months of its evolution. The light curves (LCs) display two humps of similar maximum brightness separated by 75 days, unprecedented for a broad-lined (BL) Type Ic supernova (SN IcBL). SN 2022xxf is the most nearby SN IcBL to date (in NGC 3705, z = 0.0037, at a distance of about 20 Mpc). Optical and near-infrared photometry and spectroscopy were used to identify the energy source powering the LC. Nearly 50 epochs of high signal-to-noise ratio spectroscopy were obtained within 130 days, comprising an unparalleled dataset for a SN IcBL, and one of the best-sampled SN datasets to date. The global spectral appearance and evolution of SN 2022xxf points to typical SN Ic/IcBL, with broad features (up to ∼14 000 km s-1) and a gradual transition from the photospheric to the nebular phase. However, narrow emission lines (corresponding to ∼ 1000 2500 km s-1) are present in the spectra from the time of the second rise, suggesting slower-moving circumstellar material (CSM). These lines are subtle, in comparison to the typical strong narrow lines of CSM-interacting SNe, for example, Type IIn, Ibn, and Icn, but some are readily noticeable at late times, such as in Mg I λ5170 and [O I] λ5577. Unusually, the near-infrared spectra show narrow line peaks in a number of features formed by ions of O and Mg. We infer the presence of CSM that is free of H and He. We propose that the radiative energy from the ejecta-CSM interaction is a plausible explanation for the second LC hump. This interaction scenario is supported by the color evolution, which progresses to blue as the light curve evolves along the second hump, and by the slow second rise and subsequent rapid LC drop. SN 2022xxf may be related to an emerging number of CSM-interacting SNe Ic, which show slow, peculiar LCs, blue colors, and subtle CSM interaction lines. The progenitor stars of these SNe likely experienced an episode of mass loss consisting of H/He-free material shortly prior to explosion.

Original language	English (US)
Article number	A209
Journal	Astronomy and Astrophysics
Volume	678
DOIs	https://doi.org/10.1051/0004-6361/202346526
State	Published - Oct 1 2023

Bibliographical note

Publisher Copyright:
© 2023 The Authors.

Keywords

Supernovae: general
Supernovae: individual: SN 2022xxf

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10.1051/0004-6361/202346526

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Kuncarayakti, H., Sollerman, J., Izzo, L., Maeda, K., Yang, S., Schulze, S., Angus, C. R., Aubert, M., Auchettl, K., Della Valle, M., Dessart, L., Hinds, K., Kankare, E., Kawabata, M., Lundqvist, P., Nakaoka, T., Perley, D., Raimundo, S. I., Strotjohann, N. L., ... Young, D. R. (2023). The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves: I. Signatures of H/He-free interaction in the first four months. Astronomy and Astrophysics, 678, Article A209. https://doi.org/10.1051/0004-6361/202346526

Kuncarayakti, H, Sollerman, J, Izzo, L, Maeda, K, Yang, S, Schulze, S, Angus, CR, Aubert, M, Auchettl, K, Della Valle, M, Dessart, L, Hinds, K, Kankare, E, Kawabata, M, Lundqvist, P, Nakaoka, T, Perley, D, Raimundo, SI, Strotjohann, NL, Taguchi, K, Cai, YZ, Charalampopoulos, P, Fang, Q, Fraser, M, Gutiérrez, CP, Imazawa, R, Kangas, T, Kawabata, KS, Kotak, R, Kravtsov, T, Matilainen, K, Mattila, S, Moran, S, Murata, I, Salmaso, I, Anderson, JP, Ashall, C, Bellm, EC, Benetti, S, Chambers, KC, Chen, TW, Coughlin, M, De Colle, F, Fremling, C, Galbany, L, Gal-Yam, A, Gromadzki, M, Groom, SL, Hajela, A, Inserra, C, Kasliwal, MM, Mahabal, AA, Martin-Carrillo, A, Moore, T, Müller-Bravo, TE, Nicholl, M, Ragosta, F, Riddle, RL, Sharma, Y, Srivastav, S, Stritzinger, MD, Wold, A & Young, DR 2023, 'The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves: I. Signatures of H/He-free interaction in the first four months', Astronomy and Astrophysics, vol. 678, A209. https://doi.org/10.1051/0004-6361/202346526

