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7.2. Spider diffractionMore often than not, central obstruction by a smaller secondary mirror is accompanied with aperture obstruction caused by its support structure  so called spider vanes. Their effect is generally small, but it can be significant. That makes them worth of a closer look. Unless the secondary mirror cell is supported by an optical window, the supporting vanes  so called spider vanes  are in the optical path, altering emitting area of the wavefront and, thus, creating diffraction effect. As long as the pupil area obstructed by the vanes remains relatively small, spider diffraction is more of a cosmetic damage than seriously affecting contrast level (FIG. 108). Analogously to the central obstruction effect, what FIGURE 108: Visual appearance of a bright star without spider effect (a), with threevane spider effect (b), and fourvane spider effect  the two most common spider forms  (c). The effect is noticeable mainly on objects of high telescopic brightness. While the spikes caused by spider vanes can be visually distracting, the amount of energy lost from the disc is usually negligible for general observing (3vane spider spikes are usually shorter, due to the vanes being generally thicker, as it is needed for mechanical stability in that spider configuration, but they may be less intense, since their patterns don't overlap). can be thought of as a Strehl ratio degradation factor caused by spider diffraction is, in effect, the ratio of the clear (annular) pupil area with and without the vanes, squared, or
with N being the vane count, τ the relative vane thickness and ο the relative size of central obstruction, both in units of the aperture diameter. The negative factor equals the relative spider area in units of the clear aperture (i.e. annulus) area; this is consistent with degradation factor caused by central obstruction (Eq. 60). Average spider area is somewhere between 1% and 2% of the clear aperture area. That puts an average spider vane contrast degradation factor between 0.98 and 0.96  below the level of 1/30 wave RMS wavefront error. Analogously to the effect of central obstruction, vane obstruction reduces central intensity of the main pattern by a (1a)2 factor, a being the relative vane area in units of the clear aperture area (for spider vanes, it is the area of annulus), by lowering constructive interference within central maxima and intensifying it in the outer potion of the pattern. For small values of a, typical for spider vanes, the Strehl degradation factor can be written as S'~(12a). It also closely approximates the combined Strehl degradation factor of the spider and c. obstruction in the left side of MTF graph (extended lowcontrast detail resolution) if a is their combined relative area in the aperture (this approximation is also good for the PSF maxima degradation factor for central obstructions smaller than ~0.35D). This is not quite in agreement with the popular notion that the contrast effect of spider vanes is directly proportional to their area, relative to the area of aperture. The misconception probably comes from misunderstood sequence in Suiter's "Star Testing Astronomical Telescopes", where he states that the initial quick contrast drop is in proportion to the vanes area. However, looking at the MTF graph, it is easy to see that this initial drop in contrast remains nearly unchanged linearly for nearly 2/3 of the MTF range. In other words, the actual contrast loss keeps increasing as the relative contrast value decreases for smaller spatial frequencies (detail size). The average contrast loss caused by vanes is, therefore, considerably higher, as given by Eq. 65. However, it should be emphasized that this theoretical approach is strictly valid only in the context of near monochromatic point source  i.e. coherent light. In the real world, light processed by the telescopes is typically polychromatic, i.e. partly incoherent, in which case the effect of light obstructions on intensity distribution within diffraction image is significantly smaller. As in the section about the effect of central obstruction, will continue with the standard coherent light context, but keeping in mind that it is not directly applicable to the field conditions. Depending on the object of observation, the actual spider effect can be much smaller, due to the energy being thrown so far from the Airy disc. For instance, a spider wane D/100 thick will have its principal spike length superimposed over diffraction pattern nearly 100 Airy disc diameters long (only a portion of it visible at best, depending on its telescopic brightness). For a 10" aperture, that is nearly 1 arc minute from the disc center. That would place most of the spike energy out of a relatively small object, not influencing its contrast. For Jupiter, roughly 2/3 of the principal spike fall outside the planet's disc, with 1/3, or so, of the spikes' energy left in, lowering the contrast. Assuming 4vane spider and 25% obstruction, it would cause little over 1% actual average contrast loss (nearly 0.99 Strehl equivalent), not 4% as indicated by Eq. 65. On the other hand, on large objects like the Moon, nearly entire spikes' energy remains within the image, and the effective contrast degradation factor is ~0.96. There are various vane configurations possible, but the only result is a different form of energy distribution  the amount of energy transferred out of the Airy disc remains unchanged for any given vanes area. Given size of central obstruction, the vane area is directly proportional to its width  the wider vanes, the more energy spread out, the higher its peak intensity, but the shorter spike length. Spider diffraction effect is often illustrated by the effect of a narrow slit. There doesn't seem to be a clearly defined width above which diffraction effect becomes that of an aperture. Hecht uses narrow slit relation for a 0.5mm by 30mm slit, which is very similar to the vane configuration, even if it is, evidently very wide with respect to the wavelength. Specifically, intensity distribution within diffraction pattern created by a slit aperture placed in front of an objective with focal length ƒ is described by:
