Type IIn supernova light-curve properties measured from an untargeted survey sample-猫眼课题宝

DOI：

10.1051/0004-6361/201936097

发表时间：

2019-06

期刊：

Astronomy & Astrophysics

影响因子：

6.5

通讯作者：

中科院分区：

物理与天体物理2区

文献类型：

作者：

A. Nyholm;J. Sollerman;L. Tartaglia;F. Taddia;C. Fremling;N. Blagorodnova;A. Filippenko;A. Gal-yam;D. Howell;E. Karamehmetoglu;S. Kulkarni;R. Laher;G. Leloudas;F. Masci;M. Kasliwal;K. Mora;T. Moriya;E. Ofek;S. Papadogiannakis;R. Quimby;U. Rebbapragada;S. Schulze

IIn 型超新星 (SN IIn) 的演化是由 SN 喷射物与富含氢的星周介质之间的相互作用控制的。因此，超新星 IIn 使我们能够探究其祖星的晚期质量损失历史。我们提供了来自帕洛玛瞬态工厂 (PTF) 及其后继者中间 PTF (iPTF) 的无目标、星等有限调查的超新星 IIn 样本。迄今为止，SN IIn 光学光曲线特性的统计数据通常基于目标 SN 调查的小样本（≲10 SNe）。发现的 SNe IIn 以及随后的 PTF/iPTF 用于选择 42 个事件的样本，并对上升时间以及可用的峰后光度测量进行了有用的限制。超新星样本于 2009 年至 2016 年被发现，至少具有一个低分辨率分类光谱，以及来自帕洛马天文台 P48 和 P60 望远镜的光度测量。我们使用样条拟合（对于峰值和下降部分）和模板匹配（对于上升部分）来研究这些 SNe IIn 的光曲线特性。我们研究了样本中超新星的峰值星等分布、上升时间、下降率、颜色演化、宿主星系和 K 校正。我们发现典型的上升时间分为快上升和慢上升，分别为 20 ± 6 d 和 50 ± 11 d。下降率可能分为两类（斜率分别为 0.013 ± 0.006 mag d−1 和 0.040 ± 0.010 mag d−1），但这种划分的统计意义较弱。我们发现 SNe IIn 的峰值光度与其上升时间之间没有显着相关性，但通常发现发光度越高的 SNe IIn 持续时间越长。缓慢上升的超新星 IIn 通常会缓慢下降。我们样本中的超新星由绝对星等为 -22 ≲ Mg ≲ -13 星等的星系所托管。我们发现，对于红移 z < 0.25 的超新星，对于观察者的框架 r 波段，超新星 IIn 的光曲线峰值处的 K 校正在 0.2 星等内。通过应用 K 校正并包括表面上“超光度”的 SNe IIn，我们发现峰值星等为 Mrpeak = −19.18 ± 1.32 mag。我们得出的结论是，超新星 IIn 中（例如 iPTF13z）中明显的光曲线凸点的出现仅限于超新星 IIn 的 1.4+14.6−1.0 %。我们还研究了 SNe IIn 的一种可能的子类型，该子类型快速上升到 ≳50 d 的平台期，然后缓慢、线性下降。

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 Mrpeak = −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.

Type IIn supernova light-curve properties measured from an untargeted survey sample

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