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mkfringeflat stis


NAME · USAGE · PARAMETERS · DESCRIPTION · EXAMPLES · TIME_REQUIREMENTS
REFERENCES · BUGS · SEE_ALSO

NAME

mkfringeflat -- Match fringes in STIS fringe flat to those in science data

USAGE

mkfringeflat inspec inflat outflat

PARAMETERS

inspec
Input science 2-D spectral image (typically created by prepspec )
inflat
Input fringe flat field image (typically created by normspflat )
outflat
Output fringe flat field image
(do_shifts = yes)
Shift flat field to match fringes in science spectrum?
(beg_shift = -0.5)
Starting shift for shift determination
(end_shift = 0.5)
End shift for shift determination
(shift_step = 0.1)
Step through range of shifts for shift determination
(do_scales = yes)
Scale fringe amplitude in flat field to match fringes in science spectrum?
(beg_scale = 0.8)
Starting scale for scale determination
(end_scale = 1.2)
End scale for scale determination
(scale_step = 0.04)
Step through range of scales for scale determination
(extrloc = INDEF)
Central line (row) to be extracted from 2-D spectrum? (INDEF only applicable to point source spectra)
(extrsize = INDEF)
Number of lines (rows) to be extracted from 2-D spectrum? (INDEF only applicable to point source spectra)
(opti_spreg = "INDEF")
Spectral range (first:last, e.g., 82:1106) for normalizing science spectrum?
(rmsregion = "725:900")
Spectral range (first:last) in which to measure RMS'es?

DESCRIPTION

This task provides the second (and last) step towards the creation of a "fringe flat" image that can be used to eliminate the fringes that are present in STIS first-order CCD spectra at wavelengths longer than about 700 nm. This task is suitable for flat field images that have been normalized by means of task normspflat (which supports both contemporaneous flat field images and library flat field images).

The actual fringe correction is performed by issueing task defringe for which output image outflat of MKFRINGEFLAT is an input parameter.

The main goal of this task is to determine the best match between the fringes in the input flat field image inflat and those in the science spectrum inspec . NOTE: It is advised to prepare the science spectrum by means of task prepspec .

The match is made in two separate steps, which can be issued independently by means of boolean switches do_shifts and do_scales : (1) if do_shifts = yes, determine the offset along the dispersion direction between the flat field image and the science spectrum. This is done empirically as follows: After shifting the flat field image along the dispersion direction by discrete steps (the range and increment of which are specified by input parameters beg_shift , end_shift and shift_step , respectively), the science spectrum is divided by each individual shifted flat field. The "flatfielded" science spectra is subsequently normalized by a spline fit to their "continuum" (for which a suitable spectral range can be provided in input parameter opti_spreg , see below for more information), and the variance of the "flatfielded" science spectra is measured in the spectral range specified by input parameter rmsregion , which should be a spectral range devoid of (strong) spectral lines. IT IS IMPORTANT TO CHOOSE THIS PARAMETER CAREFULLY . After collecting the variances of the flatfielded spectra, a inverse-variance-weighted shift is calculated and applied to the input flat field image. (2) if do_scales = yes, determine the best match between the fringe amplitude in the flat field image with the fringe amplitude in the science spectrum. This is equivalent to a correction for scattered light (see STIS Instrument Science Report 98-16 for an extensive discussion). This match is done empirically as follows: After scaling the amplitude of the fringes in the flat field image by discrete factors (the range and increment of which are specified by input parameters beg_scale , end_scale and scale_step , respectively), the science spectrum is divided by each scaled flat field. The "flatfielded" science spectra are subsequently normalized by a spline fit to their "continuum" after which the variance of the "flatfielded" science spectra is measured (similar to case (1) above, using the same input parameters opti_spreg ) and rmsregion ). After collecting the variances of the flatfielded spectra, a inverse-variance-weighted shift is calculated and applied to the input flat field image.

The parameter opti_spreg is the spectral region used by the task to perform a spline fit to the continuum of the spectrum of the science target in_spec . Although the spline fit will ignore pixels that have a value more than 5 sigma different from the local average, it is advised NOT to include strong (and broad) spectral lines in opti_spreg . The default "INDEF" setting will select the full spectral region covered by the input spectrum.

