Weizmann Inst. of Science, Rehovot (Israel). Dept. of Particle Physics and Astrophysics
Weizmann Inst. of Science, Rehovot (Israel). Dept. of Particle Physics and Astrophysics; Univ. of Copenhagen (Denmark). The Niels Bohr Inst., Dark Cosmology Centre
Weizmann Inst. of Science, Rehovot (Israel). Dept. of Particle Physics and Astrophysics; European Southern Observatory, Garching (Germany)
Univ. of Copenhagen (Denmark). The Niels Bohr Inst., Dark Cosmology Centre; California Inst. of Technology (CalTech), Pasadena, CA (United States). Cahill Center for Astrophysics
San Diego State Univ., San Diego, CA (United States). Dept. of Astronomy; Univ. of Tokyo (Japan). Kavli IPMU (WPI), UTIAS
Weizmann Inst. of Science, Rehovot (Israel). Dept. of Particle Physics and Astrophysics; Hebrew Univ. of Jerusalem (Israel). Racah Inst. of Physics
Univ. of Southampton (United Kingdom). School of Physics and Astronomy
California Inst. of Technology (CalTech), Pasadena, CA (United States). Infrared Processing and Analysis Center
Stockholm Univ. (Sweden). Oskar Klein Centre, Dept. of Astronomy
Univ. of California, Davis, CA (United States). Dept. of Physics
Univ. of California, Santa Barbara CA (United States). Dept. of Physics; Las Cumbres Observatory Global Telescope, Goleta, CA (United States)
Univ. of California, Berkeley, CA (United States). Dept. of Astronomy
NASA Goddard Space Flight Center (GSFC), Greenbelt, MD (United States). Astrophysics Science Division
California Inst. of Technology (CalTech), Pasadena, CA (United States). Cahill Center for Astrophysics
Weizmann Inst. of Science, Rehovot (Israel). Dept. of Particle Physics and Astrophysics; Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States). Smithsonian Astrophysical Observatory
Univ. of California, Berkeley, CA (United States). Dept. of Astronomy; Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States). Computational Cosmology Center
California Inst. of Technology (CalTech), Pasadena, CA (United States). Spitzer Science Center
California Inst. of Technology (CalTech), Pasadena, CA (United States). Jet Propulsion Lab.
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Here, we present the light curves of the hydrogen-poor superluminous supernovae (SLSNe I) PTF 12dam and iPTF 13dcc, discovered by the (intermediate) Palomar Transient Factory. Both show excess emission at early times and a slowly declining light curve at late times. The early bump in PTF 12dam is very similar in duration (~10 days) and brightness relative to the main peak (2-3 mag fainter) compared to that observed in other SLSNe I. In contrast, the long-duration ( > 30 days) early excess emission in iPTF 13dcc, whose brightness competes with that of the main peak, appears to be of a different nature. We construct bolometric light curves for both targets, and fit a variety of light-curve models to both the early bump and main peak in an attempt to understand the nature of these explosions. Even though the slope of the late-time decline in the light curves of both SLSNe is suggestively close to that expected from the radioactive decay of 56Ni and 56Co, the amount of nickel required to power the full light curves is too large considering the estimated ejecta mass. The magnetar model including an increasing escape fraction provides a reasonable description of the PTF 12dam observations. However, neither the basic nor the double-peaked magnetar model is capable of reproducing the light curve of iPTF 13dcc. A model combining a shock breakout in an extended envelope with late-time magnetar energy injection provides a reasonable fit to the iPTF 13dcc observations. Finally, we find that the light curves of both PTF 12dam and iPTF 13dcc can be adequately fit with the model involving interaction with the circumstellar medium.
Vreeswijk, Paul M., et al. "On The Early-Time Excess Emission In Hydrogen-Poor Superluminous Supernovae." The Astrophysical Journal (Online), vol. 835, no. 1, Jan. 2017. https://doi.org/10.3847/1538-4357/835/1/58
Vreeswijk, Paul M., Leloudas, Giorgos, Gal-Yam, Avishay, De Cia, Annalisa, Perley, Daniel A., Quimby, Robert M., Waldman, Roni, Sullivan, Mark, Yan, Lin, Ofek, Eran O., Fremling, Christoffer, Taddia, Francesco, Sollerman, Jesper, Valenti, Stefano, Arcavi, Iair, Howell, D. Andrew, Filippenko, Alexei V., Cenko, S. Bradley, ... Kulkarni, Shrinivas R. (2017). On The Early-Time Excess Emission In Hydrogen-Poor Superluminous Supernovae. The Astrophysical Journal (Online), 835(1). https://doi.org/10.3847/1538-4357/835/1/58
Vreeswijk, Paul M., Leloudas, Giorgos, Gal-Yam, Avishay, et al., "On The Early-Time Excess Emission In Hydrogen-Poor Superluminous Supernovae," The Astrophysical Journal (Online) 835, no. 1 (2017), https://doi.org/10.3847/1538-4357/835/1/58
@article{osti_1393607,
author = {Vreeswijk, Paul M. and Leloudas, Giorgos and Gal-Yam, Avishay and De Cia, Annalisa and Perley, Daniel A. and Quimby, Robert M. and Waldman, Roni and Sullivan, Mark and Yan, Lin and Ofek, Eran O. and others},
title = {On The Early-Time Excess Emission In Hydrogen-Poor Superluminous Supernovae},
annote = {Here, we present the light curves of the hydrogen-poor superluminous supernovae (SLSNe I) PTF 12dam and iPTF 13dcc, discovered by the (intermediate) Palomar Transient Factory. Both show excess emission at early times and a slowly declining light curve at late times. The early bump in PTF 12dam is very similar in duration (~10 days) and brightness relative to the main peak (2-3 mag fainter) compared to that observed in other SLSNe I. In contrast, the long-duration ( > 30 days) early excess emission in iPTF 13dcc, whose brightness competes with that of the main peak, appears to be of a different nature. We construct bolometric light curves for both targets, and fit a variety of light-curve models to both the early bump and main peak in an attempt to understand the nature of these explosions. Even though the slope of the late-time decline in the light curves of both SLSNe is suggestively close to that expected from the radioactive decay of 56Ni and 56Co, the amount of nickel required to power the full light curves is too large considering the estimated ejecta mass. The magnetar model including an increasing escape fraction provides a reasonable description of the PTF 12dam observations. However, neither the basic nor the double-peaked magnetar model is capable of reproducing the light curve of iPTF 13dcc. A model combining a shock breakout in an extended envelope with late-time magnetar energy injection provides a reasonable fit to the iPTF 13dcc observations. Finally, we find that the light curves of both PTF 12dam and iPTF 13dcc can be adequately fit with the model involving interaction with the circumstellar medium.},
doi = {10.3847/1538-4357/835/1/58},
url = {https://www.osti.gov/biblio/1393607},
journal = {The Astrophysical Journal (Online)},
issn = {ISSN 1538-4357},
number = {1},
volume = {835},
place = {United States},
publisher = {Institute of Physics (IOP)},
year = {2017},
month = {01}}