Kiso supernova survey (KISS): survey strategy
Morokuma, T; Tominaga, N; Tanaka, M; Mori, K; Matsumoto, E; Kikuchi, Y; Shibata, T; Sako, S; Aoki, T; Doi, M; Kobayashi, N; Maehara, H; Matsunaga, N; Mito, H; Miyata, T; Nakada, Y; Soyano, T; Tarusawa, K; Miyazaki, S; Nakata, F; Okada, N; Sarugaku, Y; Richmond, M. W; Akitaya, H; Aldering, G; Arimatsu, K; Contreras, C; Horiuchi, T; Hsiao, E. Y; Itoh, R; Iwata, I; Kawabata, K. S; Kawai, N; Kitagawa, Y; Kokubo, M; Kuroda, D; Mazzali, P; Miswava, T; Moritani, Y; Morrell, N; Okamoto, R; Pavlyuk, N; Phillips, M. M; Pian, E; Sahu, D. K; Saito, Y; Sano, K; Stritzinger, M. D; Tachibana, Y; Taddia, F; Takaki, K; Tateuchi, K; Tomita, A; Tsvetkov, D; Ui, T; Ukita, N; Urata, Y; Walker, E; Yoshii, T
Date:
2014-12
Abstract:
The Kiso Supernova Survey (KISS) is a high-cadence optical wide-field supernova
(SN) survey. The primary goal of the survey is to catch the very early light of a
SN, during the shock breakout phase. Detection of SN shock breakouts combined
with multi-band photometry obtained with other facilities would provide detailed
physical information on the progenitor stars of SNe. The survey is performed
using a 2.
◦2 × 2.
◦2 field-of-view instrument on the 1.05-m Kiso Schmidt telescope,
the Kiso Wide Field Camera (KWFC). We take a 3-min exposure in g-band once
every hour in our survey, reaching magnitude g ∼ 20–21. About 100 nights of telescope time per year have been spent on the survey since 2012 April. The number
of the shock breakout detections is estimated to be of the order of 1 during our
three-year project. This paper summarizes the KISS project including the KWFC
observing setup, the survey strategy, the data reduction system, and CBET-reported
SNe discovered so far by KISS
Description:
Restricted Access © Astronomical Society of Japan http://dx.doi.org/10.1093/pasj/psu105
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