Process a list of images using the wcs_doall routine.
Usage: wcs_list_proc list_fullpath.1 arg1 - name of input list of images % wcs_list_proc List.1This routine runs the script wcs_doall on all of the images in the input list.
In the example below I show a simple example of reducing a set of images from a commissioning night (20160302) on the HET. The images were processed at the telescope as they were obtained to install an approximate WCS header using the rough_wcs_acam rooutine.
% ls -1 /home/sco/ACAM/20160302/images/Save/20*fits > List.1 % cat List.1 /home/sco/ACAM/20160302/images/Save/20160302T034710.0_acm_sci.fits /home/sco/ACAM/20160302/images/Save/20160302T035901.7_acm_sci.fits /home/sco/ACAM/20160302/images/Save/20160302T040847.6_acm_sci.fits /home/sco/ACAM/20160302/images/Save/20160302T042939.0_acm_sci.fits /home/sco/ACAM/20160302/images/Save/20160302T065303.7_acm_sci.fits /home/sco/ACAM/20160302/images/Save/20160302T071745.9_acm_sci.fits /home/sco/ACAM/20160302/images/Save/20160302T074323.9_acm_sci.fits /home/sco/ACAM/20160302/images/Save/20160302T081255.2_acm_sci.fits % wcs_list_proc List.1The acam field of view (FoV) is small (3'x3') and the depth of our commissioning images is usually not very deep, hence we'd like to collect calibration data (USNO catalog data) that covers a small area of sky and uses a bright cut-off limit for the collected stars. In cases like this you might want to change the DSS image size and the magnitude limit of the USNO catalog pulled for the standard star set:
Special note: Note: To change radmin and faint R2 limit: Use local files: Default.DSS , Faint_Mag.LimitFinally, it is worth noting that becasue I had installed a temporary WCS in each image header, I could answer "N" to the queries by wcs_doall about flipping and rotating each image. If a WCS is detected, the code will use the ds9 "Frame > Match > WCS" facility to orient the DSS image to each ACAM field. This usually make star identification much easier. Here is a sample of my responses during this part of the run:
Flip the X orientation? (Y/N):n Rotate? (Y/N):n WCS is present = Y Mark named stars in LEFT FRAME.At this stage I would mark a few identified stars in the left-hand (ACAM) image panel.
Another thing that is slightly annoying when I run wcs_doall is that it frquently does not use a good initial greyscale level. For manual star identification I have a code that displays two image in tiled ds9 frames. It is called "ds9_2f". This code, in turn, calls a code called "adjust_view". The adjust_view code will read limits in a local Default.greyscale file and use them.
Default.greyscale
The wcs_list_proc code was really established as a way of handling multiple images.
% head -8 Li*1 /home/sco/ACAM/20160301/images/Save/20160301T023620.4_acm_sci.fits /home/sco/ACAM/20160301/images/Save/20160301T030347.7_acm_sci.fits /home/sco/ACAM/20160301/images/Save/20160301T031055.4_acm_sci.fits /home/sco/ACAM/20160301/images/Save/20160301T031747.2_acm_sci.fits /home/sco/ACAM/20160301/images/Save/20160301T032232.1_acm_sci.fits /home/sco/ACAM/20160301/images/Save/20160301T032733.5_acm_sci.fits /home/sco/ACAM/20160301/images/Save/20160301T033146.9_acm_sci.fits /home/sco/ACAM/20160301/images/Save/20160301T034459.0_acm_sci.fits % ls -1 2016*fits 20160301T023620.4_acm_sci.fits 20160301T030347.7_acm_sci.fits 20160301T031055.4_acm_sci.fits 20160301T031747.2_acm_sci.fits % gethead RMSRA RMSDEC 20*fits 20160301T023620.4_acm_sci.fits 0.2410 0.1170 20160301T030347.7_acm_sci.fits 0.0020 0.0060 20160301T031055.4_acm_sci.fits 0.2770 0.1960 20160301T031747.2_acm_sci.fits 0.4370 0.2350Hence, my first four images in the list have been processed (i.e. they are present in the local direct, and they have WCS headers with values of RMSRA,RMSDEC not equal to 1.0,1.0). The first image I will want to begin processing then is the fifth one in the list (20160301T032232.1_acm_sci.fits). This is what happens! I see lots of info fly by about the first 4 images, but nothing really happens until the script hits my fifth entry:
% wcs_list_proc List.1
....
yadda yadda
....
i= 5 /home/sco/ACAM/20160301/images/Save/20160301T032232.1_acm_sci.fits
Image (base only) = 20160301T032232.1_acm_sci.fits
AZ,rmsRA,rmsDEC:10.541 1.0000 1.0000
Process this image with wcs_daoll? (Y/N): I will process.
