Share Email Print

Proceedings Paper

NIR camera and spectrograph SWIMS for TAO 6.5m telescope: array control system and its performance
Author(s): Yasunori Terao; Kentaro Motohara; Masahiro Konishi; Hidenori Takahashi; Natsuko M. Kato; Yutaro Kitagawa; Yutaka Kobayakawa; Hirofumi Ohashi; Ken Tateuchi; Soya Todo
Format Member Price Non-Member Price
PDF $17.00 $21.00

Paper Abstract

SWIMS (Simultaneous-color Wide-field Infrared Multi-object Spectrograph) is a near-infrared imager and multi-object spectrograph as one of the first generation instruments for the University of Tokyo Atacama Observatory (TAO) 6.5m telescope. In this paper, we describe an array control system of SWIMS and results of detector noise performance evaluation. SWIMS incorporates four (and eight in future) HAWAII-2RG focal plane arrays for detectors, each driven by readout electronics components: a SIDECAR ASIC and a JADE2 Card. The readout components are controlled by a HAWAII-2RG Testing Software running on a virtual Windows machine on a Linux PC called array control PC. All of those array control PCs are then supervised by a SWIMS control PC. We have developed an "array control software system", which runs on the array control PC to control the HAWAII-2RG Testing Software, and consists of a socket client and a dedicated server called device manager. The client runs on the SWIMS control PC, and the device manager runs on the array control PC. An exposure command, issued by the client on the SWIMS control PC, is sent to the multiple device managers on the array control PCs, and then multiple HAWAII-2RGs are driven simultaneously. Using this system, we evaluate readout noise performances of the detectors, both in a test dewar and in a SWIMS main dewar. In the test dewar, we confirm the readout noise to be 4.3 e- r.m.s. by 32 times multiple sampling when we operate only a single HAWAII-2RG, whereas in the case of simultaneous driving of two HAWAII-2RGs, we still obtain sufficiently low readout noise of 10 e- r.m.s. In the SWIMS main dewar, although there are some differences between the detectors, the readout noise is measured to be 4:1−4:6 e- r.m.s. with simultaneous driving by 64 times multiple sampling, which meets the requirement for background-limited observations in J band of 14 e- r.m.s..

Paper Details

Date Published: 5 August 2016
PDF: 9 pages
Proc. SPIE 9915, High Energy, Optical, and Infrared Detectors for Astronomy VII, 99151W (5 August 2016); doi: 10.1117/12.2232014
Show Author Affiliations
Yasunori Terao, The Univ. of Tokyo (Japan)
Kentaro Motohara, The Univ. of Tokyo (Japan)
Masahiro Konishi, The Univ. of Tokyo (Japan)
Hidenori Takahashi, The Univ. of Tokyo (Japan)
Natsuko M. Kato, The Univ. of Tokyo (Japan)
Yutaro Kitagawa, The Univ. of Tokyo (Japan)
Yutaka Kobayakawa, The Univ. of Tokyo (Japan)
Hirofumi Ohashi, The Univ. of Tokyo (Japan)
Ken Tateuchi, The Univ. of Tokyo (Japan)
Soya Todo, The Univ. of Tokyo (Japan)

Published in SPIE Proceedings Vol. 9915:
High Energy, Optical, and Infrared Detectors for Astronomy VII
Andrew D. Holland; James Beletic, Editor(s)

© SPIE. Terms of Use
Back to Top
Sign in to read the full article
Create a free SPIE account to get access to
premium articles and original research
Forgot your username?