A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
The Transitional Type Ibn/IIn SN 2022pda, with Pre-explosion Outbursts and a Double-peaked Light Curve; 
Tekijät: Cai, Y. -Z; Pastorello, A.; Chiba, R.; Moriya, T. J.; Reguitti, A.; Tartaglia, L.; Moran, S.; Campana, S.; Wang, Z. -Y; Zhao, J. -W; Anderson, J. P.; Benetti, S.; Brennan, S. J.; Cappellaro, E.; Chambers, K. C.; Chen, T. -W; Chen, Z. -H; de Boer, T.; Dong, Y. -Z; Duarte, J.; Elias-Rosa, N.; Fraser, M.; Gan, W. -P; Gao, H.; Gromadzki, M.; Hosseinzadeh, G.; Howell, D. A.; Inserra, C.; Kangas, T.; Kankare, E.; Kravtsov, T.; Li, L. -P; Lin, C. -C; Lowe, T. B.; Lundqvist, P.; Magnier, E. A.; Matilainen, K.; Mazzali, P. A.; McCully, C.; Minguez, P.; Muller-Bravo, T. E.; Newsome, M.; Padilla Gonzalez, E.; Pellegrino, C.; Pessi, P. J.; Petrushevska, T.; Pignata, G.; Santos, R. P.; Schulze, S.; Smartt, S. J.; Smith, I. A.; Smith, K. W.; Sollerman, J.; Srivastav, S.; Stritzinger, M. D.; Terreran, G.; Valerin, G.; Wainscoat, R.; Wang, S. -Q; Young, D. R.; Galbany, L.; Li, Z.; Salmaso, I.; Zha, S.; Bai, J. -M; Wang, B.; Wang, X. -F; Zhang, J. -J
Kustantaja: Institute of Physics Publishing
Julkaisuvuosi: 2026
Lehti: Astrophysical Journal Letters
Artikkelin numero: L37
Vuosikerta: 1004
Numero: 2
ISSN: 2041-8205
eISSN: 2041-8213
DOI: https://doi.org/10.3847/2041-8213/ae734e
Julkaisun avoimuus kirjaamishetkellä: Avoimesti saatavilla
Julkaisukanavan avoimuus : Kokonaan avoin julkaisukanava
Verkko-osoite: https://iopscience.iop.org/article/10.3847/2041-8213/ae734e
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/526992540
Rinnakkaistallenteen lisenssi: CC BY
Rinnakkaistallennetun julkaisun versio: Kustantajan versio
We report the results of a photometric and spectroscopic follow-up campaign of the unusual interacting supernova (SN) 2022pda. Precursor variability lasting ∼100 days is observed before the explosion. The SN light curve has a double-peak shape. It reached a first maximum of Mr = −19.6 ± 0.2 mag, followed by an initial 2 month decline and a second, broad peak lasting about 6 months. The early spectra show a blue continuum with dominant H and He emission lines. A high-resolution pre-maximum spectrum shows that the profile of the He i λ 5876 line consists of a moderately narrow (∼1900 km s−1) P Cygni absorption superposed on a broader (∼3300 km s−1) component. In the blue region, several spectral features are identified, including C iii/N iii/O ii blends. Two broad bumps at 4600–5200 Å and 6400–6800 Å regions reveal a complex profile, which are likely due to blends of H, He, and other emission lines. Late-time spectra are still dominated by prominent and broad H and He lines in emission. Shock-driven model fits to the bolometric light curve suggest that the SN is powered by interaction with a massive CSM with enhanced mass-loss rates ∼5 M⊙yr−1, expelled during two events that occurred ∼1 and ∼0.2 yr before the explosion. The overall SN evolution indicates that SN 2022pda is a transitional event between an H-rich SN IIn (SN 2009ip-like) and an He-rich SN Ibn. Our findings suggest that the progenitor was likely a luminous blue variable transitioning towards a Wolf–Rayet stage.
