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., Baal, B. F. A. v., Jerkstrand, A., Dong, Y., 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., Christy, C., Chen, L., Davis, K. W., Esamdin, A., Farah, J., Foley, R. J., Hoang, E., Hosseinzadeh, G., Howell, D. A., Hsu, B., Huang, R., Iskander, A., Janzen, D., Jha, S. W., Kaur, R., Lundquist, M. J., McCully, C., Mehta, D., Ni, Y. Q., Retamal, N. M., Patra, K. C., Ransome, C., Shrestha, M., Smith, N., Subrayan, B., Taggart, K., Wang, X., Wynn, K., Yang, Y., Yan, S., Zheng, W., & Coe, D. January, 2026. arXiv:2601.00415 [astro-ph]
The Double-Peaked Calcium-Strong SN 2025coe: Progenitor Constraints from Early Interaction and Ejecta Asymmetries [link]Paper  doi  abstract   bibtex   
Supernova (SN) 2025coe at a distance of ∼25 Mpc is the third-closest calcium-strong (CaST) 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 ≲ 8 × 1014 cm), or a combination of both. The second peak is dominated by radioactive decay of 56Ni (Mej ≈ 0.4–0.5 M⊙; M56Ni ≈ 1.4 × 10−2 M⊙).
@misc{ravi_double-peaked_2026,
	title = {The {Double}-{Peaked} {Calcium}-{Strong} {SN} 2025coe: {Progenitor} {Constraints} from {Early} {Interaction} and {Ejecta} {Asymmetries}},
	shorttitle = {The {Double}-{Peaked} {Calcium}-{Strong} {SN} 2025coe},
	url = {http://arxiv.org/abs/2601.00415},
	doi = {10.48550/arXiv.2601.00415},
	abstract = {Supernova (SN) 2025coe at a distance of ∼25 Mpc is the third-closest calcium-strong (CaST) 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 ≲ 8 × 1014 cm), or a combination of both. The second peak is dominated by radioactive decay of 56Ni (Mej ≈ 0.4–0.5 M⊙; M56Ni ≈ 1.4 × 10−2 M⊙).},
	language = {en},
	urldate = {2026-01-13},
	publisher = {arXiv},
	author = {Ravi, Aravind P. and Kumar, Sahana and Baer-Way, Raphael and Valenti, Stefano and Modjaz, Maryam and Baal, Bart F. A. van and Jerkstrand, Anders and Dong, Yize 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 Christy, Collin and Chen, Liyang 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 Iskander, Abdusamatjan and Janzen, Daryl and Jha, Saurabh W. and Kaur, Ravjit and Lundquist, Michael J. and McCully, Curtis and Mehta, Darshana and Ni, Yuan Qi and Retamal, Nicolas Meza 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 Yang, Yi and Yan, Shengyu and Zheng, Weikang and Coe, Dan},
	month = jan,
	year = {2026},
	note = {arXiv:2601.00415 [astro-ph]},
	keywords = {Astrophysics - High Energy Astrophysical Phenomena, Explorable},
}
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