20171031
Priorities
- Any P0 science targets
- Pointing test near center of track in 1st half of the night
- Pointing test near start of track in the 1st half of the night
- Any P0-4 science in the 2nd half of the night
- Low priority engineering tests in queue holes.
Twilight Tests
Note: Twilight exposures are critical science calibrations for LRS and VIRUS and if possible should be done every night that science data is taken.
Pointing test near center of track
Purpose: We have installed for the first half of the night a stripped down, revised version of the pointing code. We wish to determine what residuals remain as a function of Az. We want observations near the center of the track (being exactly at the center is NOT required). We want the observations to be "normal" so if you have to redo a trajectory (due to a fault or human error) please move the Az off and then re-acquire the field.
Procedure:
- Select a star a little before the center of track but bright enough to recognize the field run through shuffle for the IHMP position.
- Send the star to TCS and go next
- After the correct for structure has completed the TO should focus based on ACAM image quality; do a GROC if needed.
- Save an ACAM image
- Look at both the fake ACAM and real ACAM and determine the position for the target star on the real ACAM.
- Record stats in a text file including: ACAM image, structure Az, X star position, Y star position, Tracker X, Tracker Y, rho
- Repeat for the following Az in this order: 210, 230, 250, 270, 290, 310, 330, 350, 10, 30, 50, 70, 90, 110, 130, 150, 170, 190, 200, 220, 240, 260, 280, 300, 320, 340, 0, 20, 40, 60, 80, 100, 120, 140, 160, 180.
If pointing is not to bad then try to complete the rest of the night with this mount model otherwise call Randy to get it reverted.
E-mail results to HET-Operations.
Pointing test near start of track
Purpose: We have installed for the first half of the night a stripped down, revised version of the pointing code. We wish to determine what residuals remain as a function of Az. We want observations near the start of the track (being exactly at the start NOT required). We want the observations to be "normal" so if you have to redo a trajectory (due to a fault or human error) please move the Az off and then re-acquire the field.
Procedure:
- Select a star a little after the start of the track but bright enough to recognize the field run through shuffle for the IHMP position.
- Send the star to TCS and go next
- After the correct for structure has completed the TO should focus based on ACAM image quality; do a GROC if needed.
- Save an ACAM image
- Look at both the fake ACAM and real ACAM and determine the position for the target star on the real ACAM.
- Record stats in a text file including: ACAM image, structure Az, X star position, Y star position, Tracker X, Tracker Y, rho
- Repeat for the following Az in this order: 210, 230, 250, 270, 290, 310, 330, 350, 10, 30, 50, 70, 90, 110, 130, 150, 170, 190, 200, 220, 240, 260, 280, 300, 320, 340, 0, 20, 40, 60, 80, 100, 120, 140, 160, 180.
If pointing is not to bad then try to complete the rest of the night with this mount model otherwise call Randy to get it reverted.
E-mail results to HET-Operations.
Low Priority Engineering
HET PSF measurement using the ACAM
Purpose: We would like to get measurements of the PSF far wings by looking at bright stars. We should do this a few times with different stack qualities to see how this changes. Note we should avoid the CCAS tower for this test. Since we are looking for the faint features this should be done when conditions are good and no moon is present.
Procedure:
- Make sure moon is down and seeing is somewhat stable.
- Select a 14th mag star with shuffle (avoiding Az 38 - 98 to keep CCAS out of the field of view) on BIB
- Setup on star on the BIB
- Get both guiders going with metrology going and saving images
- Get a WFS going and closed loop (note since the ACAM is in you might have to look at both WFS to get the one without the ACAM obstruction)
- Save 20 images of at least 5 seconds each.
- Note the RSE, time since stack, temp change since stack, tracker x and y, telescope az.
- Stop saving guider images
Repeat this for a few different conditions of the stack: Freshly stacked, RSE = 100, RSE=200, RSE=300
Repeat this for a few different tracker positions: early in track, center of track late in track etc..
Testing of the ACAM position
Purpose: We want to see if the ACAM position changes with respect to the IHMP over time. We want this data about 2 times per week and when ever we get an unusually high or low temperature.
Determine the Center of the BIB:
- Select a 14th mag star in a reasonably rich field with shuffle for the BIB
- Setup on the very center of the BIB field of view based on the wiki value and save an image.
- Guide on one of the guide probes
- Put in the ACAM and save an shallow image with the target star not saturated.
- Report on the position of the BIB in the night report and on NightOperations/Commissioning/Results
- Save a deeper image which should show more than a dozen stars.
Determine the Center of LRS2-B
- Select a 14th mag star in a reasonably rich field with shuffle for the LRS2-B
- Setup on LRS2-B and start guiding on one of the guiders
- Take LRS2-B spectrum, probably 60 seconds.
- Adjust the position so that the star is at the center of LRS2-B IFU using lmap until the offsets are less than 0.3"
syscmd -T 'Guider1_offset_fiducial ( dx_asec=-0.01,dy_asec=0.55,compensate="false")'
- Confirm the star is at the center of the IFU by taking a spectrum.
- Once it is as the center of the IFU put in the ACAM and take a shallow image so that the star is not saturated.
- Report on the position of the LRS2-B in the night report and on NightOperations/Commissioning/Results
- Take a deeper image so that there are large number of stars.
Determine the Center of LRS2-R
- Select a 14th mag=== Testing of the ACAM position === star in a reasonably rich field with shuffle for the LRS2-R
- Setup on LRS2-R and start guiding on one of the guiders
- Take LRS2-R spectrum, probably 60 seconds.
- Adjust the position so that the star is at the center of LRS2-R IFU using lmap until the offsets are less than 0.3"
- Confirm the star is at the center of the IFU by taking a spectrum.
- Once it is as the center of the IFU put in the ACAM and take a shallow image so that the star is not saturated.
- Report on the position of the LRS2-R in the night report and on NightOperations/Commissioning/Results
- Take a deeper image so that there are large number of stars.
Closed dome work
Please do the following if you are closed (in order of priority):
- VIRUS 200 ldls flats
- LRS2 dark 1800s x3
- FeAr 1800s red x4
- FeAr 1800s blue x4
See the long cals page for more information:
