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Basic characteristics of T-ReCS's imaging mode
Taken from the current T-ReCS Intro page
The following five tables provide various exposure time limits. Constraints are due to a number of factors, more than one of which may need to be considered for a given NIRI configuration:
This section mainly describes how to prepare and check NIRI observations. Setting up observing sequences at Phase II is not intuitive until one is quite experienced (and maybe even not then). Thus, the key to successful observation preparation is starting from the NIRI OT Library.
NIRI standalone (i.e., without AO) requires the use of a peripheral wavefront sensor for both imaging and spectroscopy. PWFS2 is preferred over PWFS1, as it can be used on fainter guide stars, can run at a higher frequency for a given guide star, works better under windy and cloudy conditions, and is smaller and thus vignettes less of the field of view.
Low-moderate resolution spectroscopy can be obtained either at f/6 through each of the 1-5μm windows or at f/32 (the latter usually with adaptive optics) at JHK only. A variety of slit widths are available. The properties of the slits, grisms, and blocking filters are decribed in the section. The f/6 and f/32 pixel scales in spectroscopy mode are the same as those in imaging mode.
Below are papers describing aspects of Michelle's design, fabrication and testing.
The Gemini IRAF MIDIR package has been released, consisting of scripts allowing basic reduction of imaging and spectroscopy data. Given the similarities in the reduction of data from T-ReCS and Michelle, this topic is covered in the mid-IR data reduction pages. The basic format of all Gemini data is explained in the Data section of the Gemini website.
This page guides you through the main steps and considerations for configuring Michelle observations in the Observing Tool (OT).