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title = "The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves: I. Signatures of H/He-free interaction in the first four months",

abstract = "We report on our study of the supernova (SN) 2022xxf based on observations obtained during the first four months of its evolution. The light curves (LCs) display two humps of similar maximum brightness separated by 75 days, unprecedented for a broad-lined (BL) Type Ic supernova (SN IcBL). SN 2022xxf is the most nearby SN IcBL to date (in NGC 3705, z = 0.0037, at a distance of about 20 Mpc). Optical and near-infrared photometry and spectroscopy were used to identify the energy source powering the LC. Nearly 50 epochs of high signal-to-noise ratio spectroscopy were obtained within 130 days, comprising an unparalleled dataset for a SN IcBL, and one of the best-sampled SN datasets to date. The global spectral appearance and evolution of SN 2022xxf points to typical SN Ic/IcBL, with broad features (up to ∼14 000 km s-1) and a gradual transition from the photospheric to the nebular phase. However, narrow emission lines (corresponding to ∼ 1000 2500 km s-1) are present in the spectra from the time of the second rise, suggesting slower-moving circumstellar material (CSM). These lines are subtle, in comparison to the typical strong narrow lines of CSM-interacting SNe, for example, Type IIn, Ibn, and Icn, but some are readily noticeable at late times, such as in Mg I λ5170 and [O I] λ5577. Unusually, the near-infrared spectra show narrow line peaks in a number of features formed by ions of O and Mg. We infer the presence of CSM that is free of H and He. We propose that the radiative energy from the ejecta-CSM interaction is a plausible explanation for the second LC hump. This interaction scenario is supported by the color evolution, which progresses to blue as the light curve evolves along the second hump, and by the slow second rise and subsequent rapid LC drop. SN 2022xxf may be related to an emerging number of CSM-interacting SNe Ic, which show slow, peculiar LCs, blue colors, and subtle CSM interaction lines. The progenitor stars of these SNe likely experienced an episode of mass loss consisting of H/He-free material shortly prior to explosion.",

keywords = "Supernovae: general, Supernovae: individual: SN 2022xxf",

author = "H. Kuncarayakti and J. Sollerman and L. Izzo and K. Maeda and S. Yang and S. Schulze and Angus, {C. R.} and M. Aubert and K. Auchettl and {Della Valle}, M. and L. Dessart and K. Hinds and E. Kankare and M. Kawabata and P. Lundqvist and T. Nakaoka and D. Perley and Raimundo, {S. I.} and Strotjohann, {N. L.} and K. Taguchi and Cai, {Y. Z.} and P. Charalampopoulos and Q. Fang and M. Fraser and Guti{\'e}rrez, {C. P.} and R. Imazawa and T. Kangas and Kawabata, {K. S.} and R. Kotak and T. Kravtsov and K. Matilainen and S. Mattila and S. Moran and I. Murata and I. Salmaso and Anderson, {J. P.} and C. Ashall and Bellm, {E. C.} and S. Benetti and Chambers, {K. C.} and Chen, {T. W.} and M. Coughlin and {De Colle}, F. and C. Fremling and L. Galbany and A. Gal-Yam and M. Gromadzki and Groom, {S. L.} and A. Hajela and C. Inserra and Kasliwal, {M. M.} and Mahabal, {A. A.} and A. Martin-Carrillo and T. Moore and M{\"u}ller-Bravo, {T. E.} and M. Nicholl and F. Ragosta and Riddle, {R. L.} and Y. Sharma and S. Srivastav and Stritzinger, {M. D.} and A. Wold and Young, {D. R.}",

note = "Publisher Copyright: {\textcopyright} 2023 The Authors.",

year = "2023",

month = oct,

day = "1",

doi = "10.1051/0004-6361/202346526",

language = "English (US)",

volume = "678",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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TY - JOUR

T1 - The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves

T2 - I. Signatures of H/He-free interaction in the first four months

AU - Kuncarayakti, H.

AU - Sollerman, J.

AU - Izzo, L.

AU - Maeda, K.

AU - Yang, S.

AU - Schulze, S.

AU - Angus, C. R.

AU - Aubert, M.

AU - Auchettl, K.

AU - Della Valle, M.

AU - Dessart, L.

AU - Hinds, K.

AU - Kankare, E.

AU - Kawabata, M.

AU - Lundqvist, P.

AU - Nakaoka, T.

AU - Perley, D.

AU - Raimundo, S. I.

AU - Strotjohann, N. L.

AU - Taguchi, K.

AU - Cai, Y. Z.

AU - Charalampopoulos, P.

AU - Fang, Q.

AU - Fraser, M.

AU - Gutiérrez, C. P.

AU - Imazawa, R.

AU - Kangas, T.

AU - Kawabata, K. S.

AU - Kotak, R.

AU - Kravtsov, T.

AU - Matilainen, K.

AU - Mattila, S.

AU - Moran, S.

AU - Murata, I.

AU - Salmaso, I.

AU - Anderson, J. P.

AU - Ashall, C.

AU - Bellm, E. C.

AU - Benetti, S.

AU - Chambers, K. C.

AU - Chen, T. W.

AU - Coughlin, M.

AU - De Colle, F.

AU - Fremling, C.

AU - Galbany, L.

AU - Gal-Yam, A.

AU - Gromadzki, M.

