Open access

A Unified Approach to Analysing the Anisoplanatism of Adaptive Optical Systems

Written By

Jingyuan Chen and Xiang Chang

Submitted: May 3rd, 2012 Published: December 18th, 2012

DOI: 10.5772/54602

Chapter metrics overview

1,967 Chapter Downloads

View Full Metrics

1. Introduction

To improve the quality of a laser beam propagating in atmospheric turbulence or to improve the resolution of turbulence-limited optical systems, adaptive optics (AO) (Hardy 1998; Tyson 2011) has been developed. In classical AO systems, the compensation is realized by real-time detection of the turbulence-induced perturbations from a source (beacon) using a wave-front sensing device and then removing them by adding a conjugated item on the same path using a wave-front compensating device.

However, the perturbations caused by the beacon and the target may not be the same, so when the perturbations measured by the beacon are used to compensate the perturbations caused by the target, the compensation performance is degraded. These effects are referred to as anisoplanatism (Sasiela 1992). Anisoplanatic effects are present if there is a spatial separation between the target and beacon (Fried 1982), a spatial separation between the wave-front sensing and compensating apertures (Whiteley, Welsh et al. 1998), when time delays in the system cause the beacon phase and the target phase to be only partially corrected due to atmospheric winds or motion of the system components (Fried 1990) or when the beacon and target have different properties such as distributed size (Fried 1995; Stroud 1996) or wavelength (Wallner 1977), and so on.

Conventionally, all kinds of anisoplanatic effects are studied individually, assuming that they are statistically uncorrelated, and the total effects are obtained by summing them all together when necessary (Gavel, Morris et al. 1994). This conventional approach has a rich history dating back to the earliest days of AO technology and has obtained many good results. But this approach is very limited, because for actual applications of AO systems, many kinds of anisoplanatic effects exist simultaneously and are dependent on each other (Tyler 1994). It is increasingly obvious that these methods are inadequate to treat the diverse nature of new AO applications and the concept of anisoplanatism, and the associated analysis methods must be expanded to treat these new systems so their performance may be properly assessed.

Although anisoplanatism takes many forms, it can be quantified universally by the correlative properties of the turbulence-induced phase. Therefore, instead of investigating a particular form of anisoplanatism, this paper concentrates on constructing a unified approach to analyse general anisoplanatic effects and their effects on the performance of AO systems. For the sake of brevity, we will consider only the case of classic single-conjugate AO systems and not consider the case of a multi-conjugate AO system (Ragazzoni, Le Roux et al. 2005).

In section 2 the most general analysis geometry with two spatially-separated apertures and two spatially-separated sources is introduced. In section 3, we introduce the transverse spectral filtering method which will be used to develop the unified approach for anisoplanatism in this chapter and the general expression of the anisoplanatic wave-front variance will be introduced. In section 4, some special geometries will be analysed. Under these special geometries, the scaling laws and the related characteristic quantities widely used in the AO field, such as Fried’s parameter, the Greenwood frequency, the Tyler frequency, the isoplanatic angle, the isokinetic angle, etc., can be reproduced and generalized. In section 5, two specific AO systems will be studied to illustrate the application of the unified approach described in this chapter. One of these systems is an adaptive-optical bi-static lunar laser ranging system and the other is an LGS AO system where, besides the tip-tilt components, the defocus is also corrected by the NGS subsystem. Simple conclusions are drawn in section 6.


2. General analysis geometry

In the development that follows, we will employ the geometry shown in Figure 1, which is introduced by Whiteley et al. (Whiteley, Roggemann et al. 1998). This geometry shows two apertures, including sensing aperture and compensation aperture, whose position vectors are given by rsand rc. Two optical sources, including target and beacon, are located by position vectors rtand rb, respectively. The position vectors of the two apertures and the two sources share a fixed coordinate system. A vertical atmospheric turbulence layer, located at altitude z, is also shown in Figure 1.

The projected separation of the aperture centres in this turbulence layer is given by


where d=rc-rsis the distance of two apertures, Abszand Atczare the layer scaling factors given by Absz=z-rsz^/rb-rsz^and Atcz=z-rcz^/rt-rcz^, while αzand γzare propagating factors of beacon and target, and defined by αz=1-Absz, and  γz=1-Atcz.

Figure 1.

General geometry of the adaptive optical system

Under some hypotheses, these expressions can be further simplified. We suppose two apertures are at the same altitudes and select the centre of the sensing aperture as the origin of coordinates. We express the positions of target and beacon with the zenith angle and altitude as(θt, L)and(θb, H), respectively. We notice that in studying anisoplanatic effects, the offsets angular is very small in general (Welsh and Gardner 1991), i.e., θ1, then Eq. (1) is well approximated by


where θ=θt-θbis the angular separation between target and beacon. At the same time, the propagating factors can be simplified to αz=1-z/H, and γz=1-z/L.

Further, if we consider delayed-time (τ) of the compensating process, then the projected separation can be expressed as


where vzis the vector of wind velocity in this turbulent layer.

