Detector* Resolution Slit Multi-object
Mayall 4-m Telescope
R-C CCD Spectrograph (RCSP) T2KB CCD 300-5000 5.4' single/multi
CCD Echelle Spectrograph
(ECH) T2KB CCD 18,500-65,000 2.0'
IR Cryogenic Spectrometer
(CRSP) InSb(256×256, 0.9-5.5µm) 300-1500 0.8'
CryoCam (CRYO) Loral CCD (800×1200) 400-600 4.5' single/multi
Imaging Spectrometer (ONIS) InSb(512×1024, 0.9-2.5µm) 1400 1.5'
High Resolution IR Spectro-
meter (Phoenix; PHX)
(see note 1) InSb(256×1024, 0.9-5.5µm) 50,000-100,000 0.5'
WIYN 3.5-m Telescope
Hydra + Bench
Spectrograph (HYDR) T2KC CCD 700-22,000 NA 100 fibers
DensePak (see note 2) T2KC CCD 700-22,000 IFU ~90 fibers
2.1-m Telescope
GoldCam CCD
Spectrograph (GCAM) F3KA CCD 300-4500 5.2'
IR Cryogenic
Spectrometer (CRSP) InSb(256×256, 0.9-5.5µm) 300-1500 1.3'
High Resolution IR Spectro-
meter (Phoenix; PHX)
(see note 1) InSb(256×1024, 0.9-5.5µm) 50,000-100,000 1.0'
OSU-NOAO Infrared Imaging
Spectrometer (ONIS) InSb(512×1024, 0.9-2.5µm) 1400 3.0'
Coude-Feed Telescope (see note 3)
Coude CCD Spectrograph
(CF; CAM5 or CAM6) F3KB CCD 2200-250,000 3.0'
Detector Spectral Range Scale ("/pixel) Field
Mayall 4-m Telescope
Prime Focus CCD camera (PF) T2KB CCD 3300-9700Å 0.42 14.2'
IR Imager (IRIM) HgCdTe
(256x256, 1-2.5µm) JHK + NB 0.60 2.5'
CCD Mosaic
(MOSA) (see note 4) 8Kx8K 4500-9700Å 0.26 35.4'
OSU-NOAO Infrared InSb
Imaging Spectrometer (ONIS) (512×1024, 0.9-2.5µm) JHK 0.18/0.09 3'x1.5'/1.5'x0.75'
WIYN 3.5-m Telescope
CCD Imager (WIYN) S2KB 3300-9700Å 0.197 6.7'
2.1-m Telescope
CCD Imager (DIR) T1KA 3300-9700Å 0.305 5.2'
IR Imager (IRIM) HgCdTe
(256×256, 1-2.5µm) JHK + NB 1.1 4.7'
OSU-NOAO Infrared
Imaging Spectrometer (ONIS) InSb
(512×1024, 0.9-2.5µm) JHK 0.35; 0.18 6'x3'/3'x1.5'
0.9-m Telescope
CCD Imager (DIR) T2KA 3300-9700Å 0.680 23.2'
CCD Mosaic (MOSA) (see note 4) 8Kx8K 4500-9700Å 0.425 59.0'
* Unless otherwise noted, CCDs have 3300-9700Å spectral range.
1 Phoenix is likely to be shipped to CTIO in third quarter 1998 and not available at KPNO.
2 New capability for February-July 1998 (Integrated Field Unit: 30" × 45" field, 3" fibers, 4" fiber spacing)
3 Will be continued until fiber-feed capability is available elsewhere.
4 To minimize the number of instrument installations, the CCD Mosaic Imager will be available for block-scheduled, shared-risk observing on the 4-m and 0.9-m telescopes, with priority given to 4-m use. Check the CCD Mosaic WWW page for updates concerning new filters and progress toward replacing the current engineering-grade CCDs (the default for all of semester II 1997) with science-grade CCDs.