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: http://xmm.vilspa.esa.es/sas/8.0.0/doc/omdetect/node40.html
Дата изменения: Wed Oct 22 17:31:26 2008 Дата индексирования: Tue Aug 18 14:54:13 2009 Кодировка: Поисковые слова: вечный календарь |
When the source-detection algorithms has run omdetect will compute raw count-rates for each detected source. For point-sources (ie those sources having widths consistent with those of the point-spread function) the count-rates are obtained by aperture photometry. For binned and unbinned images the aperture is 6 and 12 pixels, respectively. For a source with one or more neighbours that may be partly within the aperture, a smaller aperture will be used and its size is determined from the distance to its nearest neighbour. The actual aperture radii (unbinned pixels) that were used in the photometry are given in the column APERTURE of the SRCLIST table of the output source-list table.
The background is subtracted using the pixels within an annulus region. For the optical filters the inner and outer diameters of the annulus are 8 and 13 pixels for binned images, respectively, and 14 and 25 pixels for unbinned images, respectively. For the UV filters the inner and outer diameters of the annulus are 19.5 and 22 pixels for binned images, respectively, and 37 and 42 pixels for unbinned images, respectively. These values are stored as the fits keywords INNBCKAN and OUTBCKAN in the primary header of the output source-list file
When each point-source has had its photometry parameters computed, those with a significance of less than or equal to 10 have their photometry computed using an aperture of 6 unbinned pixels, in order to reduce the errors due to the background noise.
These ``raw'' count-rates have to be corrected for coincidence-loss, dead-fraction and the time-dependent sensitivity degradation before instrumental magnitudes can be computed (using the task ommag). Please note that the time-dependent sensitivity correction is applied by ommag. The default aperture is 12 unbinned pixels, but for some sources a smaller aperture may be used. For these cases an aperture correction is also applied using the point-spread function. For the filters UVW1, UVM2 and UVW2 a further point-spread function correction is made to extrapolate the count-rates to an unbinned aperture radius of 35 pixels.
The following summarizes the procedure used to correct the source extracted count-rates for coincidence-losses-
Please note that these coincidence-loss corrections do not contain the factor 1/(1-deadfraction).
The following further corrections will then be applied by ommag-