The above is the most general geometric relationship of AO systems. Depending on the conditions of application, more simple geometry can often be used to consider the anisoplanatism of AO systems. Some examples are showed in Figure 2. When the target is sufficiently bright, wave-front perturbation can be measured by directly observing the target. Thus an ideal compensation can be obtained and no anisoplanatism exists. This case is showed in Figure 2(a). In general, the target we are interested in is too dim to provide wave-front sensing, another bright beacon in the vicinity of the target must be used, as depicted in Figure 2(b). In this case, the so-called angular anisoplanatism exits (Fried 1982). In more general cases, a naturally existed object (NGS) cannot be find appropriately, to use AO systems, artificial beacons (LGS) must be created to obtained the wave-front perturbations (Happer, Macdonald et al. 1994; Foy, Migus et al. 1995). Then so called focal anisoplanatism (Buscher, Love et al. 2002; Muller, Michau et al. 2011) appears because of an altitude difference between LGS and target, as depicted in Figure 2(c). Figure 2(d) illustrates that a special anisoplanatism will be induced when a distributed source is used as the AO beacon because it is different from a pure point source (Stroud 1996). Distributed beacons are often occurred, for example, a LGS will wander and expand as a distributed source because of the effects of atmospheric turbulence when the laser is projected upward from the ground (Marc, de Chatellus et al. 2009). In Figure 2(e), the anisoplanatism induced by a separation of the wave-front sensing and compensation aperture is illustrated. With many applications, such as airborne lasers, the separated apertures are indispensable because of the moving platform (Whiteley, Roggemann et al. 1998). Figure 2(f) illustrates a hybrid case, in which many anisoplanatic effects coexist at the same time.

All these special anisoplanatic effects are degenerated cases and can be analysed under general geometry. In the following section, we will construct the general formularies of anisoplanatic variance under the most general geometry.

Figure 2.

Some special cases of geometry and anisoplanatism. (a) ideal compensation, where the target is also used as the beacon; (b) angular anisoplanatism; (c) focal anisoplanatism; (d) extended beacon; (e) separated apertures; (f) hybrid beacon - many anisoplanatic effects existing at the same time.


3. Transverse spectral filtering method and general expressions of corrected (anisoplanatic) wave-front variance

Sasiela and Shelton developed a very effective analytical method to solve the problem of wave propagating in atmospheric turbulence (Sasiela 2007). This method uses Rytov’s weak fluctuation theory and the filtering concept in the spatial-frequency domain for coordinates transverse to the propagation direction. In the most general case, the variance of a turbulence-induced phase-related quantity for the propagating waves, when diffraction is ignored, can be written as:


where Lis the propagation distance and k0is the space wave number, which when related to wavelengthλby k0=2π/λ; Φκ,zis two-dimensional transverse power spectrum of fluctuated refractive-index at the plane vertical to the direction of wave propagation and κ=κ,φ; fκ,zis the transverse spectral filter function related to this calculated quantity, whose explicit form can be determined by the corresponding physical processes.

For the atmospheric turbulence, the two-dimensional transverse power spectrum of fluctuated refractive-index can generally be written as:


where Cn2zis refractive-index structure parameter which is allowed to vary along the propagation path, and gκis the normalized spectrum. If gκ=1, then the classic Kolmogrov spectrum is obtained.

Now substitute Eq. (5) into Eq. (4), and sequentially perform the integration of wave vector κ=κ,φat the angular and radial components (Sasiela and Shelton 1993), then the variance reduces to


in which radial and angular integration can be written respectively as:


To evaluate the integral Eq. (6), the expression of the filter function must be given. We will introduce the anisoplanatic filter function for general geometry illustrated in Figure 1. The anisoplanatic filter function can be created from some complex filter functions, describing the process related to the observed target and beacon respectively, by taking the absolute value squared of their difference.

Clearly, when zH, the anisoplanatic filter function is


While when z<H, this item can be expressed as:


In above two equations, Gκis the complex filter function corresponding to the wanted quantity, while Gsκ,zis a complex function which can describe the characteristic of the beacon (such as distributed or point-like). When writing this equation, we have supposed that the main physical processes are linear and their complex filter function can be cascaded to form the total filter functions.

Below we list some explicit expressions of complex filter functions.

The transverse complex filter function for a uniform, circular source with angular diameter θr, can be expressed as:


Here Jnis the nth-order of Bessel function of the first kind; Similarly, the filter function for a Gaussian intensity distribution with 1/eradius θr, has a complex filter function


We also notice that for a point-like beacon, the filter function is simply 1.

For the global phase, the complex filter function is

Gϕκ,ρ=expi κρE13

The expression of the complex filter function for Zernike modeZ(m,n)depends on its radial (n) and azimuthal (m) order. For m=0, it can be written as:


For m0, it is given by


In previous two equations, Dis the diameter of aperture and


By the above complex filter functions, the expressions of anisoplanatic filter functions of global phase and its Zernike modes can be established explicitly.

For the total phase, When zH, from Eq. (9) and Eq. (13), it is


While when z<H, from Eq. (10) and Eq. (13), the result is


Similarly, the anisoplanatic filter functions for Zernike modes can also be established. For the case z<H, when m=0, it can be given by the expression


When m0, for the x, ycomponent of Zernike mode, we can write their anisoplanatic filter functions as follows:

Fn,mxκ,z=Nn2γzκ+Nn2αzκGs2κ,z+-2NnγzκNnαzκGsκ,z J0szκ--1mJ2mszκE20
Fn,mxκ,z=Nn2γzκ+Nn2αzκGs2κ,z-2NnγzκNnαzκGsκ,z J0szκ+-1mJ2mszκE21

It is easy to find that if we define a new quantity as follows:


then we can obtain

Fn,mκ,z = Cm[Nn2γzκ+Nn2αzκ Gs2κ,z-2 Nnγzκ Nnαzκ Gsκ,z J0sz κ]E23

Where Cmis a constant factor related to the azimuthal order m. If m=0, then Cm=1; otherwise Cm=2.

Similarly for the case zH, the corresponding result is


4. Some special cases

In the previous section the transverse anisoplanatic spectral filter functions for the general geometry of adaptive optical systems have been established. In this section we consider some special geometric cases, where asymptotic solutions of integrals can be obtained.

