A set of acm,gc1,gc2 images were obtained at 4 sky positions on 20190714. Useful notes from SJ:
Notes from SJ: Hi Steve, We took another dataset for you tonight (20190719) with the fiducial offsets on the ACQ. We set up on an f11 star (#20536 W), guided on the ACQ (with PID loop active), activated WFS2 for a few minutes, and were ready to start the offsets at 09:09 (and de-activated WFS2 at that point). 09:09 - 09:10 stored images at this position. 09:10:05, issued: syscmd -T 'ACQ_offset_fiducial ( dx_asec=5,dy_asec=0,compensate="false")' 09:13:00, issued: syscmd -T 'ACQ_offset_fiducial ( dx_asec=-10,dy_asec=0,compensate="false")' 09:16:15, issued: (return to original position) syscmd -T 'ACQ_offset_fiducial ( dx_asec=5,dy_asec=0,compensate="false")' 09:18:50, issued: syscmd -T 'ACQ_offset_fiducial ( dx_asec=0,dy_asec=5,compensate="false")' 09:21:00, issued: syscmd -T 'ACQ_offset_fiducial ( dx_asec=0,dy_asec=-10,compensate="false")' 09:23:20 canceled this trajectory and moved on to another target. Hope these are useful! Steven
I made some quick checks on mcs and decided to record the steps here.
[sco@mcs ~/ACM_reds_2]$ pwd
/home/mcs/sco/ACM_reds_2
[sco@mcs ~/ACM_reds_2]$ ls -1 /hetdata/data > dates.6 # edit dates.6 to run from 20190701 to 20190719
[sco@mcs ~/ACM_reds_2]$ acm_nights dates.6 none N
Date Nimages Nbias Ndark Nopen Nnone Moon_illum
20190718/ 277 5 0 262 10 98.800
20190719/ 765 0 0 765 0 95.900 very clear at end of night
*** Note: I ran this at the end of the night on 20190719, hence the bias images
for that date will be obtained later today. I pulling over the 20190718 acm
images to insure the bias images are available.
To gather data on mcs:
/home/mcs/sco/AAA
[sco@mcs ~/AAA]$ cat GRAB
#
mkdir 20190718/
cp -r /hetdata/data/20190718/acm 20190718/
#
mkdir 20190719/
cp -r /hetdata/data/20190719/acm 20190719/
cp -r /hetdata/data/20190719/gc1 20190719/
cp -r /hetdata/data/20190719/gc2 20190719/
*** Then I pull AAA to buckaroo , then sco2019
[sco@mcs ~]$ fpush AAA buckaroo
To get data from buckaroo to sco2019:
% pwd
/media/sco/DataDisk1/sco/AD/HET_work/acm_nights
% scp -r sco@buckaroo.as.utexas.edu:/home/buckaroo/sco/AAA .
*** This 5.6GB took from 7:38am to about 8:10am (about 30min)
As a start, image lists are made and then viewed wit bigds9.
From SJ's notes, the acm,gc1,gc2 images of interest are in the time range: 09:09 UT to 09:23:20 UT % pwd /home/sco/GC_Plate_Scales/2090819 % cat BaseDir /media/sco/DataDisk1/sco/AD/HET_work/acm_nights % cat Date 20190719 % pas_imlistgen l acm N # 765 acm images in the file list.IMAGES % mv list.IMAGES list.all_acm Next I want to isolate the acm image that were taken in the gc offstest. This test was performed: 09:09:00.0 to 09:23:20.0 To make a table file of just these images: % select_pas_images_by_time list.all_acm acm_ALL 09:09:00.0 09:23:20.0 acm N * Now I have a table (acm) of the images ued in the gc offset observations. I edit list.acm_all to list.acm (103 images) to have only images between 09:09 and 09:23 UT % bigds9 list.acm 1 110
At this point I want to divide the image sets by position on the sky. I have approxiamte time intervals from SJ, I start with these times and the acm table file. First I pull each acm group, and then make the final list of cleaned images with bigds9.
