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: http://xmm.vilspa.esa.es/sas/6.0.0/doc/flspec/node3.html
Дата изменения: Thu Mar 18 23:54:37 2004 Дата индексирования: Sat Dec 22 07:36:39 2007 Кодировка: Поисковые слова: comet tail |
flspec computes the spectrum of the background fluctuations in EPIC Imaging data.
The first step of the process is the 'flatfielding' (division) of the input image with the corresponding exposure map. Since the borders of the exposure map can be affected by counting statistics, it is previously 'cleaned' with the output of emask using a value of 0.1 as a threshold, i.e, only the area of the map with exposure time greater than 100% of maximum value is retained. Then the regions affected by the observed sources (listed in the input source list) are removed taking into account the sizes obtained with the task region (radiusmode=enfrac with an enclosed energy fraction of 95%).
Once the 'flatfielded' image is free from detected sources, its pixels are binned according to the input parameter binsize and classified as 'positive' (if they have more counts than the median in the image) and 'negative' pixels (less counts than the median). Those binned pixels with positive(negative) label will lead to pixels with ``1'' (``0'') in the positive(negative) mask that flspec creates with the pixel size of the input image. Those pixels that have null value in the flatfielded image (0 secs. in exposure time or pixel inside a region source) are kept as ``0'' in both masks.
These masks are then used to filter the input event list and extract positive(negative) spectra from a number of annuli around the image centre, to account for variations of the effective area as a function of the offaxis angle. The positive and negative spectra are extracted with an spectral binning of 15 eV (MOS) and 5 eV (PN).
Once created, positive and negative spectra are subtracted to obtain the 'fluctuations' spectrum in each annular region.
The subtraction is performed normalising the solid angle in units of detector pixels (squared pixels of side 0.05 arcseconds) to that of the extraction region for the positve spectrum, i.e.,
difference= positive_spec - (solid_angle_positive/solid_angle_negative)*negative_spec.
The BACKSCAL attribute in this difference spectrum will then keep the value of the solid angle for the positive one. Provided one of these positive/negative spectra has zero area, a warning is raised and the difference spectrum stores the non zero area value in the BACKSCAL attribute:
difference= positive_spec - 0.0*negative_spec
or
difference= 0.0*positive_spec - negative_spec
BACKSCAL=0 if both spectra have null extraction area.
Finally all these 'difference' spectra are stored in a unique multiple spectral file by the task specadd. See documentation of task specadd for a description of the format of this output multiple spectral file. In the particular case of the fluctuations spectra, the column ROWID stores the offaxis at which the spectrum has been calculated.
If the observation is confusion dominated (as will be the case in most of them), the fluctuation spectrum is related to the average spectrum of the sources that dominate the fluctuations (below the detection threshold). This is necessary to estimate the systematic errors in the spectra of the faint detected sources.
Otherwise, if the observation is counting-noise limited, the spectrum of the fluctuations gives the shapes of the errors in the spectra of the faint detected sources.