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DES16C3cje: a low-luminosity, long-lived supernova

Gutiérrez, C. P., Sullivan, M., Martinez, L., Bersten, M. C., Inserra, C., Smith, M., Anderson, J. P., Pan, Y. -C., Pastorello, A., Galbany, L., Nugent, P., Angus, C. R., Barbarino, C., Carollo, D., Chen, T. -W., Davis, T. M., Valle, M. Della, Foley, R. J., Fraser, M., Frohmaier, C., González-Gaitán, S., Gromadzki, M., Kankare, E., Kokotanekova, R., Kollmeier, J., Lewis, G. F., Magee, M. R., Maguire, K., Möller, A., Morrell, N., Nicholl, M., Pursiainen, M., Sollerman, J., Sommer, N. E., Swann, E., Tucker, B. E., Wiseman, P., Aguena, M., Allam, S., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Morganson, E., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R. and Wilkinson, R. 2020. DES16C3cje: a low-luminosity, long-lived supernova. Monthly Notices of the Royal Astronomical Society 496 (1) , pp. 95-110. 10.1093/mnras/staa1452

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Abstract

We present DES16C3cje, a low-luminosity, long-lived type II supernova (SN II) at redshift 0.0618, detected by the Dark Energy Survey (DES). DES16C3cje is a unique SN. The spectra are characterized by extremely narrow photospheric lines corresponding to very low expansion velocities of ≲1500 km s−1, and the light curve shows an initial peak that fades after 50 d before slowly rebrightening over a further 100 d to reach an absolute brightness of Mr ∼ −15.5 mag. The decline rate of the late-time light curve is then slower than that expected from the powering by radioactive decay of 56Co, but is comparable to that expected from accretion power. Comparing the bolometric light curve with hydrodynamical models, we find that DES16C3cje can be explained by either (i) a low explosion energy (0.11 foe) and relatively large 56Ni production of 0.075 M⊙ from an ∼15 M⊙ red supergiant progenitor typical of other SNe II, or (ii) a relatively compact ∼40 M⊙ star, explosion energy of 1 foe, and 0.08 M⊙ of 56Ni. Both scenarios require additional energy input to explain the late-time light curve, which is consistent with fallback accretion at a rate of ∼0.5 × 10−8 M⊙ s−1.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Publisher: Oxford University Press
ISSN: 0035-8711
Date of First Compliant Deposit: 16 June 2020
Date of Acceptance: 21 May 2020
Last Modified: 17 Jun 2020 11:45
URI: http://orca.cf.ac.uk/id/eprint/132495

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