A luminous stellar outburst during a long-lasting eruptive phase first, and then SN IIn 2018cnf

A. Pastorello; A. Reguitti; A. Morales-Garoffolo; Z. Cano; S. J. Prentice; D. Hiramatsu; J. Burke; E. Kankare; R. Kotak; T. Reynolds; S. J. Smartt; S. Bose; P. Chen; E. Congiu; S. Dong; S. Geier; M. Gromadzki; E. Y. Hsiao; S. Kumar; P. Ochner; G. Pignata; L. Tomasella; L. Wang; I. Arcavi; C. Ashall; E. Callis; A. de Ugarte Postigo; M. Fraser; G. Hosseinzadeh; D. A. Howell; C. Inserra; D. A. Kann; E. Mason; P. A. Mazzali; C. McCully; Rodríguez; M. M. Phillips; K. W. Smith; L. Tartaglia; C. C. Thöne; T. Wevers; D. R. Young; M. L. Pumo; T. B. Lowe; E. A. Magnier; R. J. Wainscoat; C. Waters; D. E. Wright

doi:10.1051/0004-6361/201935420

A luminous stellar outburst during a long-lasting eruptive phase first, and then SN IIn 2018cnf

A. Pastorello, A. Reguitti, A. Morales-Garoffolo, Z. Cano, S. J. Prentice, D. Hiramatsu, J. Burke, E. Kankare, R. Kotak, T. Reynolds, S. J. Smartt, S. Bose, P. Chen, E. Congiu, S. Dong, S. Geier, M. Gromadzki, E. Y. Hsiao, S. Kumar, P. OchnerG. Pignata, L. Tomasella, L. Wang, I. Arcavi, C. Ashall, E. Callis, A. de Ugarte Postigo, M. Fraser, G. Hosseinzadeh, D. A. Howell, C. Inserra, D. A. Kann, E. Mason, P. A. Mazzali, C. McCully, Rodríguez, M. M. Phillips, K. W. Smith, L. Tartaglia, C. C. Thöne, T. Wevers, D. R. Young, M. L. Pumo, T. B. Lowe, E. A. Magnier, R. J. Wainscoat, C. Waters, D. E. Wright

School of Physics and Astronomy

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Abstract

We present the results of the monitoring campaign of the Type IIn supernova (SN) 2018cnf (a.k.a. ASASSN-18mr). It was discovered about ten days before the maximum light (on MJD = 58 293.4 ± 5.7 in the V band, with M_V = ?18.13 ± 0.15 mag). The multiband light curves show an immediate post-peak decline with some minor luminosity fluctuations, followed by a flattening starting about 40 days after maximum. The early spectra are relatively blue and show narrow Balmer lines with P Cygni profiles. Additionally, Fe II, O I, He I, and Ca II are detected. The spectra show little evolution with time and with intermediate-width features becoming progressively more prominent, indicating stronger interaction of the SN ejecta with the circumstellar medium. The inspection of archival images from the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) survey has revealed a variable source at the SN position with a brightest detection in December 2015 at M_r = ?14.66 ± 0.17 mag. This was likely an eruptive phase from the massive progenitor star that started from at least mid-2011, and that produced the circumstellar environment within which the star exploded as a Type IIn SN. The overall properties of SN 2018cnf closely resemble those of transients such as SN 2009ip. This similarity favours a massive hypergiant, perhaps a luminous blue variable, as progenitor for SN 2018cnf.

Original language	English
Article number	A93
Journal	Astronomy and Astrophysics
Volume	628
DOIs	https://doi.org/10.1051/0004-6361/201935420
State	Published - Aug 2019

Keywords

Outflows
Stars: winds
Supernovae: general
Supernovae: individual: SN 2009ip
Supernovae: individual: SN 2018cnf

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10.1051/0004-6361/201935420

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Pastorello, A., Reguitti, A., Morales-Garoffolo, A., Cano, Z., Prentice, S. J., Hiramatsu, D., Burke, J., Kankare, E., Kotak, R., Reynolds, T., Smartt, S. J., Bose, S., Chen, P., Congiu, E., Dong, S., Geier, S., Gromadzki, M., Hsiao, E. Y., Kumar, S., ... Wright, D. E. (2019). A luminous stellar outburst during a long-lasting eruptive phase first, and then SN IIn 2018cnf. Astronomy and Astrophysics, 628, Article A93. https://doi.org/10.1051/0004-6361/201935420

