R-band light-curve properties of Type Ia supernovae from the (intermediate) Palomar Transient Factory. (arXiv:1812.01439v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Papadogiannakis_S/0/1/0/all/0/1">S. Papadogiannakis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goobar_A/0/1/0/all/0/1">A. Goobar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amanullah_R/0/1/0/all/0/1">R. Amanullah</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulla_M/0/1/0/all/0/1">M. Bulla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dhawan_S/0/1/0/all/0/1">S. Dhawan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doran_G/0/1/0/all/0/1">G. Doran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feindt_U/0/1/0/all/0/1">U. Feindt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferretti_R/0/1/0/all/0/1">R. Ferretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hangard_L/0/1/0/all/0/1">L. Hangard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howell_D/0/1/0/all/0/1">D. A. Howell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johansson_J/0/1/0/all/0/1">J. Johansson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kasliwal_M/0/1/0/all/0/1">M. M. Kasliwal</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:+Masci_F/0/1/0/all/0/1">F. Masci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nyholm_A/0/1/0/all/0/1">A. Nyholm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ofek_E/0/1/0/all/0/1">E. Ofek</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:+Yan_L/0/1/0/all/0/1">L. Yan</a>
We present the best 265 sampled R-band light curves of spectroscopically We present the best 265 sampled R-band light curves of spectroscopically http://arxiv.org/icons/sfx.gif
identified Type Ia supernovae (SNe) from the Palomar Transient Factory (PTF;
2009-2012) survey and the intermediate Palomar Transient Factory (iPTF;
2013-2017). A model-independent light curve template is built from our data-set
with the purpose to investigate average properties and diversity in our sample.
We searched for multiple populations in the light curve properties using
machine learning tools. We also utilised the long history of our light curves,
up to 4000 days, to exclude any significant pre- or post- supernova flares.
From the shapes of light curves we found the average rise time in the R band to
be $16.8^{+0.5}_{-0.6}$ days. Although PTF/iPTF were single-band surveys, by
modelling the residuals of the SNe in the Hubble-Lema^{i}tre diagram, we
estimate the average colour excess of our sample to be $<$E$($B$-$V$)> approx
0.05(2)$ mag and thus the mean corrected peak brightness to be $M_R =
-19.02pm0.02$ $+5 log( {rm H}_0 [{rm km} cdot{rm s}^{-1} {rm
Mpc}^{-1}]/70)$ mag with only weakly dependent on light curve shape. The
intrinsic scatter is found to be $sigma_R = 0.186 pm 0.033$ mag for the
redshift range $0.05
identified Type Ia supernovae (SNe) from the Palomar Transient Factory (PTF;
2009-2012) survey and the intermediate Palomar Transient Factory (iPTF;
2013-2017). A model-independent light curve template is built from our data-set
with the purpose to investigate average properties and diversity in our sample.
We searched for multiple populations in the light curve properties using
machine learning tools. We also utilised the long history of our light curves,
up to 4000 days, to exclude any significant pre- or post- supernova flares.
From the shapes of light curves we found the average rise time in the R band to
be $16.8^{+0.5}_{-0.6}$ days. Although PTF/iPTF were single-band surveys, by
modelling the residuals of the SNe in the Hubble-Lema^{i}tre diagram, we
estimate the average colour excess of our sample to be $<$E$($B$-$V$)> approx
0.05(2)$ mag and thus the mean corrected peak brightness to be $M_R =
-19.02pm0.02$ $+5 log( {rm H}_0 [{rm km} cdot{rm s}^{-1} {rm
Mpc}^{-1}]/70)$ mag with only weakly dependent on light curve shape. The
intrinsic scatter is found to be $sigma_R = 0.186 pm 0.033$ mag for the
redshift range $0.05<z<0.1$, without colour corrections of individual SNe. Our
analysis shows that Malmquist bias becomes very significant at z=0.13. A
similar limitation is expected for the ongoing Zwicky Transient Facility (ZTF)
survey using the same telescope, but new camera expressly designed for ZTF.
