Difference between revisions of "Aperture Photometry Overview"
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=Aperture Photometry= | =Aperture Photometry= | ||
| − | ''Much of this text was ruthlessly copied without permission from the document entitled "Photometry Using IRAF" by Lisa A. Wells, from 1994, found on the [http://iraf.noao.edu/docs/photom.html IRAF photometry documentation page].'' | + | ''Much of this text was originally ruthlessly copied without permission from the document entitled "Photometry Using IRAF" by Lisa A. Wells, from 1994, found on the [http://iraf.noao.edu/docs/photom.html IRAF photometry documentation page].'' |
There are many techniques involved in doing aperture photometry and these methods vary from one astronomer to another. Some observers use large apertures for their measurements to account for seeing, tracking, and focus variations, while others use small | There are many techniques involved in doing aperture photometry and these methods vary from one astronomer to another. Some observers use large apertures for their measurements to account for seeing, tracking, and focus variations, while others use small | ||
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Space-based data does not have to worry about variations in seeing and focus (generally), and the sky background is a function primarily of the direction in which you are looking. Moreover, space-based data usually arrive on your desktop already calibrated. So, space-based data are much easier to process than ground-based data. However, you still need to use care in selecting your photometry reduction parameters, because it is very easy to shoot yourself in the foot. | Space-based data does not have to worry about variations in seeing and focus (generally), and the sky background is a function primarily of the direction in which you are looking. Moreover, space-based data usually arrive on your desktop already calibrated. So, space-based data are much easier to process than ground-based data. However, you still need to use care in selecting your photometry reduction parameters, because it is very easy to shoot yourself in the foot. | ||
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Some references on the theory and techniques of aperture photometry are | Some references on the theory and techniques of aperture photometry are | ||
| − | + | *Golay, M., "Introduction to Astronomical Photometry," D. Reidel Publishing, Dordrecht, Holland | |
| − | Dordrecht | + | *Hardie, Robert H., 1962, in "Stars and Stellar Systems," Vol. 2, "Astronomical Techniques", ed. W. A. Hiltner, University of Chicago Press, 178 |
| − | Holland | + | *Harris, W. E., 1990, PASP, 102, 949 |
| − | + | *Harris, W. E., FitzGerald, M. P., and Reed, B. C., 1981, PASP, 93, 507 | |
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Howell S B PASP | Howell S B PASP | ||
Howell S B ed Astronomical CCD Observing and Reduction Techniques | Howell S B ed Astronomical CCD Observing and Reduction Techniques | ||
Revision as of 00:11, 15 May 2008
Aperture Photometry
Much of this text was originally ruthlessly copied without permission from the document entitled "Photometry Using IRAF" by Lisa A. Wells, from 1994, found on the IRAF photometry documentation page.
There are many techniques involved in doing aperture photometry and these methods vary from one astronomer to another. Some observers use large apertures for their measurements to account for seeing, tracking, and focus variations, while others use small apertures and apply aperture corrections. The sky algorithm used may vary according to the chip characteristics and the data There are a number of ways to do the standard calibration so be sure to observe standards in a way that is compatible with the calibration package you wish to use.
Space-based data does not have to worry about variations in seeing and focus (generally), and the sky background is a function primarily of the direction in which you are looking. Moreover, space-based data usually arrive on your desktop already calibrated. So, space-based data are much easier to process than ground-based data. However, you still need to use care in selecting your photometry reduction parameters, because it is very easy to shoot yourself in the foot.
Some references on the theory and techniques of aperture photometry are
- Golay, M., "Introduction to Astronomical Photometry," D. Reidel Publishing, Dordrecht, Holland
- Hardie, Robert H., 1962, in "Stars and Stellar Systems," Vol. 2, "Astronomical Techniques", ed. W. A. Hiltner, University of Chicago Press, 178
- Harris, W. E., 1990, PASP, 102, 949
- Harris, W. E., FitzGerald, M. P., and Reed, B. C., 1981, PASP, 93, 507
Howell S B PASP Howell S B ed Astronomical CCD Observing and Reduction Techniques ASP Conf Series Vol Philip A G Davis ed Problems of Calibration of Multicolor Photometric Systems Dudley Observatory Schenectady New York Stetson P B PASP Stetson P B PASP Stetson P B and Harris W E AJ The basic principle of aperture photometry is to sum up the observed ux within a given radius from the center of an object then subtract the total contribution of the sky background within the same region leaving only the ux from the object to calculate an instrumental magnitude The aperture size is important since seeing tracking and focus errors a ect the amount of ux within the stellar pro le The noise grows linearly with radius as the stellar ux trails o in the wings of the pro le Increasing the size of the aperture will increase the poisson shot noise of the background sky and any at
eld
errors that may be nearby The signal to noise ratio of the ux measurement reaches a maximum at an intermediate aperture radius shown by Howell referenced above The use of a smaller radius introduces the problem that the fraction of the total ux measured will vary for objects of di erent ux from image to image Aperture corrections must be used in this latter case see Section If the user is interested in applying an extinction correction to the data then extinction stars need to be observed and reduced along with the object data The extinction stars should be observed at airmasses corresponding to the range in airmass of the program objects a range of not less than magnitudes in extinction is suggested so that a good airmass correction can be determined and applied to the data Color and zero point corrections are often applied to the instrumental magnitudes as well to put them on the standard system de ned by a set of observed standard stars these same standard stars can also be used as the extinction stars These stars should be chosen prior to observing so that their colors bracket those of the program objects a good rule of thumb is to have at least a magnitude range in the colors of the standards to determine reasonable calibrations See Section for details IRAF currently provides a means of creating polygonal and elliptical aperture lists for use with speci c tasks Elliptical apertures may also be used to perform isophotal surface photometry on galaxies The next section brie y describes the many options
