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Peer-reviewedCC BYAstronomy & Astrophysics

Wild behaviour near the finish line: The Type Ibn SN 2020able and its stratified environment

  • Tartaglia L.1
  • Cappellaro E.2
  • Valerin G.2
  • Pastorello A.2
  • Benetti S.2
  • Reguitti A.2
  • Tomasella L.2
  • Lundqvist P.3
  • Misra K.4
  • Gangopadhyay A.3
  • Dastidar R.5
  • Ailawadhi B.6
20 more authors
  • Dimple7
  • Kumar B.8
  • Jha V. K.9
  • Singh M.10
  • Elias-Rosa N.2
  • Gutiérrez C. P.11
  • Howell D. A.12
  • Hiramatsu D.13
  • Pellegrino C.14
  • Andrews J.15
  • Sand D. J.16
  • Smith N.16
  • Pearson J.16
  • Wyatt S.14
  • Ochner P.17
  • Cai Y.-Z.2
  • Burke J.18
  • McCully C.12
  • Newsome M.19
  • Padilla Gonzalez E.20
20 affiliations
  1. 1INAF – Osservatorio Astronomico d’Abruzzo
  2. 2INAF – Osservatorio Astronomico di Padova
  3. 3Oskar Klein Centre, Department of Astronomy, Stockholm University
  4. 4Aryabhatta Research Institute of Observational Sciences
  5. 5INAF – Osservatorio Astronomico di Brera
  6. 6Physical Research Laboratory
  7. 7School of Physics and Astronomy, University of Birmingham
  8. 8South-Western Institute for Astronomy Research, Yunnan University
  9. 9National Centre for Radio Astrophysics, Tata Institute of Fundamental Research
  10. 10Indian Institute of Astrophysics
  11. 11Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n
  12. 12Las Cumbres Observatory
  13. 13Department of Astronomy, University of Florida, Bryant Space Science Center
  14. 14NASA Goddard Space Flight Center
  15. 15Gemini Observatory/NSF’s National Optical-Infrared Astronomy Research Laboratory
  16. 16Steward Observatory, University of Arizona
  17. 17Università degli Studi di Padova, Dipartimento di Fisica e Astronomia
  18. 18Independent researcher
  19. 19Department of Astronomy, The University of Texas at Austin
  20. 20Department of Physics and Astronomy, Johns Hopkins University
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Abstract

We present spectrophotometric observations of the Type Ibn supernova SN 2020able, along with a comprehensive analysis and modelling of its evolution. The transient occurred in SDSS J092602.93+243115.1, a faint host galaxy characterised by significantly subsolar metallicity (12 + log(O/H) ≃ 8.28 dex). The early photometric evolution and high peak luminosity (Lpeak ≃ 4.4 × 1043 erg s−1) indicate an efficient conversion of ejecta kinetic energy into radiation via interaction with the circumstellar medium. Light-curve modelling suggests that this interaction involves ejecta with a mass of Mej ≃ 1.3 M☉ impacting a shell of MCSM ≃ 0.6 M☉. However, interaction is found to be geometrically and temporally confined within a few days after explosion, with the later evolution of the transient being dominated by the free expansion of the ejecta. Spectroscopic analysis reveals a complex, stratified, circumstellar environment. In addition to the innermost shocked region, we identify two additional He-rich shells: a dense inner one (ne ≃ 1.4 × 109 cm−3) located at R ≳ 9.3 × 1014 cm, and a more extended outer component reaching Rout ≃ 3.3 × 1015 cm and expanding at approximately 1.2 × 103 km s−1. The physical parameters of the former suggest it was produced by a discrete, pre-supernova eruptive event similar to that of SN 2006jc, which expelled approximately 1.8 × 10−2 M☉ of material. Conversely, the expansion velocity of the outermost shell is consistent with the escape velocity of Wolf–Rayet stars, pointing towards a late WN- to WC-type progenitor as the most viable candidate for SN 2020able.

