Optical photometry and spectroscopy of the low-luminosity, broad-lined Ic supernova iPTF15dld

Creators: Pian, E.; Tomasella, L.; Cappellaro, E.; Benetti, S.; Mazzali, P. A.; Baltay, C.; Branchesi, M.; Brocato, E.; Campana, S.; Copperwheat, C.; Covino, S.; D'Avanzo, P.; Ellman, N.; Grado, A.; Melandri, A.; Palazzi, E.; Piascik, A.; Piranomonte, S.; Rabinowitz, D.; Raimondo, G.; Smartt, S. J.; Steele, I. A.; Stritzinger, M.; Yang, S.; Ascenzi, S.; Della Valle, M.; Gal-Yam, A.; Getman, F.; Greco, G.; Inserra, C.; Kankare, E.; Limatola, L.; Nicastro, L.; Pastorello, A.; Pulone, L.; Stamerra, A.; Stella, L.; Stratta, G.; Tartaglia, L.; Turatto, M.

Abstract

Core-collapse stripped-envelope supernova (SN) explosions reflect the diversity of physical parameters and evolutionary paths of their massive star progenitors. We have observed the Type Ic SN iPTF15dld (z = 0.047), reported by the Palomar Transient Factory. Spectra were taken starting 20 rest-frame days after maximum luminosity and are affected by a young stellar population background. Broad spectral absorption lines associated with the SN are detected over the continuum, similar to those measured for broad-lined, highly energetic SNe Ic. The light curve and maximum luminosity are instead more similar to those of low luminosity, narrow-lined Ic SNe. This suggests a behaviour whereby certain highly stripped-envelope SNe do not produce a large amount of ^(56)Ni, but the explosion is sufficiently energetic that a large fraction of the ejecta is accelerated to higher than usual velocities. We estimate SN iPTF15dld had a main-sequence progenitor of 20–25 M⊙, produced a ^(56)Ni mass of ∼0.1–0.2 M⊙, had an ejecta mass of [2–10] M⊙, and a kinetic energy of [1–18] × 10^(51) erg.

Additional Information

© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 December 9. Received 2016 December 8; in original form 2016 October 29. Published: 13 December 2016. We acknowledge data from the Pan-STARRS1 telescope that is supported by NASA under grant no. NNX12AR65G and grant no. NNX14AM74G issued through the NEO Observation Program. We acknowledge funding from ASI INAF grant I/088/06/0, from the Italian Ministry of Education and Research and the Scuola Normale Superiore, and from INAF project: 'Gravitational Wave Astronomy with the first detections of aLIGO and aVIRGO experiments' (PI: E. Brocato). GR is partially supported by the PRIN INAF-2014 'EXCALIBURS: EXtragalactic distance scale CALIBration Using first-Rank Standard candles' (PI: G. Clementini). L. Tomasella, EC and SB are partially supported by the PRIN-INAF 2014 project 'Transient Universe: unveiling new types of stellar explosions with PESSTO'. MS gratefully acknowledges generous support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant. MB, GG and GS acknowledge financial support from the Italian Ministry of Education, University and Research (MIUR) through grant FIRB 2012 RBFR12PM1F. We thank the staff of the Copernico telescope, LT, NTT, TNG, NOT and LSQ, in particular W. Boschin, D. Carosati, S. Dalle Ave, L. Di Fabrizio, A. Fiorenzano, P. Ochner, T. Pursimo and T. Reynolds. We are grateful to S. Valenti for sending archival supernova data in digital form, P. Nugent for his support of this project, L. Singer for his critical reading of the manuscript and to our referee for constructive suggestions. This research is based on observations made with the Copernico telescope (Asiago, Italy) of INAF - Osservatorio Astronomico di Padova; with the NTT at the European Organization for Astronomical Research in the Southern hemisphere, Chile, as part of the Public ESO Spectroscopic Survey for Transient Objects Survey (PESSTO) ESO programmes 188.D-3003, 191.D-0935; with the Telescopio Nazionale Galileo, operated by the Fundación Galileo Galilei of INAF, with the Liverpool Telescope, operated by Liverpool John Moores University with financial support from the UK Science and Technology Facilities Council, and with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association, all three on the island of La Palma at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. This research has made use of the Weizmann Interactive Supernova data Repository (http://wiserep.weizmann.ac.il), and it used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231.

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