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DrizzlePac 2012 Handbook
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The DrizzlePac Handbook > Chapter 7: Examples: Using DrizzlePac for Combining Images > 7.5 WFC3/UVIS: Aligning Images by Defining an Output Reference Frame

7.5
Introduction
The following example describes the alignment of images in two filters obtained with the WFC3/UVIS channel. While tweakreg aligns the image World Coordinate System (WCS) header information, this example demonstrates how to define the output frame reference image for aligning the two filters in pixel space. This example can be generalized for aligning images obtained in different cameras, for example WFC3/UVIS to ACS/WFC.
Step-by-step instructions are provided below, in a cookbook fashion, with minimal discussion of parameters. Commands are given using Python syntax executed in PyRAF. Since the tasks have been restored to default values prior to execution, mostly non-default parameters are specified in the command-line examples.
Summary of Steps
1.
2.
Use tweakreg to align images in a given filter.
3.
For each filter, combine the images using astrodrizzle to produce high signal-to-noise drizzled products, free from cosmic rays and detector artifacts.
4.
Improve the alignment between the two drizzled images, each representing a filter, using tweakreg.
5.
Using tweakback, propagate the new “tweaked” solutions obtained from aligning the two drizzled images back to their respective original flt.fits images.
6.
Drizzle-combine the updated flt.fits images for each filter, using the improved WCS offsets, to create WCS-aligned drizzled images for each filter.
7.
Demonstrate how defining a reference frame in astrodrizzle can create drizzled images for each filter that are aligned, in pixel space, to a common “output grid.”
7.5.1
In August 2009, the first epoch of M83 observations were obtained as part of the WFC3 Early Release Science program (Proposal ID 11360). Three images with small dithers (POS TARGs) were obtained, in each filter, to fill the gap between the two UVIS chips and to allow for rejection of cosmic rays and detector artifacts. This example will focus on aligning two sets of images, one in the F814W filter and the other in F438W, each obtained in different visits.
The datasets used in this example are listed in Table 7.7. Note that the images have been given different names for clarity. While the flt.fits suffix has been dropped in the new name, users should keep in mind that these are calibrated flt.fits products from the pipeline.
Unique & Orig. Image Name
Line Number
Science and data quality extensions for one of the calibrated pipeline products, the first F814W image, are shown in Figure 7.29. Note that the pipeline was overly aggressive at flagging cosmic rays, as reflected in the large number of white pixels in the data quality (DQ) array; this is likely due to a poor estimate of the sky background. These cosmic ray flags, with the value of 4096 in the flt.fits DQ array, will be, by default, automatically reset to be treated as “good” pixels by astrodrizzle (using resetbits=4096). Reprocessing the dataset with different parameter values will then allow the user to manually optimize cosmic ray rejection.
Figure 7.29: Science and Data Quality Extensions for the First F814W Calibrated (flt.fits) Image
The science extensions, [sci,2] and [sci,1], on the left, with their corresponding data quality extensions [dq,2] and [dq,1], on the right. Note that the pipeline did a poor job in flagging cosmic rays, resulting in a pattern which reflects the noise in the sky background. Manual reprocessing with astrodrizzle will allow these flags to be reset and optimized by the user.
7.5.2
Before running tweakreg, the drizzlepac package has to be loaded and the required tasks for this example have to be imported and reset to default values.
This target has few actual point sources, so the alignment is primarily based on the positions of H II regions. The commands below reflect parameters that have been optimized after several interactive trials.
The parameter value for conv_width is recommended to be approximately twice the FWHM of the PSF. By default, imagefindpars will automatically compute the sigma value (standard deviation) of the sky background, so it is necessary to adjust the threshold parameter in imagefindpars to ensure an adequate number of sources are found to compute the fit. (For images containing a large number of saturated objects, the imagefindpars parameter peakmax can be set to exclude those sources from the fit.)
