The instruments listed below are available for visitor use on KPNO telescopes during the current observing semester, unless noted otherwise.
|
Proposals for the 2010B (August 2010 - January 2011) observing semester are due March 31, 2010. The list of instruments available for this observing period can be found at http://www.noao.edu/noaoprop/help/facilities.html. This list is revised twice a year and and is available as well in the NOAO Newsletters (March and September issues). |
Observers may also wish to review the material provided in two general users guides, one for low-to-moderate resolution optical spectroscopy and one for direct imaging. See also the pages KPNO direct imaging options and KPNO spectroscopic capabilities for additional information.
Visitor instrumentation is welcome at KPNO and can be scheduled if the instrument: a) is unique; b) is required for a project of very high scientific merit; c) conforms to block scheduling; and d) has small impact on KPNO operational and engineering resources.
| SPECTROSCOPY | ||||
|---|---|---|---|---|
| Detector* | Resolution | long-slit | multi-object capability | |
| Mayall 4-m Telescope | ||||
| R-C CCD Spectrograph (RCSPL, RCSPM) | T2KB/LB1A/F3KB CCD | 300-5000 | 5.4' | single or multi-slit |
| Multi-Aperture Red Spectrometer (MARS, MARSM) | LB1A CCD (1980x800) | 300-1500 | 5.4' | single or multi-slit |
| CCD Echelle Spectrograph (ECHLR, ECHLB, ECHUV) | T2KB/F3KB CCD | 18,000-65,000 | 2.0' | |
| FLAMINGOS IR Imaging Spectrometer [1](FLMNL/FLMNM) | HgCdTe (2048x2048, 0.9-2.5μm) | 1,000-1,900 | 10.3' | single or multi-slit |
| IRMOS InfraRed Multi-Object Spectrograph [2] (IRMOS) | HgCdTe (1024x1024, 0.9-2.5μm) | 300/1000/3000 | 3.4' | single or multi-slit or imaging |
| WIYN 3.5-m Telescope [3] (IMPORTANT -Check Web for Update) | ||||
| Hydra + Bench spectrograph [4] (HYDRB, HYDRR) | STA1 CCD | 700-22,000 | NA | ~85 fibers |
| SparsePak [5] + Bench spectrograph [4] (SPSPKB, SPSPKR) | STA1 CCD | 700-22,000 | IFU | ~82 fibers |
| 2.1-m Telescope | ||||
| GoldCam CCD Spectrograph (GCAM) | F3KA CCD | 300-4500 | 5.2' | |
| FLAMINGOS IR Imaging Spectrometer [1] (FLMNL) | HgCdTe (2048x2048, 0.9-2.5μm) | 1,000-1,900 | 20.0' | long slit only |
| *Unless otherwise noted, CCDs have 3300-9700Å spectral range. | ||||
| [1] FLAMINGOS Spectral Resolution given assuming 2-pixel slit. Not all slits cover full field; check instrument manual. FLAMINGOS was built by the late Richard Elston and his collaborators at the University of Florida. Dr. Steve Eikenberry is the current PI of the instrument. | ||||
| [2] IRMOS was built by Dr. John MacKenty (STScI) and collaborators. Availability will depend on proposal demand and block scheduling constraints. | ||||
| [3] The availability of the WIYN 3.5m for science observations during 2010B is being evaluated due to the anticipated arrival of the One Degree Imager (ODI) for installation and commissioning sometime in the fall of 2010. Please check the web page ODI Status for updates prior to preparing your proposal for WIYN 3.5m observing time. Please also feel free to contact kpno@noao.edu with questions. | ||||
| [4] The Bench Spectrograph has recently been upgraded. A new CCD (STA1), a new collimator, and two new Volume Phase Holographic (VPH) gratings (740 l/mm and 3300 l/mm), are now available for use. Dispersion and wavelength range remain essentially the same in the upgraded system. However, observers should view Bench Upgrade for further details of changes in throughput and instrumental resolution, as well as new options, such as binning and gain choices, to help plan observations. Observers requesting the Simmons camera should note that the combination of the new CCD and new collimator constrains the number of fibers projected onto the CCD. | ||||