4.1. The anisoplanatism induced by separated apertures and its related characteristic distances

We first consider a simple case, where only the anisoplanatism induced by two separated apertures exists and the others are ignored. Let τ=0, θ=0, Gsκ,z=1, and L=H=+(i.e., γz=αz=1), and taking into account the limitation limx0N0x=1, then Eq. (18) and Eq. (23) reduce to


The anisoplanatic phase variance is easily obtained. Substituting Eq. (25) into Eq. (6), and using the Kolmogrov spectrum, i.e., gκ=1, the integral is equal to


Here we have calibrated the variance with a new characteristic distance d0, defined as

d0=0.526 k0-6/5μ0-3/5E28

This is about 1/3of the atmospheric coherence length r0=0.423k02μ0-3/5, Where μmrepresents the mth (full) turbulence moments. From Eq. (27), we find that the anisoplanatic variance induced by separated apertures meets the 5/3power scaling law with the distance of separated apertures.

For AO systems, the piston phase variance is not meaningful and can be removed from the total variance. Their difference, i.e., the piston-removed phase variance, cannot be expressed analytically for arbitrary distances, while for very small and very large distance their asymptotic solutions can be found. We first calculate in these limitations the wave vector integral of the piston-removed anisoplanatic phase filter function Iϕeff,aniso=Iϕ-I0, which can be found easily from the Eq. (79) and (80) in Appendix with n=0.

When dD, expanding Iϕeff,anisoto second order of D/d, the result is

Iϕeff,aniso ~ D25/3-4 Γ-5/6Γ7/3π Γ17/6Γ23/6-Γ1/64 Γ5/6Dd1/3E29

While dD, expanding it to fourth-order of d/D, the result is

Iϕeff,aniso ~-Γ-5/6Γ11/6D25/3dD5/3+Γ7/3Γ-5/6π Γ17/6Γ23/6D25/3dD25142541472dD2-935144E30

On the other hand, the wave vector integral of the piston-removed phase filter function for a single wave beam is easy to find and can be expressed as:

Iϕeff,single=-2 Γ-5/6Γ7/3π Γ17/6Γ23/6D25/3E31

From the above equations we find that in the limitation of dDthe piston-removed anisoplanatic phase variance tends to be twice that of the piston-removed phase variance of a single wave. This is predictable, because when the separated distance of apertures is large enough, the correlation of waves from two separated aperture is gradually lost, and these beams are statistically independent of each other. We also find in the limitation of dDthe piston-removed anisoplanatic phase variance remains the 5/3 power scaling law with the separated distance, which is same as that for the total phase in Eq. (27).

There are many ways to define a related characteristic distance. For an AO system, if the piston-removed anisoplanatic phase variance is greater than the same quantity for a single wave, that is to say


Then the compensation is ineffective and the AO system is not needed. We can define the uncorrected distance duncof two separated apertures as the smallest distance satisfied above inequality. Using Eq. (30), Eq. (31) and Eq. (32), an approximation of this characteristic distance can be given by dunc=0.828D.

On the other hand, to achieve a better performance, the residual error of corrected wave must be small enough. Similar to the isoplanatic angle, we can define the isoplanatic distance as the separated distance of apertures at which the residual error is an exact unit. From the scaling law of Eq. (27), this distance is same as d0, i.e., diso=d0.

The above two characteristic distances (duncand diso) give different restrictions to an apertures-separated AO system. Other characteristic distances can also be defined. For example, for such an AO system, we can define the effective corrected distance (deff) as the separated distance of apertures at which the AO system can work effectively. Obviously this distance can be determined by the smaller of the above two characteristic distances, namely,


In general, the inequality diso<duncis always satisfied, so the effective corrected distance is deff=diso=d0.

Similar to the above analysis and definitions for total phase, anisoplanatic variances and related characteristic distances can be determined for arbitrary Zernike modes. The final result is complex and can be expressed with generalized hypergeometric functions (Andrews 1998). In order to obtain a simpler close solution, we consider the limit case of very large or very small separating distance.

From Eq. (80), in the limitation dD, the integral is approximately equal to

In,mz=Cm11 Γ7/3Γn+1/6(1+n)28/3π Γ17/6Γ17/6+ndD2D5/3E34

Furthermore, performing the integration at the propagating path, the asymptotic value of the anisoplanatic phase variance for Zernike mode Z(m,n)is obtained as follows:

σn,m2= 0.879Cmk02(1+n)Γn+1/6Γn+17/6D1/3μ0d2E35

If we defined the isoplanatic distance of the Zernike mode Z(m,n)dn,m;isoas the distance satisfied the condition σn,m2=1, then the variance can be calibrated as:


This characteristic distance can be determined as follows:

dn,m;iso= 1.067k0Γn+17/6 D1/3Cmμ0n+1Γn+1/6E37

For a single beam, the expression corresponding to Eq. (34) is (n1)

In,m;singlez=Γ7/3Γn-5/6(1+n) Cm22/3π Γ17/6Γn+23/6D5/3E38

From Eq. (34) and Eq. (37), and another inequality similar to Eq. (32), the uncorrected distance of the Zernike mode Z(m,n)can be defined as:


Similarly, the effective distance of the Zernike mode Z(m,n)can be defined as (at n1):


When the separated distance of the two apertures is smaller than this characteristic distance, the Zernike mode Z(m,n)of turbulence-induced phase can be compensated effectively by the AO system. In Eq. (40), the Minimum operator is evaluated throughout all the field of m, so the result is no longer dependent on m.

In Figure 3, we show the typical values of the characteristic distances dn;effdefined above for the separated-apertures-induced anisoplanatism with D=1.2m. As a comparison with the total phase, the value of piston-removed quantity d0is also showed in the same figures at n = 0.

In Figure 3(a), the relationship among dn;effand the other two characteristic distances (for dn,m;isoand dn,m;unc, their values also select the minimum in all the ms) are showed for λ=532nm. From this figure, we find that the isoplanatic distance is monotonous - increasing with the radial order of Zernike mode - while the uncorrected distance is decreasing with it. Therefore, the effective distance is determined by the isoplanatic distance when the radial order is small (such as for the tip-tilt, defocus, et al) and by the uncorrected distance when the radial order is large. We also find that the effective distances for small ns are usually greater than those for the (piston-removed) total phase, so when only a few low-level Zernike modes need to be compensated for, apertures with greater separated distance can be used.

