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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

Pastorello, A and Prieto, JL and Elias-Rosa, N and Bersier, D and Hosseinzadeh, G and Morales-Garoffolo, A and Noebauer, UM and Taubenberger, S and Tomasella, L and Kochanek, CS and Falco, E and Basu, U and Beacom, JF and Benetti, S and Brimacombe, J and Cappellaro, E and Danilet, AB and Dong, S and Fernandez, JM and Goss, N and Granata, V and Harutyunyan, A and Holoien, TW-S and Ishida, EEO and Kiyota, S and Krannich, G and Nicholls, B and Ochner, P and Pojmanski, G and Shappee, BJ and Simonian, GV and Stanek, KZ and Starrfield, S and Szczygiel, D and Tartaglia, L and Terreran, G and Thompson, TA and Turatto, M and Wagner, RM and Wiethoff, WS and 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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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
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: 11 Sep 2017 22:02
DOI or Identification number: 10.1093/mnras/stv1812
URI: http://researchonline.ljmu.ac.uk/id/eprint/4878

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