Support and adjustment of the SDSS 2.5-m telescope conical
baffle
Sloan Digital Sky Survey Telescope Technical Note
19980421
Walter
Siegmund and Patrick Waddell
Contents
Introduction
The Sloan Digital Sky Survey (SDSS) 2.5-m telescope is based on a
wide-field fast two-mirror optical design, i.e., a 3° diameter
field of view at f/5. Such a design is difficult to baffle
adequately against stray light sources without excessive central
obstruction of the entrance pupil. The adopted solution adds a
conical baffle in the converging beam between the primary and
secondary mirrors ("2.5-m telescope light baffles" SDSS Telescope
Technical Note 19980215). Together with the usual primary and
secondary baffles, the design rejects stray light efficiently and
blocks only 28.6% of the pupil area on-axis.
A unique challenge is posed by the design of the conical baffle.
It is suspended between the primary and secondary baffles. However,
its suspension system may only minimally obstruct the light entering
the telescope and reflecting from the primary mirror. Its location
must be controlled to an accuracy of ±3 mm.
The conical baffle has three translational and two rotational
degrees of freedom that can be controlled by adjusting the length of
8 wires using turnbuckles. In addition, the natural frequency of the
torsional vibration mode of the baffle about its axis is determined
by the tension in the wires. The number of degrees of freedom and
adjustments imply that a systematic approach to adjustment is
needed.
Conical baffle adjustment
Prior to adjusting the baffle, the following steps should be
taken.
- The inside of the wind baffle is poorly illuminated. Install
temporary high intensity illumination before proceeding.
- Adjust the release force of the conical baffle support wire
anchors. A spring scale attached to the ball plunger end of the
lever should read between 50 and 60 N when the lever releases.
Adjust the release force by turning the two ball plungers
clockwise or counterclockwise equal amounts. The lever has a ratio
of 6:1. The corresponding maximum tension in the wire is 300 to
360 N.
- Insure that the secondary mirror is centered on the rotator
axis and at the nominal imaging mode focus.
- Mount the collimating telescope adaptor (manhole cover) to the
instrument rotator. Install the alignment telescope in the
adaptor. Care must be taken since these components are delicate.
Rotate the alignment telescope so that the crosshairs are
diagonal. Adjust the micrometers so that the crosshairs are
centered on the dimple ground into the secondary mirror.
- Install cross-hairs at the front and back of the conical
baffle. Holes that are approximately 1 mm in diameter have been
drilled along the two diagonals approximately 12 mm from the front
edge and 9 mm from the back edge of the baffle. White or
gold-colored Kevlar thread (approximately 100 x 200 microns)
intended for fly tying is excellent. Route the thread so that only
one joint is needed. Use hot melt adhesive to join the two ends
while keeping 100 N or so of tension in the thread until the
adhesive cools. Wrap one thread around the other to improve the
strength of the joint. Make the joint on the lower side of the
baffle to prevent adhesive from dripping on the baffle.
- Hang a steel tape measure from one of the wind baffle panels
so that it passes just in front of the front edge of the conical
baffle. Attach a ø27 mm metric crossed scales reticle
(Edmund Scientific Co. A39450) to the tape measure so that the
scales are diagonal and centered on the front crosshairs. This
grid is in focus with the front crosshairs but not the rear
crosshairs. Mount a similar reticle behind the rear crosshairs.
Displacement of the crosshairs or the baffle should be avoided. I
found that the rear grid could be used to measure the error at the
front crosshairs by refocussing the alignment telescope.
The adjustment process is divided into four steps.
- Translate the baffle along the telescope optical axis so that
its distance from the vertex of the secondary mirror is
correct.
- Rotate the baffle so that it is parallel to the telescope
optical axis.
- Center the baffle on the telescope optical axis.
- Tension the baffle.
Initially, the tension in the upper wires should be uniform. The
translation and rotation adjustments described below should not
change the tension in the wires. However, tensions should be checked
periodically. Note that when making adjustments, it is easier to turn
the turnbuckles if loosening adjustments followed by the tighting
adjustments.
Because of the weight of the baffle, the tension in the lower
wires will be less that that in the upper wires. During the first
three steps, it is easier to turn the turnbuckles if the tension is
the wires is low. The natural frequency of the fundamental string
vibration mode in the lower wires should be kept below about 60 Hz.
