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6.3.1. Star testing telescope quality

As FIG. 59 shows, even slight presence of any wavefront aberration changes the form of diffraction pattern, leaving its unique fingerprint on it. With the knowledge of what those fingerprints look like, with some practical experience, the aberrations can be detected and, most often, quantified with sufficient accuracy. Thus, all that is needed to test telescope optics for quality is a single point-source of light. It can be either a star, or a small, man-made source of light that fits the definition of a point-source. The telescope should be well collimated, and in thermal equilibrium with surrounding air (depending on telescope size, type and initial differential, it can require anything from minutes to hours).

In order to visually analyze diffraction pattern, it has to be sufficiently magnified. Minimum magnification for conducting star test is considered to be 25x per inch of aperture (equal to the aperture diameter in mm), but more is better. Optimum magnification level is probably between 40x and 50x per inch, combined with moderate defocus, of between 3 to 5 waves (number of rings in the defocused pattern roughly corresponds to the defocus in waves).

When testing on a star, it shouldn't be too bright, nor too faint; either can hide more intricate, yet potentially important features of the diffraction pattern. Optimum level of brightness for a 6 inch aperture is ~2nd magnitude star, which helps define best star magnitude for the test, in terms of aperture diameter D, as m~5logD-8.9 for the aperture D in mm, or m~5logD-1.9, for D in inches. Test star should be close to zenith, to minimize the effect of seeing, although for telescopes without tracking mechanism Polaris may be the best overall compromise. Needless to say, less than good seeing quality will compromise reliability of star test results (steady air is also required for artificial star testing; no heat radiating object or areas should be close to the light path).

When star testing with an artificial star, two more requirements have to be met: (1) angular size of the light source needs to be less than 1/2 of the Airy disc size, and (2) distance between the source and the telescope needs to be large enough to keep spherical aberration induced by finite object distance negligible.

The first requirement demands the artificial star to be what it needs to be for the test: effectively a point source of light. Diffraction theory shows (Optical Imaging and Aberrations 2, V. Mahajan, p214), that if the source diameter exceeds 1/4 of the Airy disc's, resulting diffraction pattern begins to begins to change: its full width at half maximum (FWHM), first minima radius and overall ring structure all become larger. At the source diameter of 1/2 the Airy disc's, the FWHM is nearly 15% larger, with the first minima nearly doubling in radius. At the source size equaling the Airy disc's, the FWHM is already 60% larger, and ring structure diminishes further. There is no specifics on how it affects defocused patterns, but it is a common sense to try to preserve the form of diffraction pattern produced by artificial star closely resembling the one that we are comparing it to. With today's availability of materials and products, this shouldn't be an obstacle.

Obviously, angular size of an artificial star is a function of its diameter and its distance from a telescope. A simple visualization of the Airy disc in the focus of a telescope, with two lines extending from its top and bottom to cross at the aperture stop and diverge outwards, helps define the size of Airy disc projection for any given distance from the telescope. Knowing that the Airy disc diameter in radians is given by 2.44λ/D, which for λ=0.00055mm comes to 1/745D for the aperture D in mm, linear diameter corresponding to angular Airy disc diameter at any distance L is given by Ø=L/745D. Since we want to be as close to an actual point-source pattern as possible, the target size for the artificial star is 1/4 as much, or

Ø ~ L/3000D

(note that L needs to be in the same measuring unit as D, here in mm). For instance, for D=100mm telescope, an artificial star placed at 50m distance shouldn't be significantly larger than 0.17mm in diameter. For distance L in feet, aperture D in inches, maximum source diameter Ø in mm is Ø~L/250D.

It is a bit more complicated when it comes to determining artificial star distance that will not induce spherical aberration appreciably affecting test results. The complexity arises mainly from the great variety of different telescope systems in use today. While they are all optimized for object at infinity - or at least at a large distance - the amount of sensitivity to reduced object distance can vary significantly from one type to another. Some systems are easier to deal with, in a sense that they come with the basic specifications known and/or relatively constant. Some others have undetermined optical specs, thus cannot be predicted with respect to their specific object distance sensitivity.

Among the systems that are fairly standard are single mirror systems: Newtonians with either paraboloidal or spherical mirror. For object distance in units of mirror's focal length LO/ƒ, and its reciprocal value ψ=ƒ/LO, the P-V wavefront error of spherical aberration at best focus induced by object distance is given by a simple relation,

where K is the mirror conic, D the aperture diameter in mm, and F the focal ratio. For spherical mirror, this is not even necessary; being under-corrected for object at infinity, and with closer objects inducing overcorrection, it actually gets corrected by reduced object distance, the closer object, the more so - up to its very center of curvature, where it provides perfect imaging.

  For a paraboloid, which is axially perfect for object at infinity, there is a price to pay with closer objects and the currency is over-correction. Substituting K=-1 gives Ws=(ψ-1)ψD/512F3,  and neglecting the ψ term in the bracket (for any serious test, object needs to be significantly farther away than 10 focal lengths, which makes ψ significantly smaller than 0.1), it reduces to Ws=ψD/512F3. This gives the object (i.e. star) distance in terms of the wavefront error as

Substituting optional maximum tolerable P-V error of spherical aberration for Ws gives the appropriate minimum distance for the artificial star. For instance, by substituting W=λ/20=0.0000275mm for λ=550nm, gives the distance for this error level for D=400mm, ƒ/4, as LO=710m.

Obviously, required artificial star distance becomes impractical for larger, fast paraboloids. Is 1/20 wave error tolerance really necessary? It is; moreover, it may be still to much. For instance, if a mirror is 1/6 wave P-V inherently over- or under-corrected, a 0.05 wave of over-correction induced by the object distance would alter test result into -1/4.6 wave or 1/8.6 wave P-V, respectively. For accurate star testing, the error induced by object distance shouldn't significantly exceed 1/50 wave P-V. This pretty much rules out an artificial star test for larger Newtonians.

Catadioptric Newtonians with full-aperture Maksutov or Schmidt corrector are significantly less sensitive to reduced object distance than paraboloidal Newtonians, due to their spherical mirrors. Catadioptric two-mirror systems are not uniform enough in their production types to fall under some type of generalization.

For all-reflecting two-mirror systems, close object error of spherical aberration is given by Eq. 92, and for typical commercial SCT by Eq. 120.3.

Ordinary doublet achromat is very tolerant to the reduction in object distance in focal ratios ~ƒ/10 and slower. It is in part due to relatively small apertures, but even a 200mm achromat will likely generate less than 1/20 wave P-V of under-correction with the object (artificial star) as close as 10 focal lengths away (given relative aperture, the error level is nearly in proportion to the aperture size). On the fast end, however, the sensitivity can be several times, or more, greater. A 4 inch ƒ/6 achromat can generate in excess of 1/5 P-V of under-correction with the object at 10 focal lengths away, due in part to the generated lower-order aberration falling out of balance with the higher-order component (the error is nearly inversely proportional to object distance). This aberration duality makes the sensitivity of these instruments to object distance fairly unpredictable, because the level of higher-order aberration and proportion of balanced lower- and higher order spherical aberration vary from one system to another. Similar applies to apochromatic refractors.

Harold Suiter's "Star Testing Astronomical Telescopes" discusses in details star testing, connecting it to the underlying optical theory. An interesting new development (relatively speaking) is Roddier's test, (freeware) which uses CCD image of two defocused diffraction patterns of a real star to determine wavefront quality (seeing effect is averaged out through the exposure length, and also relatively insignificant, due to the large size of defocused patterns).