Canada-France-Hawaii telescope near-infrared camera project

Simons, Douglas A.; Clark, Christopher C.; Kerr, John M.; Massey, Stephen C.; Smith, Suzanne; Toomey, Douglas W.

doi:10.1117/12.158703

Cited by 5 publications

(5 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Tables 4 and 5 list the Ðlters, only thirteen of which are available at any one time with NIRIM, and the corresponding throughput, background, and sensitivities when NIRIM is on the MLO 1 m. The measured throughput, which includes e †ects of the array detector, NIRIMÏs optics, the telescope, and the sky, is comparable to similar systems (Simons et al 1993 ;Herbst et al 1993). The background for the I, J, and H broadband Ðlters is comparable to that observed by near-IR cameras on Mauna Kea (Hodapp et al 1992 ;Simons et al 1993), while the backgrounds for K@ and K are about 1 and 2 mag brighter, respectively. The brighter background at K@ and K is probably caused by the thermal emission from the telescope, which was optimized for optical, not infrared, astronomy, and from the sky, which is brighter because of MLOÏs signiÐcantly lower elevation.…”

Section: Image Quality and Sensitivitymentioning

confidence: 99%

NIRIM: A Dual‐Purpose Near‐Infrared (0.76–2.5 μm) Imaging Camera for Wide‐Field and High‐Resolution Imaging

Meixner

Owl

Leach

1999

PUBL ASTRON SOC PAC

View full text Add to dashboard Cite

ABSTRACT. We present the design and performance characteristics of the Near-Infrared Imager (NIRIM), which is a near-infrared camera operating in the 0.76[2.5 km wavelength range. NIRIM is an example of a cost-e †ective way to expand two telescopesÏ capabilities to infrared wavelengths. NIRIM has been used for photometry and wide-Ðeld imaging on our 1 m telescope at the Mount Laguna (8@ .5 ] 8@ .5) Observatory since 1995 August. In the future, NIRIM will also be used for high angular resolution imaging with the University of Illinois Seeing Improvement System (UnISIS), which is a laser guided adaptive optics system at the focus of the Mount Wilson 2.5 m telescope. coude

show abstract

Section: Image Quality and Sensitivitymentioning

confidence: 99%

NIRIM: A Dual‐Purpose Near‐Infrared (0.76–2.5 μm) Imaging Camera for Wide‐Field and High‐Resolution Imaging

Meixner

Owl

Leach

1999

PUBL ASTRON SOC PAC

View full text Add to dashboard Cite

show abstract

“…An FTS is therefore an obvious candidate for imaging spectroscopy, offering flexibility when choosing field size and spectral resolution up to high values for both parameters (Maillard et al 2013). But as was the case with IFSs (Section 3.2), it was not until the 1990s that the technique found its first implementation in an astronomical instrument, which was BEAR (Simons et al 1994, Maillard 2000) at the CFHT. Despite the fact that this particular FTS was initially not designed for imaging spectroscopy, the usable field of view was still 24 arcsec in diameter.…”

Section: Fourier Transform Spectrometersmentioning

confidence: 99%

“…The fundamental advantages of the FTS also made the concept attractive for the James Webb Space Telescope ( JWST, formerly the Next Generation Space Telescope), resulting in a number of instrument proposals and comparisons with other imaging spectroscopy techniques (see, e.g., Smith & Long 2000). Although in the end none of these concepts were implemented on JWST, the preparatory work resulted, e.g., in the SpIOMM (Bernier et al 2008) prototype with a 12-arcsec × 12-arcsec field of view, installed at the Mont Megantic Telescope.…”

Section: Fourier Transform Spectrometersmentioning

confidence: 99%

Visible/Infrared Imaging Spectroscopy and Energy-Resolving Detectors

Eisenhauer

Raab

2015

Annu. Rev. Astron. Astrophys.

View full text Add to dashboard Cite

Imaging spectroscopy has seen rapid progress over the past 25 years, leading to breakthroughs in many fields of astronomy that would not have been otherwise possible. This review overviews the visible/infrared imaging spectroscopy techniques as well as energy-resolving detectors. We introduce the working principle of scanning Fabry-Perot and Fourier transform spectrometers and explain the most common integral field concepts based on mirror slicers, lenslet arrays, and fibers. The main advantage of integral field spectrographs is the simultaneous measurement of spatial and spectral information. Although Fabry-Perot and Fourier transform spectrometers can provide a larger field of view, it is ultimately the higher sensitivity of integral field units that make them the technique of choice. This is arguably the case for image slicers, which make the most efficient use of the available detector pixels and have equal or higher transmission than lenslet arrays and fiber integral field units, respectively. We also address the more specific issues of large étendue operation, focal ratio degradation, anamorphic magnification, and diffraction-limited operation. This review also covers the emerging technology of energy-resolving detectors, which promise very simple and efficient instrument designs. These energy-resolving detectors are based on superconducting thin film technology and exploit either the very small superconducting energy to count the number of quasi-particles excited in the absorption of the photon or the extremely steep phase transition between the normal- and superconducting phase to measure a temperature increase. We have put special emphasis on an overview of the underlying physical phenomena as well as on the recent technological progress and astronomical path finder experiments.

show abstract

“…A similar lens mount design was successfully used in the CFHT Redeye Camera. 8 The axial position of the camera doublet may be manually adjusted for focusing by rotating the lens barrel housing with respect to the dichroic tube in increments of 0.001 inch/hole. This allows precise plement of the relayed focal plane inside NSFCAM.…”

Section: Mechanical Subsystemmentioning

confidence: 99%

<title>CoCo: an infrared cold coronagraph for astronomical observations</title>

Wang¹,

Owensby²,

Toomey³

et al. 1994

Instrumentation in Astronomy VIII

Self Cite

View full text Add to dashboard Cite

This paper deScribeS the design of an infrared Cold Coronagraph (CoCo) built for use at the NASA 3-rn Infrared Telescope Facility (IRFF) at Mauna Kea Observatory for 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 111ff NSFCAM, which covers 1-5 jim and uses a 256x256 InSb array. The platescale can be varied from 0.06"/pixel to 0.1 5/ucl. covering a field of view of 14" and 38", respectively. Selectable apodized and hard occulting masks are mounted an a ibed as the first element in the system to reduce scattered light. Selectable pupil masks are cooled to 77K within tbe ('Co 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.

show abstract

Canada-France-Hawaii telescope near-infrared camera project

Cited by 5 publications

References 0 publications

NIRIM: A Dual‐Purpose Near‐Infrared (0.76–2.5 μm) Imaging Camera for Wide‐Field and High‐Resolution Imaging

NIRIM: A Dual‐Purpose Near‐Infrared (0.76–2.5 μm) Imaging Camera for Wide‐Field and High‐Resolution Imaging

Visible/Infrared Imaging Spectroscopy and Energy-Resolving Detectors

<title>CoCo: an infrared cold coronagraph for astronomical observations</title>

Contact Info

Product

Resources

About