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Phoenix is a high spectral resolution (R ~ 50,000 - 80,000) near-IR (1-5µm) echelle spectrometer built by NOAO and previously used on the Kitt Peak National Observatory 2m and 4m telescopes. An individual spectrum generated by Phoenix is single order (no cross disperser available) and covers a (very narrow) wavelength range of 0.5% of the central wavelength, corresponding to a radial velocity range of only 1500 km/sec. Blocking of other echelle orders is achieved using order-sorting filters. A large number of filters is available but collectively the filters do not cover every wavelength in the 1-5µm interval.

Phoenix contains a 63.4 degree echelle with 32 lines per millimeter giving a resolving power dispersion of about 2 x 105 per pixel. Slits of length 14 arcsec and width 2, 3, and 4 pixels are available; resolving powers for the narrower slits are somewhat less than would be obtained for perfect optics. An argon hollow cathode wavelength calibration source is supplied with the instrument.

Phoenix uses the NOAO Wildfire instrument controller, with output data format to IRAF images. Phoenix is not a Gemini facility instrument; it has its own dedicated computer for instrument control and data management. However, it is integrated into the telescope control system through the Visitor Instrument Interface (VII), enabling efficient telescope offsetting sequences. With the installation of a Gemini-supplied 512 x 1024 InSb Aladdin II array, Phoenix performance was greatly improved over its past performance at Kitt Peak.

The Instrument Scientist for Phoenix is Ken Hinkle (NOAO).


August 31, 2015: Phoenix rises again as a vistitor instrument at Gemini South in 2016A.

See the Status and Availability pages more information.

Phoenix Science Highlights

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How to Use These Pages

For the most up-to-date information on Phoenix, including an integration time calculator, visit the NOAO Phoenix webpage.  


The Phoenix pages are organized as follows:

Also see the Near-IR Resources section, which contains generic information about observing at 1-5um as well as details about calibrations, standard stars, etc. that apply to NIRI, GNIRS, NIFS, and FLAMINGOS2.