A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Long-term evolution of the SN 2009ip-like transient SN 2016cvk
Tekijät: Matilainen, Katja K.; Kankare, Erkki; Mattila, Seppo ; Reguitti, Andrea; Pignata, Giuliano; Brimacombe, Judy; Pastorello, Andrea; Fraser, Morgan; Brennan, Seán J.; Anderson, James P.; Ayala-Inostroza, Bastian; Cartier, Regis; Charalampopoulos, Panagiotis; Chen, Tsai-Wen.; Gromadzki, Mariusz; Gutierrez, Claudia P.; Inserra, Cosimo; Müller-Bravo, Tomás E.; Nicholl, Matt; Prieto, Jose L.; Ragosta, Fabio; Reynolds, Thomas M.; Salmaso, Irene; Young, Deborah Rohm
Kustantaja: EDP Sciences
Julkaisuvuosi: 2025
Lehti: Astronomy and Astrophysics
Artikkelin numero: A62
Vuosikerta: 703
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202555740
Julkaisun avoimuus kirjaamishetkellä: Avoimesti saatavilla
Julkaisukanavan avoimuus : Kokonaan avoin julkaisukanava
Verkko-osoite: https://doi.org/10.1051/0004-6361/202555740
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/505555066
Aims
The interacting transient SN 2016cvk (ASASSN-16jt) is a peculiar SN 2009ip-like event. We present our follow-up data with an aim to draw conclusions on the physical nature of the progenitor system.
Methods
Our spectrophotometric data set of SN 2016cvk covers the ultraviolet, optical, and near-infrared wavelength region extending to +1681 d from the light curve peak. In this work, we analysed the data and made comparison with other SN 2009ip-like transients. We note that archival data reveal pre-outbursts of the progenitor with the first detection at –1219 d.
Results
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 = −18.3 mag, respectively. The spectra are dominated by Balmer emission lines that have a complex, multi-component evolution resembling that of other SN 2009ip-like targets. SN 2016cvk is among the first detected SN 2009ip-like events that show early ‘flash ionisation’ features of C III, N III, and He II, lasting for 16 ± 5 d. Our late-time +405 d spectrum shows forbidden [Ca II], [Fe II], and [O I] features, with the latter detected particularly clearly for a SN 2009ip-like event.
Conclusions
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 a luminous blue variable, for example. The detection of [O I] in the +405 d spectrum suggests some possible evidence of nucleosynthesised material generated in a SN explosion.
Ladattava julkaisu This is an electronic reprint of the original article. |  |
Julkaisussa olevat rahoitustiedot:
KKM and EK acknowledge financial support from the Emil Aaltonen foundation. SM acknowledges support from the Research Council of Finland project 350458. AR acknowledges financial support from the GRAWITA Large Program Grant (PI P. D’Avanzo). AR, AP and IS acknowledge financial support from the PRIN-INAF 2022 “Shedding light on the nature of gap transients: from the observations to the models”. SJB acknowledges their support by the European Research Council (ERC) under the European Union’s Horizon Europe research and innovation programme (grant agreement No. 10104229 - TransPIre) This work was funded by ANID, Millennium Science Initiative, ICN12_009. BAI acknowledges support from National Agency for Research and Development (ANID) grants ANID-PFCHA/Doctorado Nacional/21221964. PC acknowledges support via Research Council of Finland (grant 340613). TWC acknowledges the Yushan Fellow Program by the Ministry of Education, Taiwan for the financial support (MOE-111-YSFMS-0008-001-P1). MN is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 948381). CPG acknowledges financial support from the Secretary of Universities and Research (Government of Catalonia) and by the Horizon 2020 Research and Innovation Programme of the European Union under the Marie Skłodowska-Curie and the Beatriu de Pinós 2021 BP 00168 programme, from the Spanish Ministerio de Ciencia e Innovación (MCIN) and the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the PID2023-151307NB-I00 SNNEXT project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016 and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M, and from the Departament de Recerca i Universitats de la Generalitat de Catalunya through the 2021-SGR-01270 grant. TEMB is funded by Horizon Europe ERC grant no. 101125877. JLP acknowledges support from ANID, Millennium Science Initiative, AIM23-0001. TMR is part of the Cosmic Dawn Center (DAWN), which is funded by the Danish National Research Foundation under grant DNRF140. TMR acknowledges support from the Research Council of Finland project 350458. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of ePESSTO+ (the advanced Public ESO Spectroscopic Survey for Transient Objects Survey – PI: Inserra) and ePESSTO and PESSTO (PI: Smartt). ePESSTO+ observations were obtained under ESO program ID 1103.D-0328, while ePESSTO and PESSTO observations under ESO program IDs 097.D-0891, 191.D-0935 and 199.D-0143. This work makes use of observations from the Las Cumbres Observatory global telescope network. This research has made use of data obtained through the High Energy Astrophysics Science Archive Research Center online service, provided by the NASA/Goddard Space Flight Center. This project used public archival data from the Dark Energy Survey (DES). Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey.
