CoCo: An infrared cold coronagraph for astronomical observations

Shu I. Wang; Pamela D. Owensby; Robert H. Brown; Werner E. Stahlberger; Charles P. Cavedoni; Rong Hua; Christ Ftaclas

doi:10.1117/12.176765

CoCo: An infrared cold coronagraph for astronomical observations

Shu I. Wang
, Pamela D. Owensby
, Robert H. Brown
, Werner E. Stahlberger
, Charles P. Cavedoni
, Rong Hua
, Christ Ftaclas

Research output: Contribution to journal › Conference article › peer-review

11 Scopus citations

Abstract

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.

Original language	English (US)
Pages (from-to)	578-589
Number of pages	12
Journal	Proceedings of SPIE - The International Society for Optical Engineering
Volume	2198
DOIs	https://doi.org/10.1117/12.176765
State	Published - Jun 1 1994
Externally published	Yes
Event	Instrumentation in Astronomy VIII 1994 - Kailua, Kona, United States Duration: Mar 13 1994 → Mar 18 1994

ASJC Scopus subject areas

Electronic, Optical and Magnetic Materials
Condensed Matter Physics
Computer Science Applications
Applied Mathematics
Electrical and Electronic Engineering

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10.1117/12.176765

Cite this

@article{917e72cb9c36427fa82084669126c7dc,

title = "CoCo: An infrared cold coronagraph for astronomical observations",

abstract = "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.",

author = "Wang, \{Shu I.\} and Owensby, \{Pamela D.\} and Brown, \{Robert H.\} and Stahlberger, \{Werner E.\} and Cavedoni, \{Charles P.\} and Rong Hua and Christ Ftaclas",

note = "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: {\textcopyright} 1994 SPIE. All rights reserved.; Instrumentation in Astronomy VIII 1994 ; Conference date: 13-03-1994 Through 18-03-1994",

year = "1994",

month = jun,

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doi = "10.1117/12.176765",

language = "English (US)",

volume = "2198",

pages = "578--589",

journal = "Proceedings of SPIE - The International Society for Optical Engineering",

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publisher = "SPIE",

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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.

UR - https://www.scopus.com/pages/publications/0040073942

UR - https://www.scopus.com/pages/publications/0040073942#tab=citedBy

U2 - 10.1117/12.176765

DO - 10.1117/12.176765

M3 - Conference article

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 -

CoCo: An infrared cold coronagraph for astronomical observations

Abstract

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