1993
DOI: 10.1117/12.158703
|View full text |Cite
|
Sign up to set email alerts
|

Canada-France-Hawaii telescope near-infrared camera project

Help me understand this report

Search citation statements

Order By: Relevance

Paper Sections

Select...
2
1
1
1

Citation Types

0
5
0

Year Published

1994
1994
2015
2015

Publication Types

Select...
3
2

Relationship

1
4

Authors

Journals

citations
Cited by 5 publications
(5 citation statements)
references
References 0 publications
0
5
0
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%
“…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%
“…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%
“…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%