Other sub-figures in Figure 3 show the effective distances for different compensational orders at different turbulent intensities and wavelengths. In Figure 3(b), four different turbulent intensities (r0=3cm, 6cm, 9cmand 12cmat reference wavelength of λ=500nm) are compared. In Figure 3(c), the effective distances for two different turbulence intensities (r0=5cmand10cm) and two different wavelengths (λ=532nmand 1064nm) are compared. We can find that the effective distances are smaller at stronger turbulences or smaller wavelengths.

In Figure 3(d), the relationships between the effective distances and turbulence intensities are showed for four different compensational orders (n=1, 2, 3, and 5) at λ=532nm. This shows that the effective (or uncorrected) distances are not related to the turbulence intensities for lager compensational orders, such as that for n=5.

Figure 3.

The characteristic distances for the anisoplanatism of separated apertures. (a) The relationship among three characteristic distances,λ=532nm; (b) The effective distances at for four different turbulent intensities,λ=532nm; (c) The effective compensational distances at different turbulent intensities and wavelengths; (d) The relationship between the effective distances and turbulence intensities for four different compensational orders,λ=532nm

4.2. The anglular anisoplanatism and related characteristic angles

Now we consider the geometry where only angular anisoplanatism exits. Let d=0, τ=0, γz=αz=1, and Gsκ,z=1, then Eq. (18) and Eq. (23) reduce to


Substituting Eq. (41) into Eq. (6), and using the Kolmogrov spectrum, the result is σϕ2=θ/θ05/3, here θ0is the well-known isoplanatic angle defined as (Fried 1982) θ0=2.914k02μ5/3-3/5.

Similarly, in the limitation of very small offset angle, i.e., θzD, the effective corrected offset angle between beacon and target can be defined and determined by θeff=θ0.

Using Eq. (42), the angular anisoplanatism of Zernike modes can also be calculated. The results can be expressed with the generalized hypergeometric functions, and in some limit conditions, a more compact expression can be obtained.

We consider the limitation of θzD. Using Eq. (80) in Appendix, the angular anisoplanatism of Zernike mode Z(m,n)can be expanded to the turbulence second-order structure constant moments and can be expressed as (n1)


where the characteristic angle

θn,m;iso=1.06665k0μ21/2Γn+17/6 D1/3Cmn+1Γn+1/6E44

can be defined as the isoplanatic angle for Zernike mode Z(m,n), and it is the size of the offset-axis angle between the beacon and the target when the angular anisoplanatism of Zernike mode is unit rad2.

When n=1and m=1, the tip-tilt isoplanatic angle (also called isokinetic angle) is obtained. This characteristic angle can be expressed as:


This is consistent with the results in other research (Sasiela and Shelton 1993).

Similar to anisoplanatism of separated apertures, other characteristic angles can be defined and calculated. The uncorrected offset angle of Z(m,n)can be expressed as:

θn,m;unc=12 Dμ0/μ2/11(6n-5)(6n+17)E46

and the effective offset angle of the n-order Zernike mode can be determined by


In Figure 4, the typical values of the characteristic angles θn;effdefined above are showed at D=1.2m. In Figure 4(a), we compare the values for two different turbulent intensities (r0=5cm, 10cm) and two different wavelengths (λ=532nm, and 1064nm). We can also find that the effective offset angles θn;efffor small ns are usually greater than those for the (piston-removed) total phase, the same as the characteristic quantities dn;eff. In fact, this is one of main reasons that the use of LGS can partially solve the so-called “beacon difficulty”, because a NGS may be find to correct the lower order modes of the turbulence-induced phase in a field far wider than that limited by the isoplanatic angle θ0. Unlike dn;eff, the effective offset angle θn;effis not only dependent on aperture diameter D, but also turbulence intensity. Therefore, for higher-order Zernike modes, the effectively offset angle is also dependent on the turbulence intensity. In Figure 4(b), the relationships between effective offset angles and turbulence intensities are showed for four different compensational orders (n=1, 2, 3,and5) at λ=532nm.

Figure 4.

The characteristic angles of the angular anisoplanatism for separated beacon and target. (a) the effective offset angles at different turbulent intensities and wavelengths; (b) the relationship between effective offset angles and turbulence intensities for four different compensational orders atλ=532nm

4.3. The time-delayed anisoplanatism and related characteristic quantities

When d=0, θ=0, γz=αz=1, and Gsκ,z=1, then there is only time-delayed anisoplanatism. Now Eq. (18) and Eq. (23) reduce to

Fϕκ,z=21-J0κ vzτE48
Fn,mκ,z=2CmNn2κ1-J0κ vzτE49

Using Eq. (48) and gκ=1 to perform the integration in Eq. (6), the total phase anisoplanatism variance can be expressed as σϕ2=τ/τ05/3, where τ0is normally-defined atmospheric coherence time and equal to τ0=2.913k02ν5/3-3/5, and νnis the nwth velocity moments of atmospheric turbulence defined by νn=0LdzCn2zvmz. This characteristic quantity τ0 is related to the Greenwood frequency. For a single-poles filter (controller), the variance of compensated phase can be scaled as σϕ2=f0/f3db5/3, where f is the effective control bandwidth of AO system and f0is the Greenwood frequency, defined by f0=0.103k02ν5/33/5. We can easily find there is a simple relationship between these two characteristic quantities:


as is first noted by Fried (Fried 1990).

