WFC3 Data Handbook V. 4.0

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10.1	Analysis of Scanned Data

Spatial scans enable observations of bright sources and exoplanets, as well as high precision astrometry and photometry. However, the analysis of spatially scanned data obtained with HST WFC3 is different from that of nominal, staring-mode observations. calwf3 is designed for the typical static mode, thus, for spatially scanned data the observer must perform more of the analysis herself than for staring-mode data. In this section, we describe custom analyses for A) IR spectroscopy, especially of exoplanet transits or eclipses, and B) UVIS and IR imaging. UVIS scanned spectroscopy is not recommended.

To begin their own custom analysis, we recommend observers use:

•	* _ima.fits files for IR data

•	* _flt.fits files for UVIS data.