The Double-peaked Calcium-strong SN 2025coe: Progenitor Constraints from Early Interaction and Ejecta Asymmetries. Ravi, A. P., Kumar, S., Baer-Way, R., Valenti, S., Modjaz, M., Van Baal, B. F. A., Jerkstrand, A., Dong 董, Y. 一., Kwok, L. A., Pearson, J., Sand, D. J., Hiramatsu, D., Filippenko, A. V., Andrews, J., Andrews, M., Arunachalam, P., Bostroem, K. A., Brink, T. G., Chen, L., Christy, C., Davis, K. W., Esamdin, A., Farah, J., Foley, R. J., Hoang, E., Hosseinzadeh, G., Howell, D. A., Hsu, B., Huang, R., Iskandar, A., Janzen, D., Jha, S. W., Kaur, R., Lundquist, M. J., McCully, C., Mehta, D., Retamal, N. M., Ni, Y. Q., Patra, K. C., Ransome, C., Shrestha, M., Smith, N., Subrayan, B., Taggart, K., Wang, X., Wynn, K., Yan, S., Yang 杨, Y. 轶, Zheng, W., & Coe, D. The Astrophysical Journal, 1003(1):33, May, 2026. ![The Double-peaked Calcium-strong SN 2025coe: Progenitor Constraints from Early Interaction and Ejecta Asymmetries [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex Supernova (SN) 2025coe at a distance of ∼25 Mpc is the second-closest calcium-strong transient. It was discovered at a large projected offset of ∼34 kpc from its potential host galaxy NGC 3277. Multiband photometry of SN 2025coe indicates the presence of two peaks at day ∼2 and day ∼11 after explosion. Modeling the bolometric light curve, we find that the first peak can be reproduced either by shock cooling of a compact envelope (Renv ≈6–40 R⊙; Menv ≈0.1–0.2 M⊙) or by interaction with close-in circumstellar material (CSM; RCSM ≲ 6 × 1014 cm), or a combination of both. The second peak is dominated by radioactive decay of 56Ni (Mej ≈ 0.4–0.5 M⊙; M⊙). SN 2025coe rapidly evolves from the photospheric phase dominated by He I P Cygni profiles to nebular phase spectra dominated by strong [Ca ii] λλ7291, 7323 and weak [O i] λλ6300, 6364 emission lines. Simultaneous line profile modeling of [Ca ii] and [O i] at nebular phases shows that an asymmetric core-collapse explosion of a low-mass (≲3.3 M⊙) He-core progenitor can explain the observed line profiles. Alternatively, lack of local star formation at the site of the SN explosion combined with a low ejecta mass is also consistent with a thermonuclear explosion due to a low-mass hybrid He-C/O white dwarf +C/O white dwarf merger.