Similarly, in the limitation vzτD, the effective corrected time can be defined and determined by τeff=τ0. For arbitrary Zernike mode of phase, from Eq. (80), when we consider the second order approximation, the anisoplanatic variance is equal to

σn,m2= 0.879(1+n)Γn+1/6Γn+17/6Cmk02D-1/3ν2τ2E51

Using the isoplanatic time τn,m;iso satisfied σn,m2=1to rescale, then the variance can be expressed as:


and its expression is

τn,m;iso=1.06665k0ν21/2Γn+17/6 D1/3Cmn+1Γn+1/6E53

Similar to Greenwood frequency, we can apply Eq. (50) to define a characteristic frequency related to the isoplanatic time in Eq. (53) as follows:

fn,m;iso=0.1256k0ν21/2Cmn+1Γn+1/6Γn+17/6 D1/3E54

This is the characteristic frequency using a single-poles filter to compensate for the Zernike mode Z(m,n) of the turbulence-induced phase.

Further, the effective correction time of arbitrary n-order Zernike model of phase can be defined as:


where the uncorrected time can be expressed as

τn,m;unc=12 Dμ0/ν2/11(6n-5)(6n+17)E56

When using an AO system with a time delay exceeding this characteristic time to compensate for the n-order Zernike model of phase, the compensation is ineffective.

The characteristic quantities τn;effare similar to θn;effand dn;eff. In Figure 5, we show some typical values of the characteristic angles τn;eff.

Figure 5.

The characteristic times for the time-delay anisoplanatism. (a) The effective times at different turbulent intensities and wavelengths; (b) The relationship between effective times and turbulence intensities for different compensational orders atλ=532nm.

When n = 1and m = 1, the isoplanatic times or the characteristic frequencys for the tip-tilt component of the turbulence-induced phase are obtained as: τ1,1;iso=0.668k02ν2D-1/3-1/2or f1,1;iso=0.4864 λ-1ν21/2 D-1/6. It should be noted that these results are slightly different with others. In many studies, the tilt anisoplanatic variances are calibrated as: σα2=15λD2τstτ0t2or σα2=λD2fTf3db2, Where the characteristics time (Parenti and Sasiela 1994) and frequency (Tyler 1994) are defined by τ0t=0.512k02ν-1/38/15ν14/37/15D-1/3-1/2or fT=0.368 λ-1ν21/2 D-1/6. These results are slightly different from ours because different methods of series expanding are used. However, the differences are minor and our expressions have simpler forms and are more convenient to use.

4.4. The focal anisoplanatism

If the altitudes of beacon and target are different, then focal anisoplanatism appears. When other anisoplanatic effects are neglect (i.e., θ=0, d=0, τ=0, L=+, Gsκ,z=1), the anisoplanatic filter function below the beacon are simplified to


Substituting Eq. (57) into Eq. (6), the anisoplanatic variance for total phase is given by σϕ2=0.5k02μ5/3-D/H5/3, here μm-is the mth lower turbulence moment, defined by μm-=0HCn2zzmdz.

Similarly, using Eq. (58) the anisoplanatic variance of Zernike mode Z(m,n)can also be calculated. In order to obtain a more simple close solution, we consider the limit case of a very high altitude beacon, i.e., Hz. From Eq. (81), when the second-order small quantities are retained, the anisoplanatic variance for Z(m,n)can be approximated by


By this expression, the first two components, i.e., the anisoplanatic variances of the piston and tip-tilt, can be obtained immediately as follows: σP2=σ0,02=0.0834k02D5/3μ2-/H2and σT2=σ1,12=0.3549k02D5/3μ2-/H2.

When analyzing a LGS AO system with a telescope aperture of diameter D, it is useful to express the anisoplanatic variance by σϕ2=D/de5/3, where the characteristic quantity deis a measure of effective diameter of the LGS AO system (Tyler 1994) (i.e., a telescope with a diameter equal to dewill have 1 radof rms wave-front error). Considering the fact that for a LGS system piston is meaningless and tip-tilt is non-detectable (Rigaut and Gendron 1992; Esposito, Ragazzoni et al. 2000), then an approximated value of decan be obtained by


We can further consider the effect of turbulence above the beacon. From Eq. (17) and Eq. (24), the filter functions for the total phase and its Zernike mode Z(m,n)above the beacon are


Therefore the anisoplanatic filter function of the partial phase in which the components of the piston and tip-tilt are removed can be expressed as:


Performing the integration Eq. (6), the corresponding variance is obtained as


Where μ0+is the mth upper turbulence moment, defined by μm+=HCn2zzmdz. So when consider the effect of turbulence above the beacon, the effective diameter can be expressed approximately as


This is the same result as that obtained in other research (Sasiela 1994).

4.5. The anisoplanatism induce by an extended beacon

We now consider the anisoplanatic effect induced by a distributed beacon and neglect other anisoplanatic effects. Let d=0, θ=0, τ=0, and γz=αz=1, then Eq. (18) and Eq. (23) are reduced to


Substituting above two equations into Eq. (6) and performing the integration, the anisoplanatic variance of the total phase and its Zernike components can be obtained. Below we give the corresponding results for a Gaussian distributed beacon and Kolmogrov’s turbulent spectrum, i.e., using Eq. (12) and gκ=1.

For the total phase, the integration can easily be obtained. The result is σϕ2=0.5327 θr5/3μ5/3=0.3608 θr/θ05/3, here μmis the mth turbulence moment, and θ0is atmospheric isoplanatic angle. Obviously, the result is similar to the classic 5/3power scaling law for angular anisoplanatism.

For Zernike component Z(m,n), we consider the limit case of very big θr, i.e., θrz D. From Eq. (82), the approximate results expanding to the second order turbulence moment can be obtained. Here, we only list the first two components (i.e., the anisoplanatic variances of piston and tip-tilt) as follows: σP2=σ0,02=0.5327θr5/3 μ5/3-0.4369 D5/3μ0and σT2=σ1,12=0.3799 D5/3μ0.


