Sextractor for dummies - METU Astrophysics

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54 CHAPTER 7: SE INPUT: THE CONFIGURATION FILE Original Background ’Filtered’ Objects Segementation Apertures Figure 7.9: Illustration of the different checkimages possible. The original inputimage, the BACK- GROUND image, the FILTERED image, the OBJECTS image, the SEGMENTATION image and the APERTURES image. the contrast of the BACKGROUND image has been exaggerated.
Chapter 8 Output Parameters The catalogs with output parameters is what the whole exercise is all about! 1 You can finally start constructing your Hertzsprung-Russel diagrams or lensing shear fields or whatever. The parameters you want in your catalogs should be listed in the file you gave to PARAMETERS NAME. Unless you keep using the same file for this, I really recommend using ASCII HEAD type catalogs 2 The output catalogs will have a nice header with a list of all the parameters. Parameters in the SE outputcatalog can be divided into geometric parameters ,photometric parameters, astrometric parameters and fitted parameters. 3 Geometric parameters will tell you what shape the object is in (basically how the light of the object is distributed over the pixels of that object) and the photometric parameters tell you simply how much light there is. Astrometric parameters give the position of the object in the image, be it in pixels or other coordinates. 4 Fitted parameters are calculated from fitting for instance a PSF to the data of the object. Most of these are still being developed and do not work yet. 5 There are a few that do not fall in any of these convenient categories; the catalog number, the flag parameters and the parameters associated with crosscorrellating catalogs. Name description unit NUMBER Running object number - FLAGS Extraction flags - IMAFLAGS ISO FLAG-image flags OR’ed over the iso. profile - NIMAFLAGS ISO # flagged pixels entering IMAFLAGS ISO - 1 Well that and the check-images perhaps. 2 By setting the parameter CATALOG TYPE to ASCII HEAD in the configuration file. 3 Just kidding, SE does not fit anything yet. It’s so fast for a reason. 4 There has been some improvement here as well. The now nearly ubiquitous World Coordinate System WCS is also used. 5 Meaning, I’ve tried but have not gotten them to work yet...If you have, let me know.
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The spiff new cover was made by Rob
Page 4 and 5: 4 CONTENTS 7.4 Influencing Photomet
Page 6 and 7: 6 CONTENTS
Page 8 and 9: 8 CHAPTER 1: FOREWORD
Page 10 and 11: 10 CHAPTER 2: INTRODUCTION If you g
Page 12 and 13: 12 CHAPTER 3: PROS AND CONS OF SE H
Page 14 and 15: 14 CHAPTER 4: HOW TO INSTALL SE 4.2
Page 16 and 17: 16 CHAPTER 5: HOW SE WORKS 3. Filte
Page 18 and 19: 18 CHAPTER 5: HOW SE WORKS Figure 5
Page 20 and 21: 20 CHAPTER 6: USING SE of sources a
Page 22 and 23: 22 CHAPTER 7: SE INPUT: THE CONFIGU
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Page 76 and 77: 76 CHAPTER 8: OUTPUT PARAMETERS
Page 78 and 79: 78 CHAPTER 9: STRATEGIES FOR SE USE
Page 84 and 85: 84 CHAPTER 10: AVAILABLE PACKAGES
Page 86 and 87: 86 CHAPTER 11: FOLLOW-UP PROGRAMS
Page 88 and 89: 88 CHAPTER 12: SE USE IN THE LITERA
Page 90 and 91: 90 CHAPTER 12: SE USE IN THE LITERA
Page 92 and 93: 92 CHAPTER 13: KNOWN BUGS AND FEATU
Page 94 and 95: 94 CHAPTER 14: SE PARAMETER ADDITIO
Page 96 and 97: 96 CHAPTER 15: EXAMPLES 15.2 Runnin
Page 98 and 99: 98 CHAPTER 15: EXAMPLES 1 0.8 0.6 0
Page 100 and 101: 100 CHAPTER 16: ACKNOWLEDGMENTS
Page 102 and 103: 102 CHAPTER A: ’DRIZZLE’ AND RM
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104 CHAPTER B: SE PARAMETERS MAG_GA
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106 BIBLIOGRAPHY Fasano, G. and Fil
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108 INDEX Trujillo, I., Aguerri, J.
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110 INDEX DELTAPEAK B1950, 60 DELTA
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112 INDEX XPSF IMAGE, 73 XPSF WORLD
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