TY - JOUR
T1 - CoCo
T2 - Instrumentation in Astronomy VIII 1994
AU - Wang, Shu I.
AU - Owensby, Pamela D.
AU - Brown, Robert H.
AU - Stahlberger, Werner E.
AU - Cavedoni, Charles P.
AU - Hua, Rong
AU - Ftaclas, Christ
N1 - Funding Information:
CoCo was funded by NASA contracts NAS7-1 1 14 and NAS7-1 195. The authors would like to thank Jonathan Gradie for originating this pmject. We also thank Mark Shure and Paul Kalas f their helpful discussions. We are indebted to the !RTF for providing us information on NSFCAM. The diffraction analysis software was developed by Raytron, Inc. Sandie Osborne provided invaluable assistance with the preparation of this manuscript.
Publisher Copyright:
© 1994 SPIE. All rights reserved.
PY - 1994/6/1
Y1 - 1994/6/1
N2 - This paper describes the design of an infrared Cold Coronagraph (CoCo) built for use at the NASA 3-m Infrared Telescope Facility (IRTF) at Mauna Kea Observatory, fen the imaging of faint infrared sources in proximity to bright sources. The coronagraph is designed to obtain high contrast photometric images by use of an occulting mask and a pupil mask. The coronagraph is to be used in combination with the IRTF NSFCAM, which covers 1-5 |im and uses a 256×256 InSb array. The platescale can be varied from 0.067pixel to 0.1 V/pixci. covering a field of view of 14" and 38", respectively. Selectable apodized and hard occulting masks are mounted on a wheel as the first element in the system to reduce scattered light Selectable pupil masks are cooled to 77K within the CoCo cryostat. The cryostat consists of a liquid nitrogen can for cooling the optics, masks, and baffles. The CoCo dewar is mounted on a slide in a housing to allow it to move out of the beam path so that the NSFCAM may be used with or without the coronagraph during the same observing period.
AB - This paper describes the design of an infrared Cold Coronagraph (CoCo) built for use at the NASA 3-m Infrared Telescope Facility (IRTF) at Mauna Kea Observatory, fen the imaging of faint infrared sources in proximity to bright sources. The coronagraph is designed to obtain high contrast photometric images by use of an occulting mask and a pupil mask. The coronagraph is to be used in combination with the IRTF NSFCAM, which covers 1-5 |im and uses a 256×256 InSb array. The platescale can be varied from 0.067pixel to 0.1 V/pixci. covering a field of view of 14" and 38", respectively. Selectable apodized and hard occulting masks are mounted on a wheel as the first element in the system to reduce scattered light Selectable pupil masks are cooled to 77K within the CoCo cryostat. The cryostat consists of a liquid nitrogen can for cooling the optics, masks, and baffles. The CoCo dewar is mounted on a slide in a housing to allow it to move out of the beam path so that the NSFCAM may be used with or without the coronagraph during the same observing period.
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U2 - 10.1117/12.176765
DO - 10.1117/12.176765
M3 - Conference article
AN - SCOPUS:0040073942
SN - 0277-786X
VL - 2198
SP - 578
EP - 589
JO - Proceedings of SPIE - The International Society for Optical Engineering
JF - Proceedings of SPIE - The International Society for Optical Engineering
Y2 - 13 March 1994 through 18 March 1994
ER -