Using the tweakreg parameters shown below (that also includes parameters from the imagefindpar task that is used by tweakreg for object detection settings), several thousand sources are initially detected with several hundred matches, providing solutions accurate to much better than 0.1 pixels r.ms. Users are strongly encouraged to inspect the four-panel residual plot for signs of remaining systematics in the final residuals, like, for example, a slope which indicates that a residual rotation or scale still remains in the data. Instructions for examining the source catalogs are given in Section 7.5.3.
In these tweakreg line-commands in PyRaF (that can also be run in the Python interface), the following settings were used:
conv_width=3.5, the convolution kernel which is twice the PSF FWHM of sources. It identifies potential sources which look closest to a gaussian with the FWHM equal to this parameter’s value.
threshold=200 sigma above the local background for object detection.
updatehdr=False so that the offsets are not used to modify the WCS information in each image.
shiftfile=True and outshifts=’shift_438_pos1.txt’ so that a shift file containing the computed offsets are written to a named file. The contents of the two output shift files are shown below. Shift files are only created for record-keeping purposes. Unlike multidrizzle, astrodrizzle does not accept a shift file as input because offsets are directly applied to the WCS in the image headers.
F814W and F435W shift files:
When tweakreg is run with its default setting writecat=True, it creates source catalogs with extension “.coo” for each science image extension.
tweakreg also automatically generates an ASCII table listing the names of the catalogs generated for each image. The name of the table can be specified by the parameter catfile, but if no name is provided, the default name is <reference_file>_xy_catfile.list. For this set of data, the default name of the catfile is f814w_pos1_01_xy_catfile.list, and its contents are shown below:
When the user is satisfied with the results, tweakreg should be run one last time with updatehdr=True, to update the WCS of each flt.fits image with the final solution. At this point, it is no longer necessary to run the task in interactive mode. To update the WCS information in the image headers as a batch, plotting parameters can be turned off (as shown below) and the task will run without prompting the user to verify the solutions.
This final tweakreg run uses the same settings as the previous run, except that the WCS information in the image headers are updated (updatehdr=True). In addition, writecat is set to False and the catfile parameter points to a previously-made listing of catalogs so that tweakreg makes use of existing catalogs to save processing time.
When updatehdr is set to True, the updated WCS solutions can be tracked via a unique name, given by the tweakreg parameter wcsname. (The default value is the string TWEAK). It is useful to choose a meaningful name to keep track of it when querying the flt.fits headers.
The example below shows the query results for an image header with several different WCSs, each identified by a unique name that reflects the history of the dataset.
WCSNAMEO=OPUS: the original WCS name from OPUS pipeline processing
WCSNAMEA=IDC_v5r1512gi: the WCS corresponding to the distortion reference file (IDCTAB) from running the task updatewcs
WCSNAMEB=TWEAK_438 is a user-generated solution from this example
WCSNAME =TWEAK_438 is also the most current WCS
To query the WCSNAME keywords in the image header, the following IRAF command may be used:
7.5.3
While this step is optional, it is highly recommended.
The commands below use PyRAF tasks to display a chip in a flt.fits image, overplots the initial source catalog “image_sci?_xy_catalog.coo1 (in red) on the image, then overplots the matched catalog “image_catalog_fit.match” (in green). The matched catalog shows which sources were used to compute the tweakreg solution, allowing the user to verify that actual sources (not cosmic rays or hot pixels) were used to determine this solution (See Figure 7.30).
Matched catalog files (with suffix “catalog_fit.match”) are created for all images except the first in the list, which serves, by default, as the reference. Columns 11 and 12 give the original position in the flt.fits images, and column 15 (labeled “EXTVER ID” in *catalog_fit.match files) specifies the chip that corresponds to the coordinates.
Figure 7.30: Source Catalogs Over-Plotted on a flt.fits Image
This is a useful way to inspect objects used for computing the offset fit. Matched sources are shown in green.
Create a Drizzle-combined Image for Each Filter
For each filter, images are drizzle-combined to create a high signal-to-noise image, free from cosmic rays or detector artifacts. These two drizzled image will, themselves, be aligned in a later step.
In the astrodrizzle commands shown above,
