TY - JOUR
T1 - Type IIn supernova light-curve properties measured from an untargeted survey samplE
AU - Nyholm, A.
AU - Sollerman, J.
AU - Tartaglia, L.
AU - Taddia, F.
AU - Fremling, C.
AU - Blagorodnova, N.
AU - Filippenko, A.
AU - Gal-Yam, A.
AU - Howell, D. A.
AU - Karamehmetoglu, E.
AU - Kulkarni, S. R.
AU - Laher, R.
AU - Leloudas, G.
AU - Masci, F.
AU - Kasliwal, M. M.
AU - Mora, K.
AU - Moriya, T. J.
AU - Ofek, E. O.
AU - Papadogiannakis, S.
AU - Quimby, R.
AU - Rebbapragada, U.
AU - Schulze, S.
PY - 2020
Y1 - 2020
N2 - The evolution of a Type IIn supernova (SN IIn) is governed by the
interaction between the SN ejecta and a hydrogen-rich circumstellar
medium. The SNe IIn thus allow us to probe the late-time mass-loss
history of their progenitor stars. We present a sample of SNe IIn from
the untargeted, magnitude-limited surveys of the Palomar Transient
Factory (PTF) and its successor, the intermediate PTF (iPTF). To date,
statistics on SN IIn optical light-curve properties have generally been
based on small (≲10 SNe) samples from targeted SN surveys. The SNe IIn
found and followed by the PTF/iPTF were used to select a sample of 42
events with useful constraints on the rise times as well as with
available post-peak photometry. The sample SNe were discovered in
2009−2016 and have at least one low-resolution classification spectrum,
as well as photometry from the P48 and P60 telescopes at Palomar
Observatory. We study the light-curve properties of these SNe IIn using
spline fits (for the peak and the declining portion) and template
matching (for the rising portion). We study the peak-magnitude
distribution, rise times, decline rates, colour evolution, host
galaxies, and K-corrections of the SNe in our sample. We find that the
typical rise times are divided into fast and slow risers at 20 ± 6 d and
50 ± 11 d, respectively. The decline rates are possibly divided into
two clusters (with slopes 0.013 ± 0.006 mag d−1 and 0.040 ± 0.010 mag d−1),
but this division has weak statistical significance. We find no
significant correlation between the peak luminosity of SNe IIn and their
rise times, but the more luminous SNe IIn are generally found to be
more long-lasting. Slowly rising SNe IIn are generally found to decline
slowly. The SNe in our sample were hosted by galaxies of absolute
magnitude −22 ≲ Mg ≲ −13 mag. The K-corrections at
light-curve peak of the SNe IIn in our sample are found to be within 0.2
mag for the observer’s frame r-band, for SNe at redshifts z <
0.25. By applying K-corrections and also including ostensibly
“superluminous” SNe IIn, we find that the peak magnitudes are Mpeakr
= −19.18 ± 1.32 mag. We conclude that the occurrence of conspicuous
light-curve bumps in SNe IIn, such as in iPTF13z, are limited to 1.4+14.6−1.0
% of the SNe IIn. We also investigate a possible sub-type of SNe IIn
with a fast rise to a ≳50 d plateau followed by a slow, linear decline.
AB - The evolution of a Type IIn supernova (SN IIn) is governed by the
interaction between the SN ejecta and a hydrogen-rich circumstellar
medium. The SNe IIn thus allow us to probe the late-time mass-loss
history of their progenitor stars. We present a sample of SNe IIn from
the untargeted, magnitude-limited surveys of the Palomar Transient
Factory (PTF) and its successor, the intermediate PTF (iPTF). To date,
statistics on SN IIn optical light-curve properties have generally been
based on small (≲10 SNe) samples from targeted SN surveys. The SNe IIn
found and followed by the PTF/iPTF were used to select a sample of 42
events with useful constraints on the rise times as well as with
available post-peak photometry. The sample SNe were discovered in
2009−2016 and have at least one low-resolution classification spectrum,
as well as photometry from the P48 and P60 telescopes at Palomar
Observatory. We study the light-curve properties of these SNe IIn using
spline fits (for the peak and the declining portion) and template
matching (for the rising portion). We study the peak-magnitude
distribution, rise times, decline rates, colour evolution, host
galaxies, and K-corrections of the SNe in our sample. We find that the
typical rise times are divided into fast and slow risers at 20 ± 6 d and
50 ± 11 d, respectively. The decline rates are possibly divided into
two clusters (with slopes 0.013 ± 0.006 mag d−1 and 0.040 ± 0.010 mag d−1),
but this division has weak statistical significance. We find no
significant correlation between the peak luminosity of SNe IIn and their
rise times, but the more luminous SNe IIn are generally found to be
more long-lasting. Slowly rising SNe IIn are generally found to decline
slowly. The SNe in our sample were hosted by galaxies of absolute
magnitude −22 ≲ Mg ≲ −13 mag. The K-corrections at
light-curve peak of the SNe IIn in our sample are found to be within 0.2
mag for the observer’s frame r-band, for SNe at redshifts z <
0.25. By applying K-corrections and also including ostensibly
“superluminous” SNe IIn, we find that the peak magnitudes are Mpeakr
= −19.18 ± 1.32 mag. We conclude that the occurrence of conspicuous
light-curve bumps in SNe IIn, such as in iPTF13z, are limited to 1.4+14.6−1.0
% of the SNe IIn. We also investigate a possible sub-type of SNe IIn
with a fast rise to a ≳50 d plateau followed by a slow, linear decline.
U2 - 10.1051/0004-6361/201936097
DO - 10.1051/0004-6361/201936097
M3 - Journal article
SN - 0004-6361
VL - 637
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A73
ER -