5. Two examples for hybrid anisoplanatism

To illustrate the application of the unified approach described in this chapter, we will study two special AO systems as examples in this section. In these examples many anisoplanatic effects exist at the same time, so no analytical solution for anisoplanatic variances can be obtained - only numeric results.

To calculate the anisoplanatic variances, we use the Hufnagel-Valley model:

Cn2z=A exp-z102+2.71016exp-z1500+5.94103w272z10510exp-z103E68

where w is the pseudo-wind, and the altitude zexpressed in meters. The turbulence strength is usually changed by a variation of the wterm or A, the parameter to describe the turbulence strength at the ground. At the same time, the modified von Karman spectrum


will be use. Where κoand κiare the space wave numbers corresponding to the outer scale and the inner scale of the atmospheric turbulence, respectively. To consider the effect of time-delay, we use the Bufton wind model

vz=vg+30 exp-z-94002/48002E70

Where vgis the wind speed on the ground.

5.1. An adaptive-optical bi-static Lunar Laser Ranging (LLR) system

Although the technique of Lunar Laser Ranging (LLR) is one of most important methods to modern astronomy and Earth science, it is also a very difficult task to develop a successful LLR system (Dickey, Bender et al. 1994). One of the main reasons is that the quality of the outgoing laser beams deteriorates sharply due to the effect of atmospheric turbulence, including the wandering, expansion, and scintillation. To mitigate these effects of atmospheric turbulence and improve the quality of laser beams, one can use AO systems to compensate the outgoing beams (Wilson 1994; Riepl, Schluter et al. 1999). In this section we will study the anisoplanatism of a special adaptive optical bi-static LLR system in which the receiving aperture is also used to measure the turbulence-induced wave-front and the outgoing beam is compensated by the conjugated wave-front measured by this aperture. It is a concrete application of the unified approach described in this paper.

For this special AO system, two apertures and the useful point-like beacon (Aldrin, Collins, et al.) and the targets (Apollo 11, Apollo 15, et al.) are separated, so the anisoplanatism is hybrid. Let Gsκ,z=1, L=H(=3.8×108m), and denote respectively the offset distance and angle of apertures and sources as d and θ, then the anisoplanatic filter function in altitude z are reduced to


where γz=1-z/L, sz=γzd+zθ+vzτ, and the corrected time delay has been considered. Using above Equations, the variances can be computed easily, but the results can be expressed by higher transcendental functions with no simpler expressions existing.

In Figure 6, we show the anisoplanatic variances when turbulence-induced wave-fronts are compensated to different Zernike orders.

In the first three sub-graphs, the relationships between the anisoplanatic variances and some important parameters (separation distance of apertures, offset angle of sources, time-delay of the correcting process) are also showed respectively. From Figure 6(a), we can see the variances usually monotonously increase with the separated distance. We can also see that increasing the corrected order the variance will decrease when the separated distance is small, but it will not decrease when the separated distance is increased to a certain scale. This is because the effective distances dn;effare smaller at larger orders, as has been showed in Figure 3. A similar conclusion can be drawn for the offset angle of sources from Figure 6(b) and for the time delay of the correcting process from Figure 6(c).

In Figure 6 (d), the relationship between anisoplanatic variance and turbulence intensity are showed for two wavelengths (λ=532nmand 1064nm) and two corrected orders (n=2and5). In this case, all three anisoplanatic effects (angular, time-delayed and that induced by separated apertures) exist at the same time and the corresponding parameters are selected as d=5cm, θ=2'', τ=2ms.

Figure 6.

The anisoplanatic variances for LLR AO system,D=1.2m. (a) The relationship between residual phase variance and separated distances for four different compensational orders atλ=532nmandr0=10cm; (b) the relationship between residual phase variance and offset angles; (c) the relationship between residual phase variance and corrected time-delays for four different compensational orders atλ=532nmandr0=10cm; (d) the relationship between residual phase variance and turbulent intensities for two different compensational orders (n=2and5) and two different wavelengths (λ=532nmand1064nm)

5.2. A special LGS AO system: Defocus corrected by the NGS subsystem

A laser beacon is insensitive to full-aperture tilt because the beam wanders on both the upward and the downward trips through the atmosphere, so currently when using LGS AO systems other NGS subsystems are usually used to sense and correct wave-front tilt. All other Zernike modes except tip-tilt can be corrected by LGS subsystems, but the corrected performance is limited by the focal anisoplanatism. Besides tip-tilt, the defocus (or focus) mode is another main component of the turbulence-induced phase and decreasing the focal anisoplanatism of the defocus component is very important (Esposito, Riccardi et al. 1996; Neyman 1996). In this section, we consider the performance of a special kind of LGS AO system, in which, besides the overall tilt, the focus mode can also be sensed and corrected by the NGS subsystems. Using this special LGS AO system, the focal anisoplanatism of the defocus mode can be reduced further.

We concentrate on the relationship between the focal and angular anisoplanatism of the defocus mode, and neglect the effects induced by time-delay and separated aperture. We also neglect the correlation between LGS and NGS subsystem, and suppose them to be statistically independent of each other. Then the anisoplanatic filter functions for the NGS subsystem are reduced to

Fn,m;Nκ,z = CmNn2γzκ1-2Gs,Nκ,zJ0κzθN+Gs,N2κ,zE74

While for the LGS subsystem, under the LGS beacon, the results reduce to

Fn,m;Lκ,z=Cm[Nn2γzκ+Nn2αzκGs,L2κ,z-2NnγzκNnαzκGs,L2κ,z J0κzθL]E76

Those above the LGS beacon are same as Eq. (17) and Eq. (24).