AU - Groom, S. L.

AU - Hajela, A.

AU - Inserra, C.

AU - Kasliwal, M. M.

AU - Mahabal, A. A.

AU - Martin-Carrillo, A.

AU - Moore, T.

AU - Müller-Bravo, T. E.

AU - Nicholl, M.

AU - Ragosta, F.

AU - Riddle, R. L.

AU - Sharma, Y.

AU - Srivastav, S.

AU - Stritzinger, M. D.

AU - Wold, A.

AU - Young, D. R.

PY - 2023/10/1

Y1 - 2023/10/1

N2 - We report on our study of the supernova (SN) 2022xxf based on observations obtained during the first four months of its evolution. The light curves (LCs) display two humps of similar maximum brightness separated by 75 days, unprecedented for a broad-lined (BL) Type Ic supernova (SN IcBL). SN 2022xxf is the most nearby SN IcBL to date (in NGC 3705, z = 0.0037, at a distance of about 20 Mpc). Optical and near-infrared photometry and spectroscopy were used to identify the energy source powering the LC. Nearly 50 epochs of high signal-to-noise ratio spectroscopy were obtained within 130 days, comprising an unparalleled dataset for a SN IcBL, and one of the best-sampled SN datasets to date. The global spectral appearance and evolution of SN 2022xxf points to typical SN Ic/IcBL, with broad features (up to ∼14 000 km s-1) and a gradual transition from the photospheric to the nebular phase. However, narrow emission lines (corresponding to ∼ 1000 2500 km s-1) are present in the spectra from the time of the second rise, suggesting slower-moving circumstellar material (CSM). These lines are subtle, in comparison to the typical strong narrow lines of CSM-interacting SNe, for example, Type IIn, Ibn, and Icn, but some are readily noticeable at late times, such as in Mg I λ5170 and [O I] λ5577. Unusually, the near-infrared spectra show narrow line peaks in a number of features formed by ions of O and Mg. We infer the presence of CSM that is free of H and He. We propose that the radiative energy from the ejecta-CSM interaction is a plausible explanation for the second LC hump. This interaction scenario is supported by the color evolution, which progresses to blue as the light curve evolves along the second hump, and by the slow second rise and subsequent rapid LC drop. SN 2022xxf may be related to an emerging number of CSM-interacting SNe Ic, which show slow, peculiar LCs, blue colors, and subtle CSM interaction lines. The progenitor stars of these SNe likely experienced an episode of mass loss consisting of H/He-free material shortly prior to explosion.

AB - We report on our study of the supernova (SN) 2022xxf based on observations obtained during the first four months of its evolution. The light curves (LCs) display two humps of similar maximum brightness separated by 75 days, unprecedented for a broad-lined (BL) Type Ic supernova (SN IcBL). SN 2022xxf is the most nearby SN IcBL to date (in NGC 3705, z = 0.0037, at a distance of about 20 Mpc). Optical and near-infrared photometry and spectroscopy were used to identify the energy source powering the LC. Nearly 50 epochs of high signal-to-noise ratio spectroscopy were obtained within 130 days, comprising an unparalleled dataset for a SN IcBL, and one of the best-sampled SN datasets to date. The global spectral appearance and evolution of SN 2022xxf points to typical SN Ic/IcBL, with broad features (up to ∼14 000 km s-1) and a gradual transition from the photospheric to the nebular phase. However, narrow emission lines (corresponding to ∼ 1000 2500 km s-1) are present in the spectra from the time of the second rise, suggesting slower-moving circumstellar material (CSM). These lines are subtle, in comparison to the typical strong narrow lines of CSM-interacting SNe, for example, Type IIn, Ibn, and Icn, but some are readily noticeable at late times, such as in Mg I λ5170 and [O I] λ5577. Unusually, the near-infrared spectra show narrow line peaks in a number of features formed by ions of O and Mg. We infer the presence of CSM that is free of H and He. We propose that the radiative energy from the ejecta-CSM interaction is a plausible explanation for the second LC hump. This interaction scenario is supported by the color evolution, which progresses to blue as the light curve evolves along the second hump, and by the slow second rise and subsequent rapid LC drop. SN 2022xxf may be related to an emerging number of CSM-interacting SNe Ic, which show slow, peculiar LCs, blue colors, and subtle CSM interaction lines. The progenitor stars of these SNe likely experienced an episode of mass loss consisting of H/He-free material shortly prior to explosion.

KW - Supernovae: general

KW - Supernovae: individual: SN 2022xxf

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UR - http://www.scopus.com/inward/citedby.url?scp=85176226553&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202346526

DO - 10.1051/0004-6361/202346526

M3 - Article

AN - SCOPUS:85176226553

SN - 0004-6361

VL - 678

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A209

ER -

The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves: I. Signatures of H/He-free interaction in the first four months

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