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Cite

BibTeXRIS
BibTeX
@article{tartaglia2026wild,
  title = {{Wild behaviour near the finish line: The Type Ibn SN 2020able and its stratified environment}},
  author = {Tartaglia L. and Cappellaro E. and Valerin G. and Pastorello A. and Benetti S. and Reguitti A. and Tomasella L. and Lundqvist P. and Misra K. and Gangopadhyay A. and Dastidar R. and Ailawadhi B. and Dimple and Kumar B. and Jha V. K. and Singh M. and Elias-Rosa N. and Gutiérrez C. P. and Howell D. A. and Hiramatsu D. and Pellegrino C. and Andrews J. and Sand D. J. and Smith N. and Pearson J. and Wyatt S. and Ochner P. and Cai Y.-Z. and Burke J. and McCully C. and Newsome M. and Padilla Gonzalez E.},
  journal = {Astronomy \& Astrophysics},
  year = {2026},
  month = oct,
  doi = {10.1051/0004-6361/202660937},
  url = {https://doi.org/10.1051/0004-6361/202660937},
  note = {CC BY},
}
RIS
TY  - JOUR
TI  - Wild behaviour near the finish line: The Type Ibn SN 2020able and its stratified environment
AU  - Tartaglia L.
AU  - Cappellaro E.
AU  - Valerin G.
AU  - Pastorello A.
AU  - Benetti S.
AU  - Reguitti A.
AU  - Tomasella L.
AU  - Lundqvist P.
AU  - Misra K.
AU  - Gangopadhyay A.
AU  - Dastidar R.
AU  - Ailawadhi B.
AU  - Dimple
AU  - Kumar B.
AU  - Jha V. K.
AU  - Singh M.
AU  - Elias-Rosa N.
AU  - Gutiérrez C. P.
AU  - Howell D. A.
AU  - Hiramatsu D.
AU  - Pellegrino C.
AU  - Andrews J.
AU  - Sand D. J.
AU  - Smith N.
AU  - Pearson J.
AU  - Wyatt S.
AU  - Ochner P.
AU  - Cai Y.-Z.
AU  - Burke J.
AU  - McCully C.
AU  - Newsome M.
AU  - Padilla Gonzalez E.
PY  - 2026
DA  - 2026/10/31
JO  - Astronomy & Astrophysics
DO  - 10.1051/0004-6361/202660937
UR  - https://doi.org/10.1051/0004-6361/202660937
AB  - We present spectrophotometric observations of the Type Ibn supernova SN 2020able, along with a comprehensive analysis and modelling of its evolution. The transient occurred in SDSS J092602.93+243115.1, a faint host galaxy characterised by significantly subsolar metallicity (12 + log(O/H) ≃ 8.28 dex). The early photometric evolution and high peak luminosity (Lpeak ≃ 4.4 × 1043 erg s−1) indicate an efficient conversion of ejecta kinetic energy into radiation via interaction with the circumstellar medium. Light-curve modelling suggests that this interaction involves ejecta with a mass of Mej ≃ 1.3 M☉ impacting a shell of MCSM ≃ 0.6 M☉. However, interaction is found to be geometrically and temporally confined within a few days after explosion, with the later evolution of the transient being dominated by the free expansion of the ejecta. Spectroscopic analysis reveals a complex, stratified, circumstellar environment. In addition to the innermost shocked region, we identify two additional He-rich shells: a dense inner one (ne ≃ 1.4 × 109 cm−3) located at R ≳ 9.3 × 1014 cm, and a more extended outer component reaching Rout ≃ 3.3 × 1015 cm and expanding at approximately 1.2 × 103 km s−1. The physical parameters of the former suggest it was produced by a discrete, pre-supernova eruptive event similar to that of SN 2006jc, which expelled approximately 1.8 × 10−2 M☉ of material. Conversely, the expansion velocity of the outermost shell is consistent with the escape velocity of Wolf–Rayet stars, pointing towards a late WN- to WC-type progenitor as the most viable candidate for SN 2020able.
SN  - 0004-6361
SN  - 1432-0746
ER  -