Type Ic supernovae from the (intermediate) Palomar Transient Factory. (arXiv:2010.08392v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Barbarino_C/0/1/0/all/0/1">C. Barbarino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sollerman_J/0/1/0/all/0/1">J. Sollerman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taddia_F/0/1/0/all/0/1">F. Taddia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fremling_C/0/1/0/all/0/1">C. Fremling</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karamehmetoglu_E/0/1/0/all/0/1">E. Karamehmetoglu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arcavi_I/0/1/0/all/0/1">I. Arcavi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gal_Yam_A/0/1/0/all/0/1">A. Gal-Yam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laher_R/0/1/0/all/0/1">R. Laher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schulze_S/0/1/0/all/0/1">S. Schulze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wozniak_P/0/1/0/all/0/1">P. Wozniak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yan_L/0/1/0/all/0/1">Lin Yan</a>
Type Ic supernovae represent the explosions of the most stripped massive
stars, but their progenitors and explosion mechanisms remain unclear. Larger
samples of observed supernovae can help characterize the population of these
transients. We present an analysis of 44 spectroscopically normal Type Ic
supernovae, with focus on the light curves. The photometric data were obtained
over 7 years with the Palomar Transient Factory (PTF) and its continuation, the
intermediate Palomar Transient Factory (iPTF). This is the first homogeneous
and large sample of SNe Ic from an untargeted survey, and we aim to estimate
explosion parameters for the sample. We present K-corrected Bgriz light curves
of these SNe, obtained through photometry on template-subtracted images. We
performed an analysis on the shape of the $r$-band light curves and confirmed
the correlation between the rise parameter Delta m_{-10} and the decline
parameter Delta m_{15}. Peak r-band absolute magnitudes have an average of
-17.71 +- 0.85 mag. To derive the explosion epochs, we fit the r-band
lightcurves to a template derived from a well-sampled light curve. We computed
the bolometric light curves using r and g band data, g-r colors and bolometric
corrections. Bolometric light curves and Fe II lambda 5169 velocities at peak
were used to fit to the Arnett semianalytic model in order to estimate the
ejecta mass M_{ej}, the explosion energy E_{K} and the mass of radioactive
nickel (M(56) Ni) for each SN. Including 41 SNe, we find average values of
<M_{ej}>=4.50 +-0.79 msun, <E_{K}>=1.79 +- 0.29 x10^{51} erg, and <M(56)Ni)>=
0.19 +- 0.03 msun. The explosion-parameter distributions are comparable to
those available in the literature, but our large sample also includes some
transients with narrow and very broad light curves leading to more extreme
ejecta masses values.
Type Ic supernovae represent the explosions of the most stripped massive
stars, but their progenitors and explosion mechanisms remain unclear. Larger
samples of observed supernovae can help characterize the population of these
transients. We present an analysis of 44 spectroscopically normal Type Ic
supernovae, with focus on the light curves. The photometric data were obtained
over 7 years with the Palomar Transient Factory (PTF) and its continuation, the
intermediate Palomar Transient Factory (iPTF). This is the first homogeneous
and large sample of SNe Ic from an untargeted survey, and we aim to estimate
explosion parameters for the sample. We present K-corrected Bgriz light curves
of these SNe, obtained through photometry on template-subtracted images. We
performed an analysis on the shape of the $r$-band light curves and confirmed
the correlation between the rise parameter Delta m_{-10} and the decline
parameter Delta m_{15}. Peak r-band absolute magnitudes have an average of
-17.71 +- 0.85 mag. To derive the explosion epochs, we fit the r-band
lightcurves to a template derived from a well-sampled light curve. We computed
the bolometric light curves using r and g band data, g-r colors and bolometric
corrections. Bolometric light curves and Fe II lambda 5169 velocities at peak
were used to fit to the Arnett semianalytic model in order to estimate the
ejecta mass M_{ej}, the explosion energy E_{K} and the mass of radioactive
nickel (M(56) Ni) for each SN. Including 41 SNe, we find average values of
<M_{ej}>=4.50 +-0.79 msun, <E_{K}>=1.79 +- 0.29 x10^{51} erg, and <M(56)Ni)>=
0.19 +- 0.03 msun. The explosion-parameter distributions are comparable to
those available in the literature, but our large sample also includes some
transients with narrow and very broad light curves leading to more extreme
ejecta masses values.
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