10.1 Analysis of Scanned Data
Spatial scans enable observations of bright sources such as host stars of 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, for which an established pipeline is provided to the users, namely (calwf3, see Chapter 3).
For spatially scanned data the observers are required to customize a larger fraction of their analysis with respect to the typical staring mode of observation. In this section, we describe custom analysis flows for scanned A) IR spectroscopy, especially of exoplanet transits or eclipses, and B) UVIS and IR imaging. UVIS scanned spectroscopy is not recommended, due to order overlap.
To begin their own custom analysis, we recommend observers use:
- _ima.fits files for IR
- _flt.fits or _flc.fits files for UVIS observation
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WFC3 Data Handbook
- • Acknowledgments
- Preface
- Chapter 1: WFC3 Instruments
- Chapter 2: WFC3 Data Structure
- Chapter 3: WFC3 Data Calibration
- Chapter 4: WFC3 Images: Distortion Correction and AstroDrizzle
- Chapter 5: WFC3-UVIS Sources of Error
- Chapter 6: WFC3 UVIS Charge Transfer Efficiency - CTE
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Chapter 7: WFC3 IR Sources of Error
- • 7.1 WFC3 IR Error Source Overview
- • 7.2 Gain
- • 7.3 WFC3 IR Bias Correction
- • 7.4 WFC3 Dark Current and Banding
- • 7.5 Blobs
- • 7.6 Detector Nonlinearity Issues
- • 7.7 Count Rate Non-Linearity
- • 7.8 IR Flat Fields
- • 7.9 Pixel Defects and Bad Imaging Regions
- • 7.10 Time Variable Background Contamination
- • 7.11 IR Photometry Errors
- • 7.12 References
- Chapter 8: Persistence in WFC3 IR
- Chapter 9: WFC3 Data Analysis
- Chapter 10: WFC3 Spatial Scan Data