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Дата изменения: Tue Sep 20 19:45:21 2011
Дата индексирования: Mon Apr 11 03:36:19 2016
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Поисковые слова: galactic cluster

Calibration Access and Data Handbook

Description

This CCF component is used by QLA and the SAS. A copy of this CCF component is also used by SGS tools.
There are twelve extension - one for each filter - named FILTER-FilterId. Two extensions are required for each grism to describe the displacement of the zero orders with respect to the direct image obtained with the lenticular filters.

Two additional extensions contain the polynomial coefficients describing the distortion for all the filters.

FILTER-U

FILTER-B

FILTER-V

FILTER-UVW1

FILTER-UVM2

FILTER-UVW2

FILTER-WHITE

FILTER-MAGNI

FILTER-GRISM1

FILTER-GRISM2

FILTER-GRISM10

FILTER-GRISM20

POLYNOM_MAP

POLYNOM_MAP2

Each extension FILTER-FilterId holds a binary table sampling the detector distortion of a specific filter at a coarse resolution ($\sim$ 1 datapoint every 25 subpixel). Intermediate detector position have to be obtained by interpolation. The distortion at the position RAWX, RAWY is described as the difference between the measured image position on the detector and the position assuming a linear grid. The platescale of the linear grid is the value of the keyword PLTSCALE (units: arcsec/pixel). The format of the binary tables follows the description of the CCF ICD [5].

The distortion can alternatively be obtained using two polynomials describing the offset in x- and y-direction. Analysis of calibration data showed that the detector distortion can be parameterized with an up to 7th order polynomial. The 36 parameters $a_0$, ..., $a_{35}$ (cf. section 3.5.5) needed to calculate the distortion in x- and y-direction at any detector position (equivalent to RAWX_OFF and RAWY_OFF) are stored in the columns XPOLYCOEF, YPOLYCOEF of the extension POLYNOM_MAP. There is one set of coefficients per filter element in the POLYNOM_MAP extension. The filter element is found in the column FILTER_ID. The required binary table entry is identified by matching the value of the column FILTER_ID with the State Variable FilterID. The reverse transformation from distorted to flat image is available from the polynomial stored in the extension POLYNOM_MAP2. This has an identical format to the POLYNOM_MAP block.

The format of the AstroMet file is as follows

Binary table: FILTER-FilterID
Twelve binary extensions, one per FilterID

Binary table: POLYNOM_MAP

column name	column type	column unit	comment
FILTER_ID	9A	not applicable	filter ID
PLTSCALE	E	arcsec/subpixel	platescale of filter specified in FILTER_ID
XPOLYCOEF	36E	not applicable	coefficients of x-distortion polynomial
			in ascending order
YPOLYCOEF	36E	not applicable	coefficients of y-distortion polynomial
			in ascending order

Binary table: POLYNOM_MAP2

column name	column type	column unit	comment
FILTER_ID	9A	not applicable	filter ID
PLTSCALE	E	arcsec/subpixel	platescale of filter specified in FILTER_ID
XPOLYCOEF	36E	not applicable	coefficients of x-distortion polynomial
			in ascending order
YPOLYCOEF	36E	not applicable	coefficients of y-distortion polynomial
			in ascending order