| Full text | |
| Author(s): Show less - |
Davis, K. W.
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Taggart, K.
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Tinyanont, S.
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Foley, R. J.
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Villar, V. A.
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Izzo, L.
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Angus, C. R.
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Bustamante-Rosell, M. J.
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Coulter, D. A.
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Earl, N.
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Farias, D.
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Hjorth, J.
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Huber, M. E.
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Jones, D. O.
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Kelly, P. L.
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Kilpatrick, C. D.
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Langeroodi, D.
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Miao, H-Y
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Pellegrino, C. M.
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Ramirez-Ruiz, E.
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Ransome, C. L.
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Rest, S.
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Siebert, M. R.
;
Terreran, G.
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Thornton, I. M.
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Yadavalli, S. K.
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Zeimann, G. R.
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Auchettl, K.
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Bom, C. R.
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Brink, T. G.
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Burke, J.
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Camacho-Neves, Y.
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Chambers, K. C.
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de Boer, T. J. L.
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DeMarchi, L.
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Filippenko, A. V.
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Galbany, L.
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Gall, C.
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Gao, H.
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Herpich, F. R.
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Howell, D. A.
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Jacobson-Galan, W. V.
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Jha, S. W.
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Kanaan, A.
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Khetan, N.
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Kwok, L. A.
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Lai, Z.
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Larison, C.
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Lin, C-C
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Loertscher, K. C.
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Magnier, E. A.
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McCully, C.
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McGill, P.
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Newsome, M.
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Padilla Gonzalez, E.
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Pan, Y-C
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Rest, A.
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Rho, J.
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Ribeiro, T.
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Santos, A.
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Schoenell, W.
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Sharief, S. N.
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Smith, K. W.
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Wainscoat, R. J.
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Wang, Q.
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Zenati, Y.
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Zheng, W.
Total Authors: 67
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| Document type: | Journal article |
| Source: | Monthly Notices of the Royal Astronomical Society; v. 523, n. 2, p. 21-pg., 2023-05-30. |
| Abstract | |
We present optical and near-infrared (NIR) observations of the Type Icn supernova (SN Icn) 2022ann, the fifth member of its newly identified class of SNe. Its early optical spectra are dominated by narrow carbon and oxygen P-Cygni features with absorption velocities of similar to 800 km s(-1); slower than other SNe Icn and indicative of interaction with a dense, H/He-poor circumstellar medium (CSM) that is outflowing slower than typical Wolf-Rayet wind velocities of >1000 km s(-1). We identify helium in NIR spectra 2 weeks after maximum and in optical spectra at 3 weeks, demonstrating that the CSM is not fully devoid of helium. Unlike other SNe Icn, the spectra of SN 2022ann never develop broad features from SN ejecta, including in the nebular phase. Compared to other SNe Icn, SN 2022ann has a low luminosity (o-band absolute magnitude of similar to-17.7), and evolves slowly. The bolometric light curve is well-modelled by 4.8 M-circle dot of SN ejecta interacting with 1.3 M-circle dot of CSM. We place an upper limit of 0.04 M-circle dot of Ni-56 synthesized in the explosion. The host galaxy is a dwarf galaxy with a stellar mass of 10(7.34) M-circle dot (implied metallicity of log(Z/Z(circle dot)) approximate to 0.10) and integrated star-formation rate of log(SFR) = -2.20 M-circle dot yr(-1); both lower than 97 percent of galaxies observed to produce core-collapse supernovae, although consistent with star-forming galaxies on the galaxy Main Sequence. The low CSM velocity, nickel and ejecta masses, and likely low-metallicity environment disfavour a single Wolf-Rayet progenitor star. Instead, a binary companion is likely required to adequately strip the progenitor and produce a low-velocity outflow. (AU) | |
| FAPESP's process: | 18/21661-9 - Cataloguing Variable Sources and IFU-like Science with Multiband Surveys. |
| Grantee: | Fábio Rafael Herpich |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |
| FAPESP's process: | 21/11345-5 - Search for asteroids in S-PLUS using THOR |
| Grantee: | Fábio Rafael Herpich |
| Support Opportunities: | Scholarships abroad - Research Internship - Post-doctor |