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We thank the anonymous referee for providing insightful comments and suggestions that improved the Letter. This work is supported by the B-type Strategic Priority Program of the Chinese Academy of Sciences (grant No. XDB1160202), the National Key R&D Program of China with grants 2021YFA1600404 and 2024YFA1611603, the National Natural Science Foundation of China (NSFC grants 12303054, 12173082, 12333008, 12288102, 12033003, and 11633002), the Yunnan Fundamental Research Projects (YFRP; grants 202401AU070063, 202501AV070012, 202501AS070078, and 202401BC070007), the Top-notch Young Talents Program of Yunnan Province, the Light of West China Program provided by the Chinese Academy of Sciences, and the International Centre of Supernovae (ICESUN), Yunnan Key Laboratory of Supernova Research (No. 202505AV340004). Y.-Z. Cai, A.R., G.V., and I.S. acknowledge financial support from the SOXS project (PI S. Campana). S.C. acknowledges funding from the Italian Space Agency (ASI/INAF Contract I/004/11/6. We thank M. Fulton, A. Gkini, S. C. Williams, and M.-X. Huang for their assistance with observations and for sharing their data. A.P., A.R., E.C., G.V., N.E.R., I.S., S.B., and L.T. acknowledge support from the PRIN-INAF 2022, “Shedding light on the nature of gap transients: from the observations to the models.” A.R. also acknowledges financial support from the GRAWITA Large Program grant (PI P. D’Avanzo). M.F. acknowledges financial support of Taighde Éireann—Research Ireland under grant No. 24/FFP-P/12959. T.E.M.B. is funded by Horizon Europe ERC grant No. 101125877. T.K. acknowledges support from the Research Council of Finland project 360274. T.-W.C. acknowledges the Yushan Fellow Program by the Ministry of Education, Taiwan for the financial support (MOE-111-YSFMS-0008-001-P1). S.J.B. acknowledge their support by the European Research Council (ERC) under the European Union’s Horizon Europe research and innovation program (grant agreement No. 10104229—TransPIre). J.D. and R.P.S. acknowledge support by FCT for CENTRA through grant No. UID/PRR/00099/2025 (https://doi.org/10.54499/UID/PRR/00099/2025) and grant No. UID/00099/2025 (https://doi.org/10.54499/UID/00099/2025). J.D. acknowledges support by FCT under the PhD grant 2023.01333.BD, with DOI https://doi.org/10.54499/2023.01333.BD. R.P.S. acknowledges support by FCT under the PhD grant 2024.03599.BD. L.G. acknowledges financial support from AGAUR, CSIC, MCIN, and AEI 10.13039/501100011033 under projects PID2023-151307NB-I00, PIE 20215AT016, CEX2020-001058-M, ILINK23001, COOPB2304, and 2021-SGR-01270. M.D. Stritzinger acknowledges support from the Independent Research Fund Denmark (IRFD; grant 10.46540/2032-00022B). T.P. acknowledges the financial support from the Slovenian Research Agency (grants I0-0033, P1-0031, J1-8136, J1-2460, and Z1-1853). S.Mo. is funded by Leverhulme Trust grant RPG-2023-240. S.Z. is supported by the National Natural Science Foundation of China (NSFC, grant No. 12473031), the Yunnan Fundamental Research Projects (grant No. 202501AS070078) X.F.W. is also supported by the Tencent Xplorer Prize. S.J.S. and K.W.S. acknowledge funding from STFC grants ST/Y001605/1 and ST/X001253/1, a Royal Society Research Professorship and the Hintze Family Charitable Foundation. This work was funded by ANID, Millennium Science Initiative, ICN12_009.
We acknowledge the support of the staffs of the various observatories at which data were obtained. 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). ePESSTO+ observations were obtained under ESO program IDs 108.220C and 111.24PR. Based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku, and the University of Oslo, representing Denmark, Finland, and Norway, the University of Iceland, and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Observations from the NOT were obtained through the NUTS2 collaboration which is supported in part by the Instrument Centre for Danish Astrophysics (IDA), and the Finnish Centre for Astronomy with ESO (FINCA) via Academy of Finland grant No. 306531. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. Funding for the LJT has been provided by Chinese Academy of Sciences and the People’s Government of Yunnan Province. The LJT is jointly operated and administrated by Yunnan Observatories and Center for Astronomical Mega-Science, CAS. Based on observations collected at Schmidt telescope (Asiago Mount Ekar, Italy) of the INAF—Osservatorio Astronomico di Padova. This work makes use of data from the Las Cumbres Observatory Network and the Global Supernova Project. The LCO team is supported by U.S. NSF grants AST-1911225 and AST-1911151. We acknowledge the use of public data from the ATLAS, Pan-STARRS, ZTF, Swift, and WISE data archive.