| [5] Integral Field Unit 80"x80" field, 5" fibers, graduated spacing. | ||||
| [6] The MOSAIC-1 camera will be upgraded during 2010 with new E2v CCDs and Monsoon based controllers. The improved instrument is currently scheduled to be recommissioned at the Mayall 4m during September and October 2010. We intend to offer shared risk observing with the upgraded instrument in the latter half of the 2010B observing semester. The instrument will not be available for science programs at the WIYN 0.9m during 2010B. Note: there will be slightly different inter-detector gaps, but the pixel scale remains unchanged. Owing to the new configuration, which includes two outputs per device, readout time will be significantly reduced. See Mosaic-1 Upgrade for further details. | ||||
| [7] The availabilty of the OPTIC camera from the University of Hawaii is unknown for 2010B. OPTIC has been available in the past through an agreement with John Tonry of the University of Hawaii. Please see footnote [3] above for further information regarding WIYN 3.5m science proposals. | ||||
| [8] WHIRC was built by Dr. Margaret Meixner (STSci) and collaborators. The availability of this instrument for science observing during 2010B is subject to the same uncertainty affecting all WIYN 3.5m science proposals. Please see footnote [3] above. Observers contemplating use with WTTM correction should consult with Dick Joyce or Lori Allen for details. | ||||
| [9] While T2KB is the default CCD for CFIM, use of F3KB may be justified for some applications and may be specifically requested: scale 0.19"/pixel, 9.7'x3.2' field. If T2KB is unavailable, CFIM may be offered with T2KA (scale: 0.305"/pixel, 10.4' field) or with F3KB to best match proposal requirements. See CCD Characteristics for further details on CCD characteristics. | ||||
| [10] The planned upgrade of MOSAIC-1 (see footnote [6]) will prevent use of Mosacic-1 or the upgraded instrument at the WIYN 0.9m. No proposals will be accepted for NOAO time on the WIYN 0.9m during 2010B. | ||||
| IMAGING | ||||
|---|---|---|---|---|
| Detector | Spectral Range | scale (""/pixel) |
Field-of-View | |
| Mayall 4-m Telescope | ||||
| CCD MOSAIC (MOSA) | 8Kx8K (8-2Kx4K) CCD | 3500-9700Å | 0".26 | 35'.4 |
| Simulataneous Quad IR Imager (SQIID) | InSb (3-512x512 illuminated), 0.9-2.5μm) | simultaneous JHKs | 0".39 | 3.3' |
| FLAMINGOS IR Imaging Spectrometer (FLMN) | HgCdTe (2048x2048, 0.9-2.5μm) | JHK | 0".32 | 10.3' |
| WIYN 3.5-m Telescope [3] (IMPORTANT -Check Web for Update) | ||||
| Mini-Mosaic Imager [7] (MIMO) | 4Kx4K (2-2Kx4K) CCD | 3300-9700Å | 0".14 | 9'.5 |
| U. Hawaii OPTIC Camera[7] (OPTIC) | 4KX4K (2-2Kx4K) OTCCD | 3500-9700Å | 0".14 | 9'.5 |
| WHIRC[8] |
HgCdTe (2048x2048, 0.9-2.5μm) |
JHK |
0".10 | 3'.3 |
| 2.1-m Telescope | ||||
| CCD Imager[9] (CFIM) | T2KA | 3300-9700Å | 0.305" | 10'.4 |
| Simultaneous Quad IR Imager (SQIID) | InSb (3-512x512 illuminated, 0.9-2.5μm) | simultaneous JHKs | 0.68' | 5.8' |
| FLAMINGOS IR Imaging Spectrometer [1](FLMN) | HgCdTe (2048x2048, 0.9-2.5μm) | JHK | 0.61" | 20.0' |
| WIYN 0.9-m Telescope | ||||
| CCD Mosaic (MOSA) [10] | 8Kx8K (2-2Kx4K) CCD | 3300-9700Å | 0".425 | 59' |
Go to: Kitt Peak home page