I will use the 10" jumps to delineate the positions. 09:09:00.0 09:10:05.0 A 09:13:00.0 09:16:15.0 B 09:21:00.0 09:23:20.0 C % pwd /home/sco/GC_Plate_Scales/2090819 Group A: % select_pas_images_by_time acm.images EX0 09:09:00.0 09:10:05.0 acmA N # 8 images % mkdir acmA % mkdir acmA % cd acmA % cp ../acmA.* . % ls acmA.images acmA.params acmA.parlab acmA.table % bigds9 acmA.images 1 20 *** mark a few bad images % mv ds9_list_load.nomark list.acmA Group B: % select_pas_images_by_time acm.images EX0 09:13:00.0 09:16:15.0 acmB N # 24 images % cd acmB % bigds9 acmB.images 1 30 *** mark first image as bad, then % mv ds9_list_load.nomark list.acmB *** Marked the bad focus images, then % mv mv ds9_list_load.nomark list.acmB GroupC: % select_pas_images_by_time acm.images EX0 09:21:00.0 09:23:20.0 acmC N # 17 images % cd acmC % bigds9 acmC.images 1 30 *** I marked the bad images, then % mv ds9_list_load.nomark list.acmC Now I can get time intervals for each cleaned acm set: A 09:09:09.2 09:09:57.5 B 09:13:25.4 09:16:13.4 C 09:21:25.4 09:23:09.4 Measure the acm images centroids: % pwd /home/sco/GC_Plate_Scales/2090819/acmA % ds9_imstats_fitslist list.acmA FixedRegions N # save finding chart of stars % cd ../acmB % ds9_imstats_fitslist list.acmB FixedRegions N % cd ../acmC % ds9_imstats_fitslist list.acmC FixedRegions N
I use two methods to get the offsets.
% cd /home/sco/GC_Plate_Scales/20190719
% table_XY_offsets.sh ./acmA/XYmean ./acmB/XYmean xmean ymean xme yme N
% pas_XY_offsets.sh ./acmA/list.acmA ./acmB/list.acmB 1.0 N
% table_XY_offsets.sh ./acmA/XYmean ./acmC/XYmean xmean ymean xme yme N
% pas_XY_offsets.sh ./acmA/list.acmA ./acmC/list.acmC 1.0 N
% table_XY_offsets.sh ./acmB/XYmean ./acmC/XYmean xmean ymean xme yme N
% pas_XY_offsets.sh ./acmB/list.acmB ./acmC/list.acmC 1.0 N
mido measures PAS measures
--------------------------------------------- ------------------------------------------
The procedure here is much the same except I now know the time intervals for the A,B,C positions. I will have to edit the images in each set to account for focus and seeing chnages.
Now I can get time intervals for each cleaned acm set:
A 09:09:09.2 09:09:57.5
B 09:13:25.4 09:16:13.4
C 09:21:25.4 09:23:09.4
GC1:
% pas_imlistgen l gc1 N # 6036 gc1 images in the file list.IMAGES
% mv list.IMAGES list.all_gc1
% select_pas_images_by_time list.all_gc1 EX0 09:09:09.2 09:09:57.5 gc1A N # 8 images
% select_pas_images_by_time list.all_gc1 EX0 09:13:25.4 09:16:13.4 gc1B N # 27 images
% select_pas_images_by_time list.all_gc1 EX0 09:21:25.4 09:23:09.4 gc1C N # 17 images
*** I edit each set with bigds9 in the respective directories
% bigds9 gc1A.images 1 30
% bigds9 gc1B.images 1 30
% bigds9 gc1C.images 1 30
Measure each group in its subdir
% ds9_imstats_fitslist list.gc1A FixedRegions N
% ds9_imstats_fitslist list.gc1B FixedRegions N
% ds9_imstats_fitslist list.gc1C FixedRegions N
Measure offsets
% cd /home/sco/GC_Plate_Scales/20190719
% table_XY_offsets.sh ./gc1A/XYmean ./gc1B/XYmean xmean ymean xme yme N
% pas_XY_offsets.sh ./gc1A/list.gc1A ./gc1B/list.gc1B 1.0 N
% table_XY_offsets.sh ./gc1A/XYmean ./gc1C/XYmean xmean ymean xme yme N
% pas_XY_offsets.sh ./gc1A/list.gc1A ./gc1C/list.gc1C 1.0 N
% table_XY_offsets.sh ./gc1B/XYmean ./gc1C/XYmean xmean ymean xme yme N
% pas_XY_offsets.sh ./gc1B/list.gc1B ./gc1C/list.gc1C 1.0 N
NOTE: I the cases of AB and AC the wrong star was measured by PAS
mido measures PAS measures
--------------------------------------------- ------------------------------------------
