A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Explosion sites of SN 1994W-like transients
Tekijät: Kankare, E.; Kangas, T.; Fraser, M.; Mattila, S.; Pastorello, A.; Elias-Rosa, N.; Altavilla, G.; Benetti, S.; Kotak, R.; Matilainen, K.; Mäntynen, I.
Kustantaja: EDP Sciences
Julkaisuvuosi: 2025
Journal: Astronomy and Astrophysics
Tietokannassa oleva lehden nimi: Astronomy & Astrophysics
Artikkelin numero: A177
Vuosikerta: 699
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202554795
Verkko-osoite: https://doi.org/10.1051/0004-6361/202554795
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/499272885
We study a sample of narrow-line transients that share characteristics with the Type IIn classified supernova (SN) 1994W, a prototypical member of this class of events, via an investigation of their explosion sites and spectrophotometric data. The normalised cumulative rank (NCR) method was used to compare the explosion sites of ten events to the star formation distributions of their host galaxies, and to the sites of different evolved massive stars. The resulting sample mean value of NCRHα = 0.170±0.076 is low, while the NCRNUV distribution is flat with a mean value of 0.488±0.084. The NCR distribution of SN 1994W-like events is consistent with relatively low-mass red supergiants (RSGs) and, despite the small sample size, inconsistent with high-mass stars such as luminous blue variables. To explain the nature of SN 1994W-like transients, an interaction between an expanding ejecta and a relatively massive circumstellar medium is likely required, with the latter possibly having been produced by a H envelope ejection via a nuclear flash event, or a luminous red nova (LRN) from a stellar merger; both channels are consistent with the low-mass RSGs suggested by the NCR results. In this context, we find the early −26 d spectrum from light curve maximum of SN 2003G to have similarities to those of F8-type supergiant stars and LRNe. Finally, based on late-time HST imaging, we set the deepest limits for the surviving precursor of SN 2011ht to MF438W>−3.8 and MF555W>−4.0 mag. This would exclude most supergiants as a non-terminal progenitor, assuming that such a star is not completely obscured by newly formed dust.
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Julkaisussa olevat rahoitustiedot:
We thank the anonymous referee for useful comments. We thank Enrico Cappellaro, Luca Rizzi, Cristina Romero-Canizales, and Marilena Salvo for the help with some of the observations. EK acknowledges financial support from the Emil Aaltonen foundation. TK acknowledges support from the Research Council of Finland project 360274. SM acknowledges support from the Research Council of Finland project 350458. AP, NER, and SB acknowledge financial support from PRIN-INAF 2022 Shedding light on the nature of gap transients: from the observations to the models. NER acknowledges support from the Spanish Ministerio de Ciencia e Innovacion (MCIN) and the Agencia Estatal de Investigacion (AEI) 10.13039/501100011033 under the program Unidad de Excelencia Maria de Maeztu CEX2020-001058-M. RK acknowledges support from the Research Council of Finland project 340613. 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. 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 NOT. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 67.D-0594 and 164.H-0376. Based on observations collected at Copernico telescope (Asiago, Italy) of the INAF - Osservatorio Astronomico di Padova. Based on observations made with the WHT and INT operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This paper makes use of data obtained from the Isaac Newton Group of Telescopes Archive which is maintained as part of the CASU Astronomical Data Centre at the Institute of Astronomy, Cambridge. This research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs 6673, 8602, 9042, 9788, 12229, 13007, 14149, 14614, 14668, 15166, 15645, 16179, 16241, 16691, and 17070. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. gaia is a derivative of the Skycat catalogue and image display tool, developed as part of the VLT project at ESO. Skycat and gaia are free software under the terms of the GNU copyright. We have made use of the Weizmann interactive supernova data repository (www.weizmann.ac.il/astrophysics/wiserep). We have made use of the Ned Wright's cosmology calculator (Wright 2006, www.astro.ucla.edu/similar to wright/CosmoCalc.html).