with I(0) being the intensity as a function of point radius, for the central intensity normalized to 1 (actual intensity depends on the slit area), β=Sπsinθ in units of the wavelength λ, S being the edgetoedge separation (i.e. either the slit width, or length) and θ=r/ƒ being the point angle in the image plane, in radians, with r the linear point height (linear radius r=β/πi in units of λƒ/S). The numerator angle is in degrees, denominator angle in radians. The minimas occur for β=aπ, with a=1,2,3,4... First maxima is for β=θ=0, and every subsequent maxima at β=tanβ (with β at left in radians), or for β=bπ, with b=1.43, 2.46. 3.47... This gives the second maxima intensity (for β=1.43π) as 0.047 of the central intensity, the third maxima as 0.016, the fourth 0.008, and so forth. With the slit height much larger than its width, diffracted energy drops to first minima much quicker in the plane perpendicular to the slit height, negligible in comparison to the energy spread in the plane perpendicular to the slit's width (for instance, with the widthtoheight ratio of 1:100, sinθ in β=Sπsinθ has to be 100 times smaller in order for β to have any given value, including the first minima at β=π. What seems to be more appropriate reference shape for the vane in the visual wavelengths is rectangular aperture. Its width is still much smaller than its height, but it is quite large relative to the wavelength. In the case of rectangular aperture, intensity distribution within diffraction pattern is described with a double squared sinc function:
where subscripts W and H stand for aperture's width and height, respectively, along its sides, with βW=Wxπ/ƒ and βH=Hyπ/ƒ, also in units of λ, where x and y are the linear point coordinates in image plane in the horizontal and vertical direction, respectively. Evidently, this relation gives identical distribution of minimas and maximas in the two perpendicular planes as Eq. 66 (one perpendicular to the vane width, the other to vane's height), with either x or y being the equivalent of r under Eq. 66, and either being zero along one of the two perpendicular axes in image plane. Still, this relation is more complete since directly determining intensity distribution along both perpendicular axes, and in any chosen direction in the image plane. With the first intensity minima falling at a constant nominal value of β, its angular radius, given by θ=x/ƒ=βWλ/πW (for small angles sinθ=θ in radians) is inversely proportional to the width W. Thus, the longer the vane, the more narrow its spike; the wider vane, the shorter its spike. A 200x1mm vane  so with W=1 and H=200 (neglecting central obstruction), for λ=0.00055mm will produce first maxima nearly 4 arc minutes long (for βW=π) and about 1.1 arc seconds wide (βH=π); a vane twice as thick will produce maxima half as long, with its width unchanged. Thicker vanes may appear to be producing less intrusive, shorter spikes, but they drain more energy from the Airy disc, causing greater negative effect on the contrast level. The actual spike diffraction intensity, similarly to circular aperture, is proportional to its area, and can be written as I=πΦW/ƒλ2, where Φ, W, ƒ are the flux (blocked by the vane), vane width and focal length. The flux as a product of vane area and flux per unit area, and can be written as Φ=WHu, u being the flux per unit area. The W/ƒ factor reflects the effect of spike size (i.e. length), with the intensity being proportional to the width for given flux, and proportional to the square of it considering that the flux also changes in proportion to the width. Obviously, if we scale a vane to a twice larger aperture, its area  and flux blocked out  increases fourfold, and with it its spike intensity. But the same happens with the aperture's diffraction pattern, whose intensity, I=πΦ/(2λF)2, also changes with the flux, and their brightness relative to each other does not change. If, however, it is the focal length ƒ that doubles, spike intensity relative to the star diffraction pattern also doubles, since the latter is spread onto four times larger, and the former only two times larger area. The form of pattern change is determined by the vane profile in the pupil, which in turn determines intensity distribution of the vane as an aperture. Straight vane projects a spike that is centered over diffraction pattern, as illustrated on FIG. 109. Since "dark aperture" created by the vane becomes a part of the wavefront, it projects a spike centered at the chief ray (i.e. center of the diffraction pattern), extending orthogonally to the vane orientation, regardless of its orientation in the pupil, or length (shorter section will produce wider, fainter spike).