driz_sep_bits and final_bits set to “64,32” tells astrodrizzle to treat input pixels flagged in the flt.fits data quality extensions with the value 64 (CTE tails) and 32 (warm pixels) as “good” pixels.
driz_cr_corr =yes is a switch to tell the software to create a cosmic ray mask for each input image.
final_wcs= yes because there are two “custom” output image parameter settings in that category:
-
final_scale, the final output scale, is set to 0.0396 arcseconds/pixel
-
final_rot=02 orients the output image such that its y-axis is relative to the north (at the top of the image).
Note:
Information about the primary WCS solution for each input image that was used to create the drizzled image is stored in a new drizzled file extension of type HDRTAB. The WCSNAME in the drizzled image header itself is set to the value DRZWCZ.
Next, the data products are inspected to look for any offsets. In ds9, the images may be matched by the WCS or in physical (or pixel) units, and then blinked. In this case, the positions of stars in each science array appear to be offset by approximately (+1,+6) pixels.
The weight images should also be inspected. In this case, the final weight image parameter was set to EXP, so the WHT images for each filter resemble an exposure time map of the combined dataset. For UVIS data, it is important to verify that an imprint of sources is not apparent in the weight image, which could imply that one or more frames were being excluded from the final product.
Figure 7.31: Science Extension of the F814W Drizzled Product Oriented North-Up
Figure 7.32: Weight Extension of the F814W Drizzled Product
The gap dither pattern can be seen, as well as pixels with DQ flags and cosmic rays which were treated as “bad” in the final drizzle step.
The quality of the cosmic ray masks should be verified by blinking the original flt.fits image with both the cosmic ray-cleaned image (suffix cr_clean.fits) and the cosmic ray mask (suffix cr_mask.fits). When testing various parameter values, the user may find that the cores of stars have been improperly masked, and this indicates that either the driz_cr_scale parameter should be increased or that the alignment computed by tweakreg was not optimal. If not enough cosmic rays were detected, the driz_cr_snr parameter should be lowered to detect fainter objects. The example below is for a single chip, but this should be repeated for both chips.
Figure 7.33: Close-up of the Same Region in Three Types of Input Products
The top image is a “zoomed-in” region of a flt.fits image, a cosmic ray-cleaned version of that image (middle), and the corresponding CR-mask image (bottom). Blinking these products is recommended to ensure that the cores of stars are not flagged as cosmic rays.
7.5.4
tweakreg is run on each drizzle-combined filter image to compute the offsets that were previously seen in the ds9 display:
Note that the threshold parameter was selected to produce a matched catalog with a few thousand (3,900) sources. Before matching, the lists contain 6,900 sources in F438W and 51,100 sources in F814W. When the input image and the reference image have very different signal-to-noise values, it may be useful to create a reference catalog a priori and provide this to tweakreg via the refcat parameter. This will help ensure that the two filters (or detectors) have similar numbers of objects for matching. The example below shows the syntax for providing a prepared reference catalog:
The contents of the resulting shift file are given below. Notice that the fit produces an offset similar to the one predicted from the earlier visual inspection of the drizzled products in ds9.
To update the image headers with the new solution, run tweakreg with updatehdr=True.
IRAF’s hedit command shows that the keyword WCSNAME has now been updated to reflect the new solution:
The WCS of the F814W and F438W drizzled images are now aligned. No further processing is necessary, as long as the user defines photometric source catalogs in R.A. and Dec. coordinates.
If, however, the user requires the physical pixels of the two frames to align (for example, to subtract a broad-band image from a narrowband image in order to remove the continuum), the images must be drizzled one more time with a pre-defined output frame of reference.
7.5.5
After tweakreg has been used to align drizzled products3, the tweakback task can be used to propagate the updated WCS back to the original flt.fits images. AstroDrizzle may then be used to re-drizzle the flt.fits images frames; the drizzle products will be aligned, and can be verified by displaying and blinking them in ds9. Note that tweakreg only aligns the WCS in the image headers. To ensure that the actual pixels are aligned in the final drizzled product, a output frame of reference must be defined, as described in the next section.
 
