SMU FCO
Functional Checkout of the Secondary Mirror
Draft - a work in progress
This is a draft plan for the SMU FCO of July 2003 following its complete
overhaul. It assumes passage of an electro-mechanical checkout on 22 July.
Participation of many JCMT staff is anticipated and appreciated.
This document already contains contributions from JW and CW.
The document was written in advance of the completion of the repairs
and has been updated in blue with the reality
that followed.
Preliminaries
- Settings prior to the overhaul are as described in
smu.ifl (in mt_smudir), and
in the
SMU focus document in this tree.
- It may be anticipated that nominal settings (zero-points) and limits
will
all change, but that relative positions may remain unchanged. For
example :
- the default Z focus position for SCUBA will change, but the
relative
offsets between SCUBA and other receivers will remain the same,
- the values assigned to the soft limits will change, but (given
the same
screw pitch) the difference between the upper and lower limits
should
remain the same.
Nonetheless, and to repeat, the FCO plan must anticipate 'all change'.
- It is anticipated that Chopper functionality has not been changed -
i.e.
that the subreflector and Chopping hardware have not been separated -
although a cautious FCO would include one perfunctory check.
Daytime plan
- Determine hard limits on X,Y and Z tables (TCC, NTM), and set soft
limits.
The reality :
| 1 |
2 |
3 |
4 |
5 |
6 |
| axis |
limit switch interval |
LSL |
USL |
4-3 |
2-5 |
| X |
13108 |
400 |
13300 |
12900 |
~200 |
| Y |
13362 |
275 |
13250 |
12975 |
~375 |
| Z |
12841 |
300 |
12900 |
12600 |
~250 |
The soft limits are a couple of hundred encoder units 'closer in'
than the switch limits - as expected. Crude (plastic ruler) measures
of the switch intervals for the X & Y tables yielded 51 and 50mm resp.,
giving X_SCALE = 257 enc.units/mm and Y_SCALE = 267.
Accuracies of +10 units/mm should be expected.
These should be compared with current values from SMU.ifl
of 273.756 and 257.02, resp. These values do not need changing :
they're just not as accurate as the quoted 2 or 3 decimal places suggest,
or were originally determined in a more precise manner.
The soft limits are clearly set to be roughly 300 from each end.
Since the re-positioning accuracy of all parts (eg limit switched w.r.t.
the tables) is no worse than 1mm then changing any of the current
values for the soft limits and the zero-points seems
unjustified.
On 24 July, the SMU.ifl parameters were restored to their pre-failure values.
With these (old) default operational settings sources should be acquired
within the hardware restoration accuracies of a mm or two; this
translates
to about 15-20"
in the focal plane : not enough to move off the SCUBA FOV.
Now - the weather . . . .
Nighttime Plan
- Start optimistically :
- Configure telescope for SCUBA observing.
- Set (dX,dY,dZ) = (0,0,0), (uaz,uel) = (0,0)
- Take a jiggle map of a bright source (Jupiter early evening, G34.3
mid-evening-shift, Mars 2nd shift).
- If source is seen on the array : skip to 5.
- Configure RxH3 as front end and point at HOLO, with offsets = (0,0)
and a Z-focus setting of +31mm. (dZ should show on screen s0 as +31.00)
(Ensure that the source at UKIRT is switched ON).
- slogin to mamo as OPERATOR and run
mamo> rxh3_eng        
(see
Jan's documentation).
The entry to watch is     Lo Sig Pwr, the signal
strength.
It may be possible to 'peak-up' on this signal using appropriate
setoff commands, but if in doubt take a small (1000x1000 point)
holography map : this should only take a few minutes, and will cover
enough space to catch the signal. Jan will reduce offline (thank you)
and provide 'pointing' offsets. The technique is insensitive to the
focus offset.
- However, such pointing offsets are not due to pointing/collimation
changes (for there have been none) so they must be due to a change in
the configuration of the SMU tables. It is not anticipated that the
optical-table-quality tables will be restored to a configuration too
different from that prior to the shutdown so these 'pointing errors'
ought to be small (and steps 3 & 4 ought to be unnecessary !).
The offsets must be due to an error in the orientation of the tables
w.r.t. the optical axis, either in translation or tilt.
The optical precision of the SMU hopefully eliminates the latter.
A translation error in X or Y of 1mm generates a displacement of the
best image by 7mm, or 8"
(calculations by IMC).
Adjust the X & Y zero points accordingly to move the peak holography
signal to the centre of the map. (Repeat the map and repeat . . .)
Actually, the most recent RxH3 map of 30 June 2003 had pointing offsets
of (-1",+7") (in (daz,del) = (Y,X) in SMU coordinates).
- Repeat step 1.
- On a more point-like source perform focus measurements and determine
total offsets (dX,dY,dZ).
- Add these to (X_ZERO, Y_ZERO, Z_ZERO) in smu.ifl and mt_compifl
(FJO).
Repeat step 5 to ensure signs are OK - (dX,dY,dZ) should now be (0,0,0)
Iain Coulson
24 Jul 2003
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