@article{ravi_double-peaked_2026,
title = {The {Double}-peaked {Calcium}-strong {SN} 2025coe: {Progenitor} {Constraints} from {Early} {Interaction} and {Ejecta} {Asymmetries}},
volume = {1003},
issn = {0004-637X, 1538-4357},
shorttitle = {The {Double}-peaked {Calcium}-strong {SN} 2025coe},
url = {https://iopscience.iop.org/article/10.3847/1538-4357/ae5b6e},
doi = {10.3847/1538-4357/ae5b6e},
abstract = {Supernova (SN) 2025coe at a distance of ∼25 Mpc is the second-closest calcium-strong transient. It was discovered at a large projected offset of ∼34 kpc from its potential host galaxy NGC 3277. Multiband photometry of SN 2025coe indicates the presence of two peaks at day ∼2 and day ∼11 after explosion. Modeling the bolometric light curve, we find that the first peak can be reproduced either by shock cooling of a compact envelope (Renv ≈6–40 R⊙; Menv ≈0.1–0.2 M⊙) or by interaction with close-in circumstellar material (CSM; RCSM ≲ 6 × 1014 cm), or a combination of both. The second peak is dominated by radioactive decay of 56Ni (Mej ≈ 0.4–0.5 M⊙; M⊙). SN 2025coe rapidly evolves from the photospheric phase dominated by He I P Cygni profiles to nebular phase spectra dominated by strong [Ca ii] λλ7291, 7323 and weak [O i] λλ6300, 6364 emission lines. Simultaneous line profile modeling of [Ca ii] and [O i] at nebular phases shows that an asymmetric core-collapse explosion of a low-mass (≲3.3 M⊙) He-core progenitor can explain the observed line profiles. Alternatively, lack of local star formation at the site of the SN explosion combined with a low ejecta mass is also consistent with a thermonuclear explosion due to a low-mass hybrid He-C/O white dwarf +C/O white dwarf merger.},
language = {en},
number = {1},
urldate = {2026-05-14},
journal = {The Astrophysical Journal},
author = {Ravi, Aravind P. and Kumar, Sahana and Baer-Way, Raphael and Valenti, Stefano and Modjaz, Maryam and Van Baal, Bart F. A. and Jerkstrand, Anders and Dong 董, Yize 一泽 and Kwok, Lindsey A. and Pearson, Jeniveve and Sand, David J. and Hiramatsu, Daichi and Filippenko, Alexei V. and Andrews, Jennifer and Andrews, Moira and Arunachalam, Prasiddha and Bostroem, K. Azalee and Brink, Thomas G. and Chen, Liyang and Christy, Collin and Davis, Kyle W. and Esamdin, Ali and Farah, Joseph and Foley, Ryan J. and Hoang, Emily and Hosseinzadeh, Griffin and Howell, D. Andrew and Hsu, Brian and Huang, Ruifeng and Iskandar, Abdusamatjan and Janzen, Daryl and Jha, Saurabh W. and Kaur, Ravjit and Lundquist, Michael J. and McCully, Curtis and Mehta, Darshana and Retamal, Nicolás Meza- and Ni, Yuan Qi and Patra, Kishore C. and Ransome, Conor and Shrestha, Manisha and Smith, Nathan and Subrayan, Bhagya and Taggart, Kirsty and Wang, Xiaofeng and Wynn, Kathryn and Yan, Shengyu and Yang 杨, Yi 轶 and Zheng, Weikang and Coe, Dan},
month = may,
year = {2026},
keywords = {SYS: CosmicAI Contact Author, Use-Inspired, WG: Explorable},
pages = {33},
}
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Modeling the bolometric light curve, we find that the first peak can be reproduced either by shock cooling of a compact envelope (Renv ≈6–40 R⊙; Menv ≈0.1–0.2 M⊙) or by interaction with close-in circumstellar material (CSM; RCSM ≲ 6 × 1014 cm), or a combination of both. The second peak is dominated by radioactive decay of 56Ni (Mej ≈ 0.4–0.5 M⊙; M⊙). SN 2025coe rapidly evolves from the photospheric phase dominated by He I P Cygni profiles to nebular phase spectra dominated by strong [Ca ii] λλ7291, 7323 and weak [O i] λλ6300, 6364 emission lines. Simultaneous line profile modeling of [Ca ii] and [O i] at nebular phases shows that an asymmetric core-collapse explosion of a low-mass (≲3.3 M⊙) He-core progenitor can explain the observed line profiles. 