| Title | 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 |
| Authors | Pastorello, A. Prieto, J. L. Elias-Rosa, N. Bersier, D. Hosseinzadeh, G. Morales-Garoffolo, A. Noebauer, U. M. Taubenberger, S. Tomasella, L. Kochanek, C. S. Falco, E. Basu, U. Beacom, J. F. Benetti, S. Brimacombe, J. Cappellaro, E. Danilet, A. B. Dong, Subo Fernandez, J. M. Goss, N. Granata, V. Harutyunyan, A. Holoien, T. W.S. Ishida, E. E. O. Kiyota, S. Krannich, G. Nicholls, B. Ochner, P. Pojmanski, G. Shappee, B. J. Simonian, G. V. Stanek, K. Z. Starrfield, S. Szczygiel, D. Tartaglia, L. Terreran, G. Th |
| Affiliation | INAF Osservatorio Astron Padova, I-35122 Padua, Italy. Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. Millennium Inst Astrophys, Santiago, Chile. Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. CSIC IEEC, Inst Ciencies Espai, E-08193 Cerdanyola Del Valles, Spain. Max Planck Inst Astrophys, D-85748 Garching, Germany. European Org Astron Res Southern Hemisphere ESO, D-85748 Garching, Germany. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Grove City High Sch, Grove City, OH 43123 USA. Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. Coral Towers Observ, Unit Coral Towers 38, Cairns CAIRNS, Australia. Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. Observ Inmaculada Molino, E-41640 Osuna, Spain. Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy. Fdn Galileo Galilei INAF, Telescopio Nazl Galileo, E-38712 Brena Baja, TF, Spain. Variable Star Observers League Japan, Chiba 2730126, Japan. Roof Observ Kaufering, D-86916 Kaufering, Germany. Mt Vernon Observ, Nelson 7010, New Zealand. Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland. Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. SOLO Observ, Port Wing, WI 54865 USA. Univ Minnesota, Dept Geol Sci, Duluth, MN 55812 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. |
| Keywords | supernovae: general supernovae: individual: ASASSN-15ed supernovae: individual: SN 1991D supernovae: individual: SN 2006jc supernovae: individual: SN 2010al WOLF-RAYET STARS DIGITAL SKY SURVEY CORE-COLLAPSE SUPERNOVAE SN 2006JC FUNDAMENTAL PARAMETERS DUST FORMATION WNL STARS EXPLOSION SPECTROSCOPY EXTINCTION |
| Issue Date | 2015 |
| Publisher | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY |
| Citation | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY.2015,453,(4),3649-3661. |
| 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 Super-Novae (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 M-r approximate to -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. |
| URI | http://hdl.handle.net/20.500.11897/415306 |
| ISSN | 0035-8711 |
| DOI | 10.1093/mnras/stv1812 |
| Indexed | SCI(E) |
| Appears in Collections: | 科维理天文与天体物理研究所 |