 Processing f438w_pos1_01.fits[(’SCI’, 1)]
As a sanity check, one can rerun tweakreg on the original list to ensure that the intra-visit alignment is still optimal. This step is not necessary, but it is shown for completeness, along with the output from the shift file.
7.5.6
This section demonstrates how the drizzled images for the two filters can be aligned in pixel space. Some reasons for doing this include creating color images, subtracting one image from another, or combining them to create an object detection “white light” image (i.e., adding images taken with different filters).
 
This maybe done in one of two ways:
Option A:
Set the parameter final_refimage to point to the F814W drizzled product. This will automatically define the size, orientation, scale, and R.A./Dec. of the central pixel. To retain the drizzled product from Section 7.5.5 for comparison, it can be renamed as a “version 1” image prior to reprocessing.
Parameters specifying the final output grid are shown in bold in the examples below.
If final_refimage is not defined, the F438W drizzled product will not be aligned with the F814W image in pixel space because tweakreg operates on the images’ header WCS, not the physical pixels.
AstroDrizzle automatically computes the image reference frame for each set of input images based on the orientation of the reference image (f814w_pos1_drz_sci.fits in the example above) and the distortion solution of each filter. The product dimensions will be the smallest-sized output image which incorporates the full set of input frames.
Option B:
Instead of defining a final_refimage, set up a pre-defined output grid based on keywords in the original F814W drizzled product. The hselect command, shown below, queries the value of the reference position in pixels and in sky coordinates (R.A./Dec.), and the imheader command returns the size of the array. The user may wish to allow for additional “padding” in the final drizzled product to account for offsets in pointing or differences in geometric distortion with respect to the reference image. This may be done by specifying the final_outnx and final_outny parameters in AstroDrizzle. Note that the output products have been given unique rootnames, f814w_pos1r and f438w_pos1r, to reflect the fact that they were drizzled to a pre-defined reference grid.
 
final_bits=’64,32’,final_wcs=yes,final_scale=0.0396,final_rot=0,\
final_bits=’64,32’,final_wcs=yes,final_scale=0.0396,final_rot=0,\
Following the same logic, an ACS/WFC image may be aligned to a WFC3/UVIS image, though one may need to think about how to set the final_scale parameter since the native ACS/WFC plate scale, at 0.05 arcseconds/pixel, is larger than the WFC3/UVIS plate scale of 0.0396 arcseconds/pixel. If the frames have been dithered, it may be possible to set the final_scale to a value smaller than the native plate scale. For more information, refer to the examples on optimizing image sampling in Sections 7.2 and 7.4.
The drizzled products are now aligned to the same reference pixel, as shown in the result below. These products can be compared to those from Section 7.5.5 which used a different reference pixel.
In ds9, the frames may now be aligned by physical pixels rather than by WCS. Comparing the position of a few stars in each image using imexamine will verify the alignment.
An optional step: to verify that there are no remaining residuals in the two aligned filter images, tweakreg can be used to prove the integrity of the results:
The drizzled science products are shown for comparison in Figure 7.34 and the 4-panel fit residual plot is shown in Figure 7.35. The images, as shown in the shift file below, are now aligned to ~0.1 pixel accuracy,
Figure 7.34: A Comparison of the F438W and F814W Products
Figure 7.35: Astrometric Residuals for F438W with Respect to F814W
Relative alignment is accurate to ~0.1 pixels.

1
“?” is a single-character wildcard for the extension number, either 1 or 2 for UVIS. The names in quotes are files suffixes for the catalogs, as illustrated in the command examples. In this example, chip 1 of the first F814W image is displayed, which corresponds to science extension 2.

2
Setting final_rot to the default value, none or INDEF, will orient the output image to the same orientation as the reference image.

3
In this example, tweakreg was used to align two drizzled images, each with a different filter. The same concept can be applied to aligning drizzled images of different detectors and mosaic pointings.


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