TY - JOUR
T1 - SN 2009ip at late times - An interacting transient at +2 years
AU - Fraser, M
AU - Kotak, R
AU - Pastorello, A
AU - Jerkstrand, A
AU - Smartt, SJ
AU - Chen, TW
AU - Childress, M
AU - Gilmore, G
AU - Inserra, C
AU - Kankare, E
AU - Margheim, S
AU - Mattila, S
AU - Valenti, S
AU - Ashall, Christopher
AU - Benetti, Stefano
AU - Botticella, Maria-Teresa
AU - Erik Bauer, Franz
AU - Campbell, Heather
AU - Elias-Rosa, Nancy
AU - Fleury, Mathilde
AU - Gal-Yam, Avishay
AU - Hachinger, Stephan
AU - Howell, D. Andrew
AU - Le Guillou, Laurent
AU - Léget, Pierre-François
AU - Morales-Garoffolo, Antonia
AU - Polshaw, Joe
AU - Spiro, Susanna
AU - Sullivan, Mark
AU - Taubenberger, Stefan
AU - Turatto, Massimo
AU - Walker, Emma S.
AU - Young, David R.
AU - Zhang, Bonnie
N1 - European Organization for Astronomical Research in the Southern hemisphere, Chile as part of ESO [291.D-5010, 092.D-0586]; European Organization for Astronomical Research in the Southern hemisphere, Chile part of PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects Survey), ESO program [188.D-3003/191.D-0935]; NASA [90255]; UK Science and Technology Facilities Council; W. M. Keck Foundation; European Union FP7 programme through ERC [320360]; STFC [ST/L000709/1, ST/I001123/1]; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; European Research Council under the European Union's Seventh Framework Programme (FP7)/ERC [291222]; Spanish Ministerio de Economia y competitividad (MINECO) [ESP2013-41268-R]; EU/FP7-ERC [307260]; 'The Quantum Universe' I-Core program by the Israeli Committee for planning and budgeting; ISF; GIF; Minerva; Weizmann-UK; Kimmel award; CONICYT-Chile [Basal-CATA PFB-06/2007, FONDECYT 1141218, PCCI 130074]; 'Millennium Institute of Astrophysics (MAS)' - Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009]; Minerva ARCHES award of the German Ministry of Education and Research (BMBF); PRIN-INAF; project 'Transient Universe: from ESO Large to PESSTO'; European Union Seventh Framework Programme (FP7), 'Astronomy Fellowships in Italy' (AstroFIt) [267251] Based on observations collected at the European Organization for Astronomical Research in the Southern hemisphere, Chile as part of ESO programmes 291.D-5010 and 092.D-0586, and as part of PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects Survey), ESO program 188.D-3003/191.D-0935. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA (Proposal ID 90255). Based on observations (GS-2013A-DD-3 and GS-2012B-Q-86) obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. This work makes use of observations from the LCOGT network. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mo
PY - 2015/11/11
Y1 - 2015/11/11
N2 - We present photometric and spectroscopic observations of the interacting transient SN 2009ip taken during the 2013 and 2014 observing seasons.We characterize the photometric evolution as a steady and smooth decline in all bands, with a decline rate that is slower than expected for a solely 56Co-powered supernova at late phases. No further outbursts or eruptions were seen over a two year period from 2012 December until 2014 December. SN 2009ip remains brighter than its historic minimum from pre-discovery images. Spectroscopically, SN 2009ip continues to be dominated by strong, narrow (≲2000 km s-1) emission lines of H, He, Ca, and Fe. While we make tenuous detections of [Fe II] λ7155 and [O I] λλ6300, 6364 lines at the end of 2013 June and the start of 2013 October, respectively, we see no strong broad nebular emission lines that could point to a core-collapse origin. In general, the lines appear relatively symmetric, with the exception of our final spectrum in 2014 May, when we observe the appearance of a redshifted shoulder of emission at +550 km s-1. The lines are not blueshifted, and we see no significant near- or mid-infrared excess. From the spectroscopic and photometric evolution of SN 2009ip until 820 d after the start of the 2012a event, we still see no conclusive evidence for core-collapse, although whether any such signs could be masked by ongoing interaction is unclear.
AB - We present photometric and spectroscopic observations of the interacting transient SN 2009ip taken during the 2013 and 2014 observing seasons.We characterize the photometric evolution as a steady and smooth decline in all bands, with a decline rate that is slower than expected for a solely 56Co-powered supernova at late phases. No further outbursts or eruptions were seen over a two year period from 2012 December until 2014 December. SN 2009ip remains brighter than its historic minimum from pre-discovery images. Spectroscopically, SN 2009ip continues to be dominated by strong, narrow (≲2000 km s-1) emission lines of H, He, Ca, and Fe. While we make tenuous detections of [Fe II] λ7155 and [O I] λλ6300, 6364 lines at the end of 2013 June and the start of 2013 October, respectively, we see no strong broad nebular emission lines that could point to a core-collapse origin. In general, the lines appear relatively symmetric, with the exception of our final spectrum in 2014 May, when we observe the appearance of a redshifted shoulder of emission at +550 km s-1. The lines are not blueshifted, and we see no significant near- or mid-infrared excess. From the spectroscopic and photometric evolution of SN 2009ip until 820 d after the start of the 2012a event, we still see no conclusive evidence for core-collapse, although whether any such signs could be masked by ongoing interaction is unclear.
UR - http://www.scopus.com/inward/record.url?scp=84960966867&partnerID=8YFLogxK
U2 - 10.1093/mnras/stv1919
DO - 10.1093/mnras/stv1919
M3 - مقالة
SN - 0035-8711
VL - 453
SP - 3886
EP - 3905
JO - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
JF - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
IS - 4
ER -