@article{5e1dea6df5fb4c1580640b42852c42ce,

title = "A luminous stellar outburst during a long-lasting eruptive phase first, and then SN IIn 2018cnf",

abstract = "We present the results of the monitoring campaign of the Type IIn supernova (SN) 2018cnf (a.k.a. ASASSN-18mr). It was discovered about ten days before the maximum light (on MJD = 58 293.4 ± 5.7 in the V band, with MV = ?18.13 ± 0.15 mag). The multiband light curves show an immediate post-peak decline with some minor luminosity fluctuations, followed by a flattening starting about 40 days after maximum. The early spectra are relatively blue and show narrow Balmer lines with P Cygni profiles. Additionally, Fe II, O I, He I, and Ca II are detected. The spectra show little evolution with time and with intermediate-width features becoming progressively more prominent, indicating stronger interaction of the SN ejecta with the circumstellar medium. The inspection of archival images from the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) survey has revealed a variable source at the SN position with a brightest detection in December 2015 at Mr = ?14.66 ± 0.17 mag. This was likely an eruptive phase from the massive progenitor star that started from at least mid-2011, and that produced the circumstellar environment within which the star exploded as a Type IIn SN. The overall properties of SN 2018cnf closely resemble those of transients such as SN 2009ip. This similarity favours a massive hypergiant, perhaps a luminous blue variable, as progenitor for SN 2018cnf.",

keywords = "Outflows, Stars: winds, Supernovae: general, Supernovae: individual: SN 2009ip, Supernovae: individual: SN 2018cnf",

author = "A. Pastorello and A. Reguitti and A. Morales-Garoffolo and Z. Cano and Prentice, {S. J.} and D. Hiramatsu and J. Burke and E. Kankare and R. Kotak and T. Reynolds and Smartt, {S. J.} and S. Bose and P. Chen and E. Congiu and S. Dong and S. Geier and M. Gromadzki and Hsiao, {E. Y.} and S. Kumar and P. Ochner and G. Pignata and L. Tomasella and L. Wang and I. Arcavi and C. Ashall and E. Callis and {de Ugarte Postigo}, A. and M. Fraser and G. Hosseinzadeh and Howell, {D. A.} and C. Inserra and Kann, {D. A.} and E. Mason and Mazzali, {P. A.} and C. McCully and Rodr{\'i}guez and Phillips, {M. M.} and Smith, {K. W.} and L. Tartaglia and Th{\"o}ne, {C. C.} and T. Wevers and Young, {D. R.} and Pumo, {M. L.} and Lowe, {T. B.} and Magnier, {E. A.} and Wainscoat, {R. J.} and C. Waters and Wright, {D. E.}",

note = "Publisher Copyright: {\textcopyright} ESO 2019",

year = "2019",

month = aug,

doi = "10.1051/0004-6361/201935420",

language = "אנגלית",

volume = "628",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Pastorello, A, Reguitti, A, Morales-Garoffolo, A, Cano, Z, Prentice, SJ, Hiramatsu, D, Burke, J, Kankare, E, Kotak, R, Reynolds, T, Smartt, SJ, Bose, S, Chen, P, Congiu, E, Dong, S, Geier, S, Gromadzki, M, Hsiao, EY, Kumar, S, Ochner, P, Pignata, G, Tomasella, L, Wang, L, Arcavi, I, Ashall, C, Callis, E, de Ugarte Postigo, A, Fraser, M, Hosseinzadeh, G, Howell, DA, Inserra, C, Kann, DA, Mason, E, Mazzali, PA, McCully, C, Rodríguez, Phillips, MM, Smith, KW, Tartaglia, L, Thöne, CC, Wevers, T, Young, DR, Pumo, ML, Lowe, TB, Magnier, EA, Wainscoat, RJ, Waters, C & Wright, DE 2019, 'A luminous stellar outburst during a long-lasting eruptive phase first, and then SN IIn 2018cnf', Astronomy and Astrophysics, vol. 628, A93. https://doi.org/10.1051/0004-6361/201935420

TY - JOUR

T1 - A luminous stellar outburst during a long-lasting eruptive phase first, and then SN IIn 2018cnf

AU - Pastorello, A.

AU - Reguitti, A.

AU - Morales-Garoffolo, A.

AU - Cano, Z.

AU - Prentice, S. J.

