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Pastorello, A, Prieto, JL, Elias-Rosa, N, Bersier, D, Hosseinzadeh, G, Morales-Garoffolo, A, Noebauer, UM, Taubenberger, S, Tomasella, L, Kochanek, CS, Falco, E, Basu, U, Beacom, JF, Benetti, S, Brimacombe, J, Cappellaro, E, Danilet, AB, Dong, S, Fernandez, JM, Goss, N , Granata, V, Harutyunyan, A, Holoien, TW-S, Ishida, EEO, Kiyota, S, Krannich, G, Nicholls, B, Ochner, P, Pojmanski, G, Shappee, BJ, Simonian, GV, Stanek, KZ, Starrfield, S, Szczygiel, D, Tartaglia, L, Terreran, G, Thompson, TA, Turatto, M, Wagner, RM, Wiethoff, WS, Wilber, A and Wozniak, PR (2015) Massive stars exploding in a He-rich circumstellar medium - VII. The metamorphosis of ASASSN-15ed from a narrow line Type Ibn to a normal Type Ib Supernova. Monthly Notices of the Royal Astronomical Society, 453 (4). pp. 3649-3661. ISSN 0035-8711
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Abstract
We present the results of the spectroscopic and photometric monitoring campaign of ASASSN-15ed. The transient was discovered quite young by the All Sky Automated Survey for SuperNovae (ASAS-SN) survey. Amateur astronomers allowed us to sample the photometric SN evolution around maximum light, which we estimate to have occurred on JD = 2457087.4 ± 0.6 in the r band. Its apparent r-band magnitude at maximum was r = 16.91 ± 0.10, providing an absolute magnitude Mr ≈ −20.04 ± 0.20, which is slightly more luminous than the typical magnitudes estimated for Type Ibn SNe. The post-peak evolution was well monitored, and the decline rate (being in most bands around 0.1 mag d−1 during the first 25 d after maximum) is marginally slower than the average decline rates of SNe Ibn during the same time interval. The object was initially classified as a Type Ibn SN because early-time spectra were characterized by a blue continuum with superimposed narrow P-Cygni lines of He I, suggesting the presence of a slowly moving (1200–1500 km s−1), He-rich circumstellar medium. Later on, broad P-Cygni He I lines became prominent. The inferred velocities, as measured from the minimum of the broad absorption components, were between 6000 and 7000 km s−1. As we attribute these broad features to the SN ejecta, this is the first time we have observed the transition of a Type Ibn SN to a Type Ib SN.
| Item Type: | Article |
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| Additional Information: | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 the Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
| Uncontrolled Keywords: | 0201 Astronomical And Space Sciences |
| Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
| Divisions: | Astrophysics Research Institute |
| Publisher: | Oxford University Press |
| Related URLs: | |
| Date Deposited: | 28 Nov 2016 11:26 |
| Last Modified: | 03 Aug 2022 09:14 |
| DOI or ID number: | 10.1093/mnras/stv1812 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/4878 |
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