FIGURE 109: TOP LEFT: Spider vane diffraction effect is one of a narrow,
elongated rectangular aperture. Its diffraction pattern extends
appropriately less in the direction of elongation, than in the direction orthogonal to
it. The ratio between these two pattern extensions is 1/ς, with ς being the widthtolength ratio of the vane. Consequently, it makes the
central spider vane maxima ~1/ς times wider than the Airy disc of a
telescope. Peak PSF intensities of the vane vs. Airy disc are
proportional to the ratio of their respective areas.
CENTER: Intensity distribution*
within diffraction pattern of 2x200mm opening centered over 200mm
ƒ/10
mirror (so ς=0.01), calculated by OSLO. Its central diffraction maxima is nearly 1mm long (purple), and nearly 0.01mm wide (green, magnified
below). At
0.0134mm and 550nm, the Airy disc is only slightly wider than
the spike width, and nearly 80 times higher (blue).
The central vane maxima is ~70 Airy disc diameters long, but how much of it
is visible  if any  depends on star's telescopic brightness and
magnification. Practically all
visual effect of the vane results from its central maxima. With ~80
times (the reciprocal of the area ratio) lower intensity than the
telescope's PSF central maxima (showing intensity distribution over the
Airy disc), it is fainter here than the first bright ring. Its own second
maxima is another 21 times fainter, nearly as faint as the 5th bright ring of
a perfect aperture. However, similarly to the first bright ring,
the central spike appears nearly half as bright as the disc at high
telescopic brightness levels, due to the logarithmic
intensity response of the eye (since its actual intensity is so
much lower, it fades away much sooner with the drop in brightness, as
its intensity approaches visual threshold of detection).
Above, to the right, the highmagnification simulation of the effect of
a 4vane spider on the diffraction pattern of a
bright star, with the spikes clearly visible, extending far out from the
central disc. Note that, all else equal, the spike width is greater the
greater central obstruction, due to the inverse slit aperture formed by
the vane having its length reduced by a factor (1o)/2, o
being the relative linear obstruction size (for instance, spike maxima
in the presence of D/3 central obstruction will be three times wider
than that of a vane spanning the entire aperture; with the
combined intensity of its two sections lower by 1/3).
BOTTOM LEFT: PSF of a double slit/vane has double the
central intensity of a single slit/vane of the same width, with the central maxima
of a single vane effectively
fractionalized into 2s1 maximas (including central maxima),
s being the slit/vane separation in units of their (equal)
width W. BOTTOM RIGHT: PSF of a multiple slit/vane has the central
intensity higher by a factor of N than a single slit, N being the slit/vane number.
Within the width of diffraction envelope of a single slit/vane central
maxima, it forms central maxima narrower approximately by a factor
1/5(N1)s, with (N2) subsidiary maximas between subsequent
principal maximas (sth principal maxima is suppressed by a
diffraction envelope null).
Since at these small angles there is practically no difference between the angle and its tangent, linear length of the spike maxima is approximately 2λƒ/w, with ƒ being the mirror focal length; substituting the vane width w in terms of the aperture diameter as w=ςD gives the linear spike length as ~2λF/ς, F being the telescope focal ratio. As the two insets on the bottom of FIG. 109 show, it is possible to reduce diffraction effect of a spider vane by replacing a single vane with two or more parallel vanes. Multiple vane replaces a single central maxima of a single vane with multiple subsiding maximas covering bearly identical width angularly. Intensity of the central maxima is proportional to the combined vane area, thus for the reduction in energy transferred from the Airy disc, such multiple vane would need to have unit vanes of lesser width than a single vane it would replace. Curved vane spider The intense spike produced by a straight vane can be visually eliminated by curving the vanes. The result is a curved vane spider. Diffraction effect of a curved vane can be illustrated by breaking it into a number of smaller, practically straight sections, with varying orientations (FIG. 110a). While the total amount of energy produced by a curved vane is identical to that of a straight vane of equal length and thickness, it is spread out wide, making it practically invisible (it still lowers the contrast the same, on average). The Strehl degradation factor is somewhat different from that for the straight vanes (Eq. 65):
with α=180/N being the vane arch angle in degrees. However, the result is only slightly lower for given count (N) and relative thickness (τ) of the vanes, reflecting slightly greater curved vane length.