Calibration data is already present.
Number of catalog stars = 19
The dss.fits file exists already.
I am ready to run ds9
Enter any key AFTER ds9 window opens.
At this stage I am ready to begin processing my image with
wcs_doall in the usual way.
Suppose you have WCS-calibrates some ACAM images and you want to see if the image properties are consistant. For a further analysis, after some of my image I used the RUN_STATS script to process header info with the code: acam_wcs_stats.
* Be sure you have solutions:
% gethead RMSRA RMSDEC 20*fits
20160301T023620.4_acm_sci.fits 0.2410 0.1170
20160301T030347.7_acm_sci.fits 0.0020 0.0060
20160301T031055.4_acm_sci.fits 0.2770 0.1960
20160301T031747.2_acm_sci.fits 0.4370 0.2350
20160301T032232.1_acm_sci.fits 0.0670 0.1990
20160301T032733.5_acm_sci.fits 0.1970 0.2940
20160301T033146.9_acm_sci.fits 0.2280 0.1820
20160301T034459.0_acm_sci.fits 0.1460 0.3100
20160301T035356.8_acm_sci.fits 0.1980 0.4610
20160301T040708.6_acm_sci.fits 0.4860 0.1840
20160301T041917.6_acm_sci.fits 0.2530 0.0770
20160301T043419.8_acm_sci.fits 0.0020 0.0060
20160301T044319.0_acm_sci.fits 0.2800 0.2570
20160301T045456.8_acm_sci.fits 0.4170 0.3530
* Build an input file
% ls -1 20*fits > RUN_STATS
**** I edit the RUN_STATS file to make is a script
% chmod 777 RUN_STATS
% cat RUN_STATS
#
acam_wcs_stats.sh 20160301T023620.4_acm_sci.fits
acam_wcs_stats.sh 20160301T030347.7_acm_sci.fits
acam_wcs_stats.sh 20160301T031055.4_acm_sci.fits
acam_wcs_stats.sh 20160301T031747.2_acm_sci.fits
acam_wcs_stats.sh 20160301T032232.1_acm_sci.fits
acam_wcs_stats.sh 20160301T032733.5_acm_sci.fits
acam_wcs_stats.sh 20160301T033146.9_acm_sci.fits
acam_wcs_stats.sh 20160301T034459.0_acm_sci.fits
acam_wcs_stats.sh 20160301T035356.8_acm_sci.fits
acam_wcs_stats.sh 20160301T040708.6_acm_sci.fits
acam_wcs_stats.sh 20160301T041917.6_acm_sci.fits
acam_wcs_stats.sh 20160301T043419.8_acm_sci.fits
acam_wcs_stats.sh 20160301T044319.0_acm_sci.fits
acam_wcs_stats.sh 20160301T045456.8_acm_sci.fits
% RUN_STATS
0.268 88.619 0.26947 180.000 20160301T023620.4_acm_sci.fits
0.006 88.142 0.27072 21.452 20160301T030347.7_acm_sci.fits
0.339 87.917 0.27156 21.452 20160301T031055.4_acm_sci.fits
0.496 88.028 0.27109 21.452 20160301T031747.2_acm_sci.fits
0.210 88.073 0.27105 21.452 20160301T032232.1_acm_sci.fits
0.354 88.155 0.27009 21.452 20160301T032733.5_acm_sci.fits
0.292 88.279 0.27213 21.452 20160301T033146.9_acm_sci.fits
0.343 88.186 0.27051 66.856 20160301T034459.0_acm_sci.fits
0.502 88.274 0.27211 94.089 20160301T035356.8_acm_sci.fits
0.520 88.609 0.27252 115.276 20160301T040708.6_acm_sci.fits
0.264 88.392 0.27085 137.787 20160301T041917.6_acm_sci.fits
0.006 89.052 0.26887 162.610 20160301T043419.8_acm_sci.fits
0.380 86.651 0.27047 189.374 20160301T044319.0_acm_sci.fits
0.546 88.101 0.27107 214.103 20160301T045456.8_acm_sci.fits
% cat acam_wcs_stats.explain
col01 = RMS, combined Ra,Dec residual rms in arcsec
col02 = tz, tz = Acam_PosAngle - HETQ (degrees)
col03 = plate scale (arcsec/pixel_)
col04 = HETQ, HET parallactic angle
col05 = image name
RMS tz ps HETQ Image
My next question is "How do I plot these results?", and I
show a little example here.
I built a dedicate plot script to make plots of various WCS parameters for my wcs-calibrated ACAM images. The routine for this is acam_plots.