27.132 27.132 0.809 1 -999 -999 -999 0 ABgc1
28.187 28.187 0.741 1 -999 -999 -999 0 ACgc1
39.647 39.647 0.895 1 39.107 39.036 1.094 12 BCgc1
*** -999 indicates the images had no metrology in headers.
The procedure here is much the same except I now know the time intervals for the A,B,C positions. I will have to edit the images in each set to account for focus and seeing chnages.
Now I can get time intervals for each cleaned acm set:
A 09:09:09.2 09:09:57.5
B 09:13:25.4 09:16:13.4
C 09:21:25.4 09:23:09.4
GC2:
% pas_imlistgen l gc2 N # 6031 gc2 images in the file list.IMAGES
% mv list.IMAGES list.all_gc2
% select_pas_images_by_time list.all_gc2 EX0 09:09:09.2 09:09:57.5 gc2A N # 8 images
% select_pas_images_by_time list.all_gc2 EX0 09:13:25.4 09:16:13.4 gc2B N # 27 images
% select_pas_images_by_time list.all_gc2 EX0 09:21:25.4 09:23:09.4 gc2C N # 17 images
*** I edit each set with bigds9 in the respective directories
% bigds9 gc2A.images 1 30
% bigds9 gc2B.images 1 30
% bigds9 gc2C.images 1 30
Measure each group in its subdir
% ds9_imstats_fitslist list.gc2A FixedRegions N
% ds9_imstats_fitslist list.gc2B FixedRegions N
% ds9_imstats_fitslist list.gc2C FixedRegions N
Measure offsets
% cd /home/sco/GC_Plate_Scales/20190719
% table_XY_offsets.sh ./gc2A/XYmean ./gc2B/XYmean xmean ymean xme yme N
% pas_XY_offsets.sh ./gc2A/list.gc2A ./gc2B/list.gc2B 1.0 N
% table_XY_offsets.sh ./gc2A/XYmean ./gc2C/XYmean xmean ymean xme yme N
% pas_XY_offsets.sh ./gc2A/list.gc2A ./gc2C/list.gc2C 1.0 N
% table_XY_offsets.sh ./gc2B/XYmean ./gc2C/XYmean xmean ymean xme yme N
% pas_XY_offsets.sh ./gc2B/list.gc2B ./gc2C/list.gc2C 1.0 N
NOTE: I the cases of AB and AC the wrong star was measured by PAS
mido measures PAS measures
--------------------------------------------- ------------------------------------------
27.470 27.470 0.554 1 26.643 27.101 0.698 17 ABgc2
29.751 29.751 0.697 1 27.676 27.851 0.827 12 ACgc2
41.410 41.410 0.671 1 39.752 39.833 0.702 21 BCgc2
WHAT TO DO???????????
Build a file names 20190719.dat:
AB
20.281 20.309 0.151 4 19.857 19.686 0.588 10 ABacm
27.132 27.132 0.809 1 -999 -999 -999 0 ABgc1
27.470 27.470 0.554 1 26.643 27.101 0.698 17 ABgc2
AC
21.457 21.222 0.423 4 20.954 21.075 0.849 7 ACacm
28.187 28.187 0.741 1 -999 -999 -999 0 ACgc1
29.751 29.751 0.697 1 27.676 27.851 0.827 12 ACgc2
BC
29.261 29.052 0.458 4 28.210 27.957 0.957 13 BCacm
39.647 39.647 0.895 1 39.107 39.036 1.094 12 BCgc1
41.410 41.410 0.671 1 39.752 39.833 0.702 21 BCgc2
Next we compute the plate scale
% gcps.sh 20190719.dat N
Th plate scale data are in table files: gc1_plate_scales gc2_plate_scales
To make a plot of the estimates (for example):
Generic_Points
% xyplotter_auto gc1_plate_scales q q 1 N
(edit Axws.1 List.1)
% xyplotter List.1 Axes.1 N