(The frequency can estimated by plucking the wires and listening to
the tone. Alternatively, a light stroboscope can be used to measure
the vibration frequency.)
Each set of four wires along one diagonal of the conical baffle
mounting frame acts largely independently of the other set. The
exception is if the front set along one diagonal is tightened and the
front set of the opposite diagonal is loosened. This causes uneven
tension in the wires and distortion of the baffle. Consequently, it
should be avoided.
The turnbuckle threads have a pitch of 635 microns (5-40 machine
screws). It is convenient to adjust the turnbuckles in quanta of
one-sixth turn since the turnbuckles have hex wrench flats machined
on their surfaces. Since the turnbuckle is threaded on both ends, the
adjustment quanta is 211 microns, more than fine enough for our
purposes. The opening half-angle of the wires is 15°.
An axial translation adjustment consists of loosening the four
rear turnbuckles one quantum and tightening the four front
turnbuckles one quantum. This adjustment translates the baffle 815
microns toward the secondary mirror. Set the spacing between the
secondary vertex and front crosshairs to 994.8 mm (39.17 inches).
A rotation adjustment consists of loosening the rear turnbuckle
one quantum and tightening the front turnbuckle one quantum in one
corner of the frame. In the diagonally opposite corner, these
adjustments are reversed. This adjustment rotates the baffle about
the opposite diagonal of the frame in the direction of the tightened
turnbuckle of each corner pair. The front and rear crosshairs move in
opposite directions 449 microns and 596 microns respectively per
quantum.
A centering adjustment consists of loosening the turnbuckle pair
in one corner of the frame one quantum and tightening the pair in the
opposite corner one quantum. This adjustment translates the baffle
204 microns along the diagonal of the frame.
To adjust tension, first verify that the tension in the upper
wires is uniform by plucking them and listening to the tone. Then,
attach a spring scale to each of the lower anchor levers in turn.
Adjust the tension in each of the lower wires so that a spring scale
attached to the ball plunger end of the lever reads 35 N with the
ball plungers just out of contact with the ball buttons. This step
should not translate or rotate the baffle a significant amount as
long as the initial tension was approximately correct.
Figure 1: One of eight conical
baffle support wire anchors.
Results
Table 1 gives the spacings of the baffles with respect to the
optical surfaces for the imaging mode ("2.5-m
telescope imaging optical design", SDSST Technical Note
19960410). These numbers are from the drawing "baffle layout97".
Table 1: Spacings of baffle features
and optical surfaces.
Feature
|
x (mm)
|
Focal surface
|
0
|
Common corrector front surface
|
784
|
M1 baffle tip
|
2065
|
Conical baffle rear tip
|
2697
|
Conical baffle front tip
|
3423
|
M2 baffle tip
|
3945
|
M2 vertex
|
4406
|
Table 2 gives the error in position of the critical features of
the light baffles on May 23, 1998. They were measured with the
telescope pointed at the horizon. Standing behind the focal surface
facing the secondary with the telescope pointed at the horizon, +x is
right, +y is up and +z is toward the focal surface.
All measurements are within the tolerances that were used to
design the baffle system ("2.5-m
telescope light baffles", SDSST Technical Note 19960616) except
the error in z of the conical baffle location. It was adjusted to the
wrong value. The location in the z direction is less critical than in
x and y and gravity loading at smaller zenith angles will reduce the
error. Consequently, it should have no effect. It will be set to the
correct value the next time the baffle is adjusted. Visual inspection
did not indicate any discrepancies, e.g., direct views of the sky
from the focal surface.
Table 2: One of eight conical baffle
support wire anchors.
Feature
|
x (mm)
|
y (mm)
|
z (mm)
|
tolerance (mm)
|
M1 baffle tip
|
1.9
|
-0.8
|
*
|
2
|
Conical back
|
-0.3
|
0.5
|
*
|
3
|
Conical front
|
-0.8
|
0.8
|
-4.7
|
3
|
M2 baffle tip
|
1.8
|
-0.6
|
-0.6
|
2
|
* Not directly measured but not likely to be out of
tolerance.
Date created: 4/21/98
Last modified: 2/12/99
Copyright © 1998, 1999, Walter A. Siegmund
Walter A. Siegmund
siegmund@astro.washington.edu