AU - Hiramatsu, D.

AU - Burke, J.

AU - Kankare, E.

AU - Kotak, R.

AU - Reynolds, T.

AU - Smartt, S. J.

AU - Bose, S.

AU - Chen, P.

AU - Congiu, E.

AU - Dong, S.

AU - Geier, S.

AU - Gromadzki, M.

AU - Hsiao, E. Y.

AU - Kumar, S.

AU - Ochner, P.

AU - Pignata, G.

AU - Tomasella, L.

AU - Wang, L.

AU - Arcavi, I.

AU - Ashall, C.

AU - Callis, E.

AU - de Ugarte Postigo, A.

AU - Fraser, M.

AU - Hosseinzadeh, G.

AU - Howell, D. A.

AU - Inserra, C.

AU - Kann, D. A.

AU - Mason, E.

AU - Mazzali, P. A.

AU - McCully, C.

AU - Rodríguez,

AU - Phillips, M. M.

AU - Smith, K. W.

AU - Tartaglia, L.

AU - Thöne, C. C.

AU - Wevers, T.

AU - Young, D. R.

AU - Pumo, M. L.

AU - Lowe, T. B.

AU - Magnier, E. A.

AU - Wainscoat, R. J.

AU - Waters, C.

AU - Wright, D. E.

PY - 2019/8

Y1 - 2019/8

N2 - We present the results of the monitoring campaign of the Type IIn supernova (SN) 2018cnf (a.k.a. ASASSN-18mr). It was discovered about ten days before the maximum light (on MJD = 58 293.4 ± 5.7 in the V band, with MV = ?18.13 ± 0.15 mag). The multiband light curves show an immediate post-peak decline with some minor luminosity fluctuations, followed by a flattening starting about 40 days after maximum. The early spectra are relatively blue and show narrow Balmer lines with P Cygni profiles. Additionally, Fe II, O I, He I, and Ca II are detected. The spectra show little evolution with time and with intermediate-width features becoming progressively more prominent, indicating stronger interaction of the SN ejecta with the circumstellar medium. The inspection of archival images from the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) survey has revealed a variable source at the SN position with a brightest detection in December 2015 at Mr = ?14.66 ± 0.17 mag. This was likely an eruptive phase from the massive progenitor star that started from at least mid-2011, and that produced the circumstellar environment within which the star exploded as a Type IIn SN. The overall properties of SN 2018cnf closely resemble those of transients such as SN 2009ip. This similarity favours a massive hypergiant, perhaps a luminous blue variable, as progenitor for SN 2018cnf.

AB - We present the results of the monitoring campaign of the Type IIn supernova (SN) 2018cnf (a.k.a. ASASSN-18mr). It was discovered about ten days before the maximum light (on MJD = 58 293.4 ± 5.7 in the V band, with MV = ?18.13 ± 0.15 mag). The multiband light curves show an immediate post-peak decline with some minor luminosity fluctuations, followed by a flattening starting about 40 days after maximum. The early spectra are relatively blue and show narrow Balmer lines with P Cygni profiles. Additionally, Fe II, O I, He I, and Ca II are detected. The spectra show little evolution with time and with intermediate-width features becoming progressively more prominent, indicating stronger interaction of the SN ejecta with the circumstellar medium. The inspection of archival images from the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) survey has revealed a variable source at the SN position with a brightest detection in December 2015 at Mr = ?14.66 ± 0.17 mag. This was likely an eruptive phase from the massive progenitor star that started from at least mid-2011, and that produced the circumstellar environment within which the star exploded as a Type IIn SN. The overall properties of SN 2018cnf closely resemble those of transients such as SN 2009ip. This similarity favours a massive hypergiant, perhaps a luminous blue variable, as progenitor for SN 2018cnf.

KW - Outflows

KW - Stars: winds

KW - Supernovae: general

KW - Supernovae: individual: SN 2009ip

KW - Supernovae: individual: SN 2018cnf

UR - http://www.scopus.com/inward/record.url?scp=85079430632&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201935420

DO - 10.1051/0004-6361/201935420

M3 - ???researchoutput.researchoutputtypes.contributiontojournal.article???

AN - SCOPUS:85079430632

SN - 0004-6361

VL - 628

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A93

ER -

A luminous stellar outburst during a long-lasting eruptive phase first, and then SN IIn 2018cnf

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Keywords

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