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Input Data and Preprocessing

The information involved in a reduction session consists of user data and system tables. User data is a set of echelle images, observed with the same instrument configuration, including a wavelength calibration image (WLC), a flat field image (FLAT) and astronomical objects OBJ. Optionally, this set will include standard stars (STD) to be used in the absolute or relative flux calibration, and dark images (DARK). Catalogues with comparison lines and absolute fluxes for standard stars are available in the system as MIDAS tables.

Before starting the actual reduction some preprocessing of the data is required to correct for standard detector effects as follows:


next up previous contents
Next: Retrieving demonstration and calibration Up: Echelle Reduction Method Previous: Echelle Reduction Method
http://www.eso.org/midas/midas-support.html
1999-06-15