TY - GEN
T1 - Conceptual design of a wide-field near UV transient survey in a 6U CubeSat
AU - Yatsu, Yoichi
AU - Ozawa, Toshiki
AU - Sasaki, Kenichi
AU - Mamiya, Hideo
AU - Kawai, Nobuyuki
AU - Kikuya, Yuhei
AU - Matsushita, Masanori
AU - Matunaga, Saburo
AU - Nikzad, Shouleh
AU - Bilgi, Pavaman
AU - Kulkarni, Shrinivas R.
AU - Tominaga, Nozomu
AU - Tanaka, Masaomi
AU - Morokuma, Tomoki
AU - Takeyama, Norihide
AU - Enokuchi, Akito
N1 - Funding Information:
This work was supported by JSPS Grant-in-Aid for Young Scientists (A) Grant Number JP17H04829. YY thanks Mr. Ryo Adachi of Tokyo Tech for checking the surface stellar density by using data archive of MITSuME telescope.
Publisher Copyright:
© 2018 SPIE.
PY - 2018
Y1 - 2018
N2 - A conceptual design of a wide-field near UV transient survey in a 6U CubeSat is presented. Ultraviolet is one of the frontier in the transient astronomy. To open up the discovery region, we are developing a 6U CubeSat for transient exploration. The possible targets will be supernova shock-breakouts, tidal disruption events, and the blue emission from NS-NS mergers in very early phase. If we only focused on nearby/bright sources, the required detection limit is around 20 mag (AB). To avoid the background and optical light, we chose a waveband of 230-280 nm. As an imaging detector, we employ a delta-doped back-illuminated CMOS. In addition to delta doping, the multi-layer coating directly deposited on the detector enables both a high in-band UV QE and the ultra-low optical rejection ratio. Taking into account these specifications, even an 8 cm telescope can achieve the detection limit of 20 magAB. The expected FoV is larger than 60 deg2.
AB - A conceptual design of a wide-field near UV transient survey in a 6U CubeSat is presented. Ultraviolet is one of the frontier in the transient astronomy. To open up the discovery region, we are developing a 6U CubeSat for transient exploration. The possible targets will be supernova shock-breakouts, tidal disruption events, and the blue emission from NS-NS mergers in very early phase. If we only focused on nearby/bright sources, the required detection limit is around 20 mag (AB). To avoid the background and optical light, we chose a waveband of 230-280 nm. As an imaging detector, we employ a delta-doped back-illuminated CMOS. In addition to delta doping, the multi-layer coating directly deposited on the detector enables both a high in-band UV QE and the ultra-low optical rejection ratio. Taking into account these specifications, even an 8 cm telescope can achieve the detection limit of 20 magAB. The expected FoV is larger than 60 deg2.
KW - Tidal disruption events
KW - Ultraviolet
KW - cubesat
KW - gravitational wave
KW - supernovae shockbreakouts
KW - time-domain
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U2 - 10.1117/12.2313026
DO - 10.1117/12.2313026
M3 - Conference contribution
AN - SCOPUS:85051848250
SN - 9781510619517
T3 - Proceedings of SPIE - The International Society for Optical Engineering
BT - Space Telescopes and Instrumentation 2018
A2 - Nikzad, Shouleh
A2 - Den Herder, Jan-Willem A.
A2 - Nakazawa, Kazuhiro
PB - SPIE
T2 - Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray
Y2 - 10 June 2018 through 15 June 2018
ER -