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Updated: Sept 23, 2013

KPNO Telescopes-Instrument Capabilities


The instruments listed below are available for visitor use on KPNO telescopes during the current observing semester, unless noted otherwise.

Proposals for the 2014A (February 2043 - July 2014) observing semester are due September 26, 2013. 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.


Instruments currently in use

SPECTROSCOPY

Detector* Resolution long-slit multi-object capability
Mayall 4-m Telescope



R-C CCD Spectrograph 1 (RCSPL, RCSPM) T2KA/LB1A CCD 300-5000 5.4' single or multi-slit
KOSMOS 2 e2v CCD 2400 up to 10' single or multi-slit
CCD Echelle Spectrograph 1 (ECHLR, ECHLB, ECHUV) T2KA CCD 18,000-65,000 2.0' single
Phoenix 3 InSb (512x1024, 1-5μm) 50,000-70,000 30" single





WIYN 3.5-m Telescope



Hydra + Bench spectrograph 4 (HYDRB, HYDRR) STA1 CCD 700-22,000 NA ~82 fibers
SparsePak 5 (SPSPKB, SPSPKR) STA1 CCD 400-13,000 IFU ~82 fibers





1PIs can propose for RC Spec in 14A, but projects which can be moved to KOSMOS, upon its successful commissioning in 14A, will be. T2KA is default CCD for RCSP and ECH. T2KB now serves as T2KA's backup. LB1A may be requested for RCSP if appropriate.
2PIs should write proposals using the capabilities offered by RCSP. If the science requirements could be met by the initial capabilities of KOSMOS, PIs should specifically indicate an interest in adapting the proposal for KOSMOS when writing the Technical Description section. See page 16 of the March 2012 NOAO Newsletter for more details.
3See http://www.noao.edu/kpno/phoenix/ before preparing the proposal
4One degree field with two fiber bundles of ∼ 85 fibers each. "Blue" (3") and "Red" (2") fibers. See article in this NOAO Newsletter referring to block scheduling of this instrument.
5Integral Field Unit, 80" x 80" field, 5" fibers, graduated spacing. See article this NOAO Newsletter referring to block scheduling of this instrument.

IMAGING

Detector Spectral Range scale
(""/pixel)
Field-of-View
Mayall 4-m Telescope



CCD MOSAIC 1.1 (MOSA) 8K x 8K 3500-9700Å 0.26 35.4'
NEWFIRM 6 InSb (mosaic, 4, 2048 x 2048) 1-2.3μm 0.4 28.0'





WIYN 3.5-m Telescope



pODI 7 12Kx12K central + 4 (4Kx4K) distributed 3600-9500Å 0.11 24'x24' central
WHIRC 8
VIRGO HgCdTe (2048x2048)
0.9-2.5μm
0.10 3.3'





2.1-m Telescope



CCD Imager 9 (CFIM) STA CCD 3300-9700Å 0.305 (DEC)





WIYN 0.9-m Telescope



HDI 10 4K x 4K 3000-9700Å 0.43 29.2'





6Permanently installed filters include J, H, Ks. See http://www.noao.edu/ets/newfirm for further information and for filter availability, and policy on filter changes.
7Due to the scheduled upgrade to pODI, proposals will be accepted for February and March only.
8WHIRC was built by Dr. Margaret Meixner (STScI) and collaborators. Potential users requiring WTTM are advised to contact KPNO support staff for details on its current status before making a proposal and http://www.wiyn.org/Observe/status.html for any updates.
9An STA CCD with Monsoon Controller will become the default CCD for the 2.1m; T2KB will serve as backup. Lab performance will be made available as soon as possible, meanwhile contact KPNO support staff for further information.
10Availability of HDI is anticipated beginning in 2014A, pending successful commissioning.







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