J/A+A/703/A62 SN 2016cvk light curves (Matilainen+, 2025)
Long-term evolution of the SN 2009ip-like transient SN 2016cvk.
Matilainen K.K., Kankare E., Mattila S., Reguitti A., Pignata G.,
Brimacombe J., Pastorello A., Fraser M., Brennan S.J., Anderson J.P.,
Ayala-Inostroza B., Cartier R., Charalampopoulos P., Chen T.-W.,
Gromadzki M., Gutierrez C.P., Inserra C., Muller-Bravo T.E., Nicholl M.,
Prieto J.L., Ragosta F., Reynolds T.M., Salmaso I., Young D.R.
<Astron. Astrophys. 703, A62 (2025)>
=2025A&A...703A..62M 2025A&A...703A..62M (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry, UBV ; Photometry, ugriz
Keywords: stars: circumstellar material - stars: massive -
supernovae: general - supernovae: individual: SN 2016cvk -
supernovae: individual - SN 2009ip
Abstract:
The interacting transient SN 2016cvk (ASASSN-16jt) is a member of the
peculiar SN 2009ip-like events. We present our follow-up data and aim
to draw conclusions about the physical nature of the progenitor
system.
Our spectrophotometric data set of SN 2016cvk covers the ultraviolet,
optical, and near-infrared wavelength region extending to +1681d from
the light curve peak; the data is analysed and compared to other SN
2009ip-like transients. Archival data reveals pre-outbursts of the
progenitor with the first detection at -1219d.
The light curve evolution of SN 2016cvk consists of two consecutive
luminous events A and B with peak magnitudes of MV←15.6 and
Mr=-18.3mag, respectively. The spectra are dominated by Balmer
emission lines that have a complex, multi-component evolution similar
to other SN 2009ip-like targets. SN 2016cvk is among the first
detected SN 2009ip-like events that show early 'flash ionisation'
features of CIII, NIII, and HeII, lasting for 16±5d. Our late-time
+405d spectrum shows forbidden [CaII], [FeII], and [OI] features with
the latter detected particularly clearly for a SN 2009ip-like event.
The evolution of SN 2016cvk is similar to other SN 2009ip-like
transients, with some uncommon traits. The lack of a double-peaked
structure in the Balmer lines is likely caused by differences in the
circumstellar medium structure or viewing angle. The flash features in
the early spectra propose abundances consistent with a red, yellow, or
blue supergiant progenitor rather than for example a luminous blue
variable. The detection of [OI] in the +405d spectrum suggests
possible evidence of nucleosynthesised material generated in a SN
explosion.
Description:
Optical imaging of the field of SN 2016cvk was taken between 2014
September 16 and 2021 April 9 in ugVrizY bands through several
observing programmes and in near-infrared JHK bands between 2016
September 9 and 2017 November 25.
Ground-based photometric measurements in optical bands for SN 2016cvk
are provided.
Objects:
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RA (2000) DE Designation(s)
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22 19 49.42 -40 40 05.5 SN2016cvk = ASASSN -16jt
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
photom.dat 120 134 Photometry of SN 2016cvk
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Byte-by-byte Description of file: photom.dat
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Bytes Format Units Label Explanations
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1- 7 F7.1 d JD Julian date (JD-2400000)
9- 15 F7.1 d t Time from r-band peak
17- 21 F5.2 mag umag ?=- Magnitude in u band
23- 26 F4.2 mag e_umag ?=- Error of magnitude in u band
28- 32 F5.2 mag Bmag ?=- Magnitude in B band
34- 37 F4.2 mag e_Bmag ?=- Error of magnitude in B band
39- 43 F5.2 mag gmag ?=- Magnitude in g band
45- 48 F4.2 mag e_gmag ?=- Error of magnitude in g band
50 A1 --- l_Vmag Limit flag on V band magnitude
51- 55 F5.2 mag Vmag ?=- Magnitude in V band
57- 60 F4.2 mag e_Vmag ?=- Error of magnitude in V band
62 A1 --- l_rmag Limit flag on r band magnitude
63- 67 F5.2 mag rmag ?=- Magnitude in r band
69- 72 F4.2 mag e_rmag ?=- Error of magnitude in r band
74- 78 F5.2 mag imag ?=- Magnitude in i band
80- 83 F4.2 mag e_imag ?=- Error of magnitude in i band
85- 89 F5.2 mag zmag ?=- Magnitude in z band
91- 94 F4.2 mag e_zmag ?=- Error of magnitude in z band
96-100 F5.2 mag Ymag ?=- Magnitude in Y band
102-105 F4.2 mag e_Ymag ?=- Error of magnitude in Y band
107-120 A14 --- Tel Telescope, instrument
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Acknowledgements:
Katja Matilainen, katja.matilainen(at)utu.fi
(End) Patricia Vannier [CDS] 04-Sep-2025