In above equations, γz, θN, and Gs,N(or αz, θL, Gs,L) are main related parameters of anisoplanatic effect, and they are the propagating factor, the offset angle, and the filter function of the NGS (or LGS), respectively. Here we have supposed that the altitude of NGS is same as that of the target.

Using these filter functions, the effective anisoplantic variance for this particular LGS AO system can be calculated and expressed as follows:


In this equation, the first two items in parentheses are the contribution of the NGS subsystem, describing the anisoplanatism of tip-tilt and defocus modes respectively. While the items in brackets are the contribution of the LGS subsystem, and the four items are the variance of the total phase, the piston, the tip-tilt and the defocus mode, sequentially. As a comparison, the effective anisoplanatic variance for a usual LGS AO system, in which only tip-tilt mode can be sensed and corrected by the NGS subsystem, can be expressed as:


Obviously, for this special LGS AO system, the contribution of the defocus mode to the effective anisoplanatic variance comes from the NGS system, i.e., σ2,0;N2, while for a usual LGS AO system, it comes from the LGS subsystem.

Below we give some numerical results. We mainly study the changes of the anisoplanatic variance with some control parameters, including the altitudes (LandH), the offset angles (θNand θL), and the angular width (for Gaussian sources: θr,Nand θr,L) of the NGS and LGS sources. Some typical results are showed in the figures below. In our calculation, the altitude of the target L is selected as 500km(a typical value for a LEO satellite), and the wavelength as 1.315μm.

In Figure 7(a) and Figure 7(b), the changes of the anisoplanatic variance with the angular widths and the offset angles of the beacons are given. In this case the invalid piston component of variance has been removed. In these figures, we also compare the values for three different altitudes of beacons, including a NGS (H=L=500km) and two kinds of LGSs with altitude H=15kmand H=90kmrespectively. It is easy to see that the variances generally increase with the offset angles and the angular widths of the beacons. But there is some minor difference for the beacon size: the variance first decrease as beacon size increases, then it increases. We can also see that the changes are more obvious when the altitudes of the beacons are larger, for example, we can see the variance changes from 0.1to1.6rad2when the offset angles changes from 0to10''for NGS, but there are nearly no changes for 15kmRayleigh LGS, as showed in Figure 7(b).

Figure 7.

(a) Anisoplanatism of distributed beacon; (b) angular anisoplanatism; (c) the focal anisoplanatism (below the beacon); (d) focal anisoplanatism (above the beacon); (e) focal anisoplanatism (sum); (f) effective variance.

In Figure 7(c) and (d), the components of anisoplanatic variance below and above the beacon, are given respectively. The values for the total phase and its first three components (piston, tilt and defocus) are showed altogether. In Figure 7(e), the variances for the total phase, the piston and tip-tilt removed phase, and the piston and tip-tilt and defocus removed phase, are showed respectively. When the altitudes of the beacon are more than 20 kmthe variances are almost the same as the results of the NGS. In Figure 7(f), the effective anisoplanatic variances expressed by Eq. (77) are showed for three different offset angles of NGS.

For the special LGS AO system, the anisoplanatic variance of defocus comes from NGS sub-system and not from the LGS subsystems as usual LGS AO systems. In Figure 8, we compare the values of these two variances and the relationship between the altitude of LGS and the offset angle of NGS. The transverse coordinates are magnitudes of the variances. The solid line describes the change of the defocus variances with the altitude of LGS and the altitude of LGS is showed in the left longitudinal coordinates. Similarly, the dotted line describes the change of the defocus variances with the offset angle of NGS and the offset angle of NGS is showed in the right longitudinal coordinates.

From this figure the value of the LGS altitude and the NGS offset angle, having the same value of the variance, can be read directly and some operational conclusions can be drawn.For example, for a Rayleigh LGS (with an altitude of 10kmto20km) the anisoplanatic variance of the focus component has the value between 0.08to0.1rad2, same as that for a NGS with the offset angle between 8''and 9''. Similarly, the sodium LGS (with altitude of 90km) correspond to the offset angle of NGS between 2''and 3''. It is also easy to see that the variance is a monotonically increasing function of the NGS offset angle and a almost monotonically decreasing function of the LGS altitude. Therefore, if the NGS offset angle is smaller or 0''(such as directly imaging of a bright satellite) using NGS to correct the defocus component, the variance is smaller. Otherwise, when the NGS offset angle is larger (for example, when projecting laser beams to a LEO satellite, the advance angle about 10''must be considered) using sodium LGS to correct the defocus the variance is smaller.

Figure 8.

The anisoplanatism of the defocus component


6. Summary

Using transverse spectral filtering techniques we reconsider the anisoplanatism of general AO systems. A general but simple formula was given to find the anisoplanatic variance of the turbulence-induced phase and its arbitrary Zernike components under the general geometry of AO systems. This general geometry can describe most kinds of anisoplanatism appearing in currently running AO systems, including angular anisoplanatism, focal anisoplanatism and that induced by distributed sources or separated apertures, and so on. Under some special geometry, close-form solutions can be obtained and are consistent with classic results, which prove the effectiveness and universality of the general formula constructed in this chapter. We also give some numerical results of hybrid anisoplanatism under some more complex geometry.



Here we give some expressions describing the integrations of the anisoplanatic filter function Fn,mκ,zfor the Zernike mode Z(m,n)with respect to the radial component of the wave vector, i.e.,

Inz=0dκ Fn,mκ,zκ-8/3

Expressions used in section 4.1.- 4.3.

