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Observing Strategies

Nod size: Like all infrared spectrographs, observations are taken in pairs (ab) or quads (abba) in order to remove sky emission. For small sources (angular dimensions are much less than the slit length of 14 arcsec), the telescope is nodded back and forth along the slit. For large sources the telescope is nodded between the source and blank sky. For pointlike sources nods are thus very small.

Exposure Times

Due to its very high spectral resolution exposure times with Phoenix can be very long. In the JHK windows spectroscopic exposure times of 10,000 seconds on a tenth magnitude star would be needed to saturate the array. Since we are currently unable to abort an exposure in progress, we typically limit the exposure time to 900s.


In the thermal infrared (LL'M) saturation times on the sky and telescope background are 300 seconds near 3µm and 30 seconds near 5µm and limit the individual exposure times.

Slits

Slit name Slit width
(arcsec)
Slit length

Blocking Filters

The table below lists all filters, including the wavenumbers/wavelengths of half the maximum transmission, that are available for use with Phoenix. Note that the CVF filters described in the NOAO Instrument Manual are no longer available. The second filter wheel is called CVF for historical reasons only.

Calibration

Near-IR calibrations are discussed in detail on the general near-IR web pages, as they are generally similar for all Gemini near-IR imagers and spectrographs. A baseline calibration set (not charged to the PI) is taken for each observation, generally the minimum calibrations necessary to ensure the utility of the observations in the archive.

Documents

In addition to the general acknowledgment to the Gemini Observatory, the following specific acknowledgment should be included in any paper containing Phoenix data:


This paper is based on observations obtained with the Phoenix infrared
spectrograph, developed and operated by the National Optical Astronomy
Observatory.

Data Format and Reduction

Phoenix data are formatted into IRAF compatible images (fits files). Gemini does not provide a specific IRAF package for Phoenix, but the data reduction process is straightforward and documented in the NOAO Phoenix web pages.

Observation Preparation

This section describes how to prepare and check Phoenix observations.

Guiding Options

Phoenix does not contain an on-instrument wavefront sensor and therefore the fast tip-tilt guiding, which is mandatory for all observations with Gemini, requires guide stars to be acquired using the facility peripheral wavefront sensor (usually PWFS-2).

Sensitivity and Overheads

It is recommended that the user consult the Sensitivity Table or the Sensitivity Plots to estimate limiting magnitudes and total integration times.