Superluminous Supernovae from the Dark Energy Survey. (arXiv:1812.04071v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Angus_C/0/1/0/all/0/1">C. R. Angus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_M/0/1/0/all/0/1">M. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sullivan_M/0/1/0/all/0/1">M. Sullivan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Inserra_C/0/1/0/all/0/1">C. Inserra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wiseman_P/0/1/0/all/0/1">P. Wiseman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAndrea_C/0/1/0/all/0/1">C. B. D'Andrea</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thomas_B/0/1/0/all/0/1">B. P. Thomas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nichol_R/0/1/0/all/0/1">R. C. Nichol</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asorey_J/0/1/0/all/0/1">J. Asorey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_P/0/1/0/all/0/1">P. J. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casas_R/0/1/0/all/0/1">R. Casas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castander_F/0/1/0/all/0/1">F. J. Castander</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Curtin_C/0/1/0/all/0/1">C. Curtin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frohmaier_C/0/1/0/all/0/1">C. Frohmaier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galbany_L/0/1/0/all/0/1">L. Galbany</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glazebrook_K/0/1/0/all/0/1">K. Glazebrook</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruen_D/0/1/0/all/0/1">D. Gruen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_A/0/1/0/all/0/1">A. G. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lidman_C/0/1/0/all/0/1">C. Lidman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macaulay_E/0/1/0/all/0/1">E. Macaulay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nugent_P/0/1/0/all/0/1">P. Nugent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pursiainen_M/0/1/0/all/0/1">M. Pursiainen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sako_M/0/1/0/all/0/1">M. Sako</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thomas_R/0/1/0/all/0/1">R. C. Thomas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_T/0/1/0/all/0/1">T. M. C. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_S/0/1/0/all/0/1">S. Avila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_E/0/1/0/all/0/1">E. Bertin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_D/0/1/0/all/0/1">D. Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buckley_Geer_E/0/1/0/all/0/1">E. Buckley-Geer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burke_D/0/1/0/all/0/1">D. L. Burke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosell_A/0/1/0/all/0/1">A. Carnero Rosell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carretero_J/0/1/0/all/0/1">J. Carretero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costa_L/0/1/0/all/0/1">L. N. da Costa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vicente_J/0/1/0/all/0/1">J. De Vicente</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desai_S/0/1/0/all/0/1">S. Desai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diehl_H/0/1/0/all/0/1">H. T. Diehl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doel_P/0/1/0/all/0/1">P. Doel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eifler_T/0/1/0/all/0/1">T. F. Eifler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flaugher_B/0/1/0/all/0/1">B. Flaugher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fosalba_P/0/1/0/all/0/1">P. Fosalba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frieman_J/0/1/0/all/0/1">J. Frieman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Bellido_J/0/1/0/all/0/1">J. García-Bellido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruendl_R/0/1/0/all/0/1">R. A. Gruendl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gschwend_J/0/1/0/all/0/1">J. Gschwend</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hartley_W/0/1/0/all/0/1">W. G. Hartley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hollowood_D/0/1/0/all/0/1">D. L. Hollowood</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Honscheid_K/0/1/0/all/0/1">K. Honscheid</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoyle_B/0/1/0/all/0/1">B. Hoyle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+James_D/0/1/0/all/0/1">D. J. James</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuehn_K/0/1/0/all/0/1">K. Kuehn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuropatkin_N/0/1/0/all/0/1">N. Kuropatkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lahav_O/0/1/0/all/0/1">O. Lahav</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lima_M/0/1/0/all/0/1">M. Lima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maia_M/0/1/0/all/0/1">M. A. G. Maia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+March_M/0/1/0/all/0/1">M. March</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marshall_J/0/1/0/all/0/1">J. L. Marshall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menanteau_F/0/1/0/all/0/1">F. Menanteau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_C/0/1/0/all/0/1">C. J. Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miquel_R/0/1/0/all/0/1">R. Miquel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ogando_R/0/1/0/all/0/1">R. L. C. Ogando</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plazas_A/0/1/0/all/0/1">A. A. Plazas</a>, et al. (10 additional authors not shown)
We present a sample of 21 hydrogen-free superluminous supernovae (SLSNe-I), We present a sample of 21 hydrogen-free superluminous supernovae (SLSNe-I), http://arxiv.org/icons/sfx.gif
and one hydrogen-rich SLSN (SLSN-II) detected during the five-year Dark Energy
Survey (DES). These SNe, located in the redshift range 0.220
and one hydrogen-rich SLSN (SLSN-II) detected during the five-year Dark Energy
Survey (DES). These SNe, located in the redshift range 0.220<z<1.998, represent
the largest homogeneously-selected sample of SLSN events at high redshift. We
present the observed g,r, i, z light curves for these SNe, which we interpolate
using Gaussian Processes. The resulting light curves are analysed to determine
the luminosity function of SLSN-I, and their evolutionary timescales. The DES
SLSN-I sample significantly broadens the distribution of SLSN-I light curve
properties when combined with existing samples from the literature. We fit a
magnetar model to our SLSNe, and find that this model alone is unable to
replicate the behaviour of many of the bolometric light curves. We search the
DES SLSN-I light curves for the presence of initial peaks prior to the main
light-curve peak. Using a shock breakout model, our Monte Carlo search finds
that 3 of our 14 events with pre-max data display such initial peaks. However,
10 events show no evidence for such peaks, in some cases down to an absolute
magnitude of <-16, suggesting that such features are not ubiquitous to all
SLSN-I events. We also identify a red pre-peak feature within the light curve
of one SLSN, which is comparable to that observed within SN2018bsz.