SPECTRAL 1-D EXTRACTIONS

The task allows for user-specified as well as `default' 1-D extractions, through the parameters extrloc and extrsize . When parameter extrloc is INDEF, the task will search for the center of the brightest object in the central 20% of the CCD along the slit and assign the fitted peak pixel as the center of the extraction (which is mostly appropriate for single point sources in the center of the slit). When extrsize is INDEF, the task will extract the `default' number of pixels perpendicular to the dispersion direction. This default extraction size is 11 pixels for a long-slit spectrum. In case a short-slit fringe flat is used (i.e., using the 0.3X0.09 or 0.2X0.06 slits), the extraction size is chosen to stay within the spatial extents of those slits, i.e., 9 and 7 pixels respectively. Note that in cases of extended objects or off-center point sources, the INDEF settings for extrloc and extrsize are very likely to be inadequate; in those cases, it is advised to provide appropriate values for extrloc and extrsize .

INPUT AND OUTPUT IMAGES

The input STIS science spectral image is assumed to be a FITS "imset" file, with three extensions in an imset: science (EXTNAME=SCI), error (ERR), and data quality (DQ). As far as the input flat field image is concerned, MKFRINGEFLAT can handle FITS imset files with three extensions as well as "old-fashioned" FITS files (with only one extension). The output FITS file only has one extension.

EXAMPLES

1. Match the fringes in a STIS flat field image to those in a STIS point source spectrum by shifting the flat field along the dispersion and by scaling the fringe amplitude.


    cl> mkfringeflat science.fits flat.fits flat_matched.fits

2. Same as 1, for a specified off-center extraction and a non-default range of shifting factors.


    cl> mkfringeflat science.fits flat.fits flat_matched.fits \
    >>> beg_shift=0.4 end_shift=1.4 scale_step=0.2 extrloc=610 extrsize=5

3. Same as 1, but only by scaling the fringe amplitude, with a non-default range of scaling factors.


    cl> mkfringeflat science.fits flat.fits flat_matched.fits \
    >>> do_shifts- beg_scale=1.00 end_scale=1.20 scale_step=0.04

4. Same as 1, but perform the normalization of the science spectrum for a non-default spectral range


    cl> mkfringeflat science.fits flat.fits flat_matched.fits \
    >>> opti_spreg="500:1000"

5. Same as 1, but determine the variance of the normalized spectra within a non-default spectral range


    cl> mkfringeflat science.fits flat.fits flat_matched.fits \
    >>> rmsregion="500:1000"

6. Example of all steps involved in fringe correction for a G750M spectrum o3st20gdr_raw.fits and its associated contemporaneous fringe flat o3st20gds_raw.fits:


    cl> normspflat o3st20gds_raw.fits normff750M.fits \
    >>> darkfile="mysuperdark.fits" wavecal="o3st20gdr_wav.fits"
    cl> prepspec o3st20gdr_raw.fits darkfile="mysuperdark.fits"
    cl> mkfringeflat o3st20gdr_sx2.fits normff750M.fits normff750M_fin.fits
    cl> defringe o3st20gdr_sx2.fits normff750M_fin.fits \
    >>> outspec="o3st20gdr_final.fits" do_cal-

7. Same as 6, but for a G750L spectrum o3st20gda_raw.fits, wavecal o3st20gda_wav.fits and contemporaneous fringe flat o3st20gdb_raw.fits:


    cl> normspflat o3st20gdb_raw.fits normff750L.fits \
    >>> darkfile="mysuperdark.fits" wavecal="o3st20gda_wav.fits"
    cl> prepspec o3st20gda_raw.fits darkfile="mysuperdark.fits"
    cl> mkfringeflat o3st20gda_crj.fits normff750L.fits normff750L_fin.fits
    cl> defringe o3st20gda_crj.fits normff750L_fin.fits \
    >>> outspec="o3st20gda_defr.fits" do_cal-

TIME REQUIREMENTS

REFERENCES

Task created by Paul Goudfrooij on April 3, 1998.
Task modified by Paul Barrett on October 21, 2004.

BUGS

SEE ALSO

normspflat, prepspec, defringe


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