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CosmicAI Contact Author, Use-Inspired, WG: Explorable","pages":"33","bibtex":"@article{ravi_double-peaked_2026,\n\ttitle = {The {Double}-peaked {Calcium}-strong {SN} 2025coe: {Progenitor} {Constraints} from {Early} {Interaction} and {Ejecta} {Asymmetries}},\n\tvolume = {1003},\n\tissn = {0004-637X, 1538-4357},\n\tshorttitle = {The {Double}-peaked {Calcium}-strong {SN} 2025coe},\n\turl = {https://iopscience.iop.org/article/10.3847/1538-4357/ae5b6e},\n\tdoi = {10.3847/1538-4357/ae5b6e},\n\tabstract = {Supernova (SN) 2025coe at a distance of ∼25 Mpc is the second-closest calcium-strong transient. It was discovered at a large projected offset of ∼34 kpc from its potential host galaxy NGC 3277. Multiband photometry of SN 2025coe indicates the presence of two peaks at day ∼2 and day ∼11 after explosion. Modeling the bolometric light curve, we find that the first peak can be reproduced either by shock cooling of a compact envelope (Renv ≈6–40 R⊙; Menv ≈0.1–0.2 M⊙) or by interaction with close-in circumstellar material (CSM; RCSM ≲ 6 × 1014 cm), or a combination of both. The second peak is dominated by radioactive decay of 56Ni (Mej ≈ 0.4–0.5 M⊙; M⊙). SN 2025coe rapidly evolves from the photospheric phase dominated by He I P Cygni profiles to nebular phase spectra dominated by strong [Ca ii] λλ7291, 7323 and weak [O i] λλ6300, 6364 emission lines. Simultaneous line profile modeling of [Ca ii] and [O i] at nebular phases shows that an asymmetric core-collapse explosion of a low-mass (≲3.3 M⊙) He-core progenitor can explain the observed line profiles. Alternatively, lack of local star formation at the site of the SN explosion combined with a low ejecta mass is also consistent with a thermonuclear explosion due to a low-mass hybrid He-C/O white dwarf +C/O white dwarf merger.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2026-05-14},\n\tjournal = {The Astrophysical Journal},\n\tauthor = {Ravi, Aravind P. and Kumar, Sahana and Baer-Way, Raphael and Valenti, Stefano and Modjaz, Maryam and Van Baal, Bart F. A. and Jerkstrand, Anders and Dong 董, Yize 一泽 and Kwok, Lindsey A. and Pearson, Jeniveve and Sand, David J. and Hiramatsu, Daichi and Filippenko, Alexei V. and Andrews, Jennifer and Andrews, Moira and Arunachalam, Prasiddha and Bostroem, K. Azalee and Brink, Thomas G. and Chen, Liyang and Christy, Collin and Davis, Kyle W. and Esamdin, Ali and Farah, Joseph and Foley, Ryan J. and Hoang, Emily and Hosseinzadeh, Griffin and Howell, D. Andrew and Hsu, Brian and Huang, Ruifeng and Iskandar, Abdusamatjan and Janzen, Daryl and Jha, Saurabh W. and Kaur, Ravjit and Lundquist, Michael J. and McCully, Curtis and Mehta, Darshana and Retamal, Nicolás Meza- and Ni, Yuan Qi and Patra, Kishore C. and Ransome, Conor and Shrestha, Manisha and Smith, Nathan and Subrayan, Bhagya and Taggart, Kirsty and Wang, Xiaofeng and Wynn, Kathryn and Yan, Shengyu and Yang 杨, Yi 轶 and Zheng, Weikang and Coe, Dan},\n\tmonth = may,\n\tyear = {2026},\n\tkeywords = {SYS: CosmicAI Contact Author, Use-Inspired, WG: Explorable},\n\tpages = {33},\n}\n\n\n\n\n\n\n\n","author_short":["Ravi, A. P.","Kumar, S.","Baer-Way, R.","Valenti, S.","Modjaz, M.","Van Baal, B. F. A.","Jerkstrand, A.","Dong 董, Y. 一.","Kwok, L. A.","Pearson, J.","Sand, D. J.","Hiramatsu, D.","Filippenko, A. V.","Andrews, J.","Andrews, M.","Arunachalam, P.","Bostroem, K. A.","Brink, T. G.","Chen, L.","Christy, C.","Davis, K. W.","Esamdin, A.","Farah, J.","Foley, R. 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