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Data Reduction

IRAF tools have been developed by Gemini staff to expedite reduction of Mid-IR data. Scripts for basic imaging and spectral data processing of Michelle and T-ReCS data have been released as part of the Gemini IRAF package. These are found in the midir package under the main Gemini IRAF package. Tasks are also available for very basic imaging polarimetry reductions, but these should normally be used just to obtain images at the different waveplate positions.

MIR Baseline Calibrations

For all queue observations, a set of "baseline" calibrations is required to ensure the long-term utility of data in the archive. The baseline calibration set will vary with mode (and sometimes instrument) but includes all the observations deemed necessary to produce scientifically useful data. PIs are free to request additional calibrations beyond the baseline set. However, while baseline calibrations are not charged to the program, additional calibrations are charged to the program and time to observe them must be included in the original proposal.

Polarimetry: special conditions

Michelle's imaging polarimetry capabilities are described in detail in the Michelle-specific pages; here we outline the special S/N requirements for polarimetric measurements and the weather conditions necessary for these to be obtained.

Polarisation accuracy and signal-to-noise ratio

Mid-IR Observing Strategies

On this page we describe the principal observing and calibration issues that users of Gemini's mid-IR instruments should consider when planning their programs and writing their proposals. We recommend that proposers weigh the importance of each issue to their program's scientific goals and formulate their observing plans accordingly. For Michelle and T-ReCS, the principal concerns are the relatively small field of view, the need to chop and nod, and the restricted chopping amplitude. A secondary concern is astrometric accuracy.

Introduction to Ground-based Mid-IR Observing

Compared to observing from space platforms such as Spitzer, observing at mid-IR wavelengths from large ground-based telescopes on good sites brings two principal benefits. First the image quality from such sites is usually diffraction limited (thus scaling with the telescope diameter) and therefore on Gemini, for example, is higher by more than an order of magnitude than on mid-IR space telescopes such as Spitzer.

Tables of transmission and S/N in various filters

                   ON MAUNA KEA AND CERRO PACHO
           (S/N est. includes 4% telescope + instrument emissivity)

                                     MAUNA KEA

                Transmission                    S/N (norm to secz=1,1mm H2O)
        1.0mm   1.6mm   3.0mm   5.0mm   H2O     1.0mm   1.6mm   3.0mm  5.0mm