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Preface
Data reduction
1. Astronomical Images
1.1. Components of astronomical images
1.2. An artificial, but realistic, image
1.3. Non-uniform sensitivity in astronomical detectors
1.4. Calibration overview
1.5. Image combination
1.6. Overscan
1.7. Calibration choices to make
1.8. Reading images
2. Overscan and bias images
2.1. About bias and overscan
2.2. Calibrating bias images
2.3. Combine bias images to make master bias
3. Dark current and dark frames
3.1. Dark current: the ideal case
3.2. Real dark current: noise and other artifacts
3.3. Handling overscan and bias for dark frames
3.4. Calibrate dark images
3.5. Combine calibrated dark images for use in later reduction steps
4. Flat fielding
4.1. Calibrating flat frames
4.2. Calibrating flat frames
4.3. Combining flat frames
5. Calibrating science images
5.1. Two calibration examples
6. Finding and dealing with bad pixels
6.1. Identifying hot pixels
6.2. Identifying bad pixels with ccdmask
6.3. Removing cosmic rays
6.4. Incorporating masks in science images
Photometry
7. Overview
8. Source detection
8.1. Background estimation
8.1.1. Overview with simulated image
8.1.2. Handling images that need masking
8.1.3. Removing a gradient in a ground-based image
8.2. IRAF-like source detection
8.2.1. Overview with simulated image
8.2.2. Detecting sources in the XDF
8.2.3. Detecting stellar sources in a ground-based image
8.3. Local peak detection
8.3.1. Overview with simulated image
8.3.2. Peak detection in the XDF
8.3.3. Peak detection in a ground-based stellar image
8.4. Image segmentation
8.4.1. Overview with simulated image
8.4.2. Image segmentation in the XDF
8.4.3. Image segmentation in a ground-based stellar image
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