When the filter function is equal to


The results are determined by the sizes of szand γzD. If szγzD, then

Inz=(n+1)Γn-56(γzD)5/321/3Γ7/3/Γ17/6π Γn+23/6-


Further, if szγD, an asymptotic series of small parameter γzD/szcan be found. When expanding to second-order, the results are

Inz=1+nΓn-562Dγz53Γ73/Γn+236 24/3π Γ176--2 γzD/sz2n+1/3Γ116-n2nΓ2+n2 n-562n+2+  2-13/3γzD/sz2E79

if sz<γzD, then

Inz=21/3n+1γzD5/3Γ73Γn-56π Γ176Γn+236-

-Γ73Γn-56π Γ176Γn+2363F2-116,-n-176,n-56;-43,1;szγzD2-

-Γ-73π Γ103szγzD14/33F212,-n-12,n+32;103,103;szγzD2

Further if szγzD, the second-order asymptotic expansions of parameter szγzDare

Inz=(1+n)Γ73 π Γ176γzD253szγzD211 Γn+162 Γn+176-55 Γn+7616 Γn+116szγzD2E80

Expressions used in section 4.4.

When the filter function is equal to


The integrations can be expressed by

Inz=n+1Γn-56D5322n+113Γ176Γn+2 8Γ43Γ2n+3αz53+13Γn+32Γn+236-


-6αz2n-6n-22 2F1-5/6, n- 5/6;n+2;αz2]

When the beacon is high enough (Hz), we can obtain the following asymptotic solution expanding to second-order turbulence moments:

Inz=8n+1108n(n+2)-556237 π Γ-10/3 Γn+23/6Γ2-83Γn-56zH2D5/3E81

Expressions used in section 4.5.

When the filter function is equal to


For the Gaussian source Eq. (12), the results can be expressed as:


+θσz-2n+5/3D2n24nΓn+222F2n-5/6,n+3/2;n+2, 2n+3;-D24θrz2-

-2n+1/62F2n-5/6,n+3/2;n+2, 2n+3;-D22θrz2

If the widths of the distributed source are very large (θrz D), expanding the solutions to second-order terms of small parameter D/(θrz), the results are obtained as follows:

Inz =(1+n)Γn-56 22/3D-5/3Γ73/Γ176 π Γn+236 -2θrz/D5/3-2n2n+1Γn+222n+1/6-1+n-562n+7/6-12(2+n)2θrz/D2 E82


  1. 1. AndrewsL. C1998Special functions of mathematics for engineers. SPIE-International Society for Optical Engineering, Bellingham
  2. 2. BuscherD. FG. DLoveet al2002Laser beacon wave-front sensing without focal anisoplanatism.Opt. Lett.,273149151
  3. 3. DickeyJ. OP. LBenderet al1994Lunar laser ranging- A continuing legacy of the Apollo program.Science2655171482490
  4. 4. EspositoSRRagazzoniet al2000Absolute tilt from a laser guide star: a first experiment.Experimental Astronomy101135145
  5. 5. EspositoSARiccardiet al1996Focus anisoplanatism effects on tip-tilt compensation for adaptive optics with use of a sodium laser beacon as a tracking reference.J.Opt.Soc.Am.A,13919161923
  6. 6. FoyRAMiguset al1995The polychromatic artificial sodium star: A new concept for correcting the atmospheric tilt.Astron. Astrophys. Suppl. Ser.,1113569578
  7. 7. FriedD. L1982Anisoplanatism in adaptive optics.J.Opt.Soc.Am,7215261
  8. 8. FriedD. L1990Time-delay-induced mean-square error in adaptive optics.J.Opt.Soc.Am.A7712241225
  9. 9. FriedD. L1995Focus anisoplanatism in the limit of infinitely many artificial-guide-star reference spots.J.Opt.Soc.Am.A,125939949
  10. 10. GavelD. TJ. RMorriset al1994Systematic design and analysis of laser-guide-star adaptive-optics systems for large telescopes.J.Opt.Soc.Am.A,112914924
  11. 11. HapperWG. JMacdonaldet al1994Atmospheric-turbulence compensation by resonant optical backscattering from the sodium layer in the upper atmosphere.J.Opt.Soc.Am.A,111263276
  12. 12. HardyJ. W1998Adaptive optics for astronomical telescopes. Oxford University Press.
  13. 13. MarcFH. GDe Chatelluset al2009Effects of laser beam propagation and saturation on the spatial shape of sodium laser guide stars.Optics Express17749204931
  14. 14. MullerNVMichauet al2011Differential focal anisoplanatism in laser guide star wavefront sensing on extremely large telescopes.Opt. Lett.,362040714073
  15. 15. NeymanC. R1996Focus anisoplanatism: A limit to the determination of tip-tilt with laser guide stars.Opt. Lett.,212218061808
  16. 16. ParentiR. RandR. JSasiela1994Laser-guide-star systems for astronomical applications.J.Opt.Soc.Am.A,111288309
  17. 17. RagazzoniRBLeRoux, et al. (2005Multi-Conjugate Adaptive Optics for ELTs: constraints and limitations.C. R. Phys.61010811088
  18. 18. RieplSWSchluteret al1999Evaluation of an SLR adaptive optics system. Laser Radar Ranging and Atmospheric Lidar Techniques II. U. Schreiber and C. Werner. Bellingham.Proc. SPIE.38659095
  19. 19. RigautFandEGendron1992Laser guide star in adaptive optics-The tilt determination problem.Astron.Astrophys.2612677684
  20. 20. SasielaR. J1992Strehl ratios with various types of anisoplanatism.J.Opt.Soc.Am.A,9813981405
  21. 21. SasielaR. J1994Wave-front correction by one or more synthetic beacons.J.Opt.Soc.Am.A,111379393
  22. 22. SasielaR. J2007Electromagnetic wave propagation in turbulence: evaluation and application of Mellin transforms. SPIE Press.
  23. 23. SasielaR. JandJ. DShelton1993Transverse spectral filtering and Mellin transform techniques applied to the effect of outer scale on tilt and tilt anisoplanatism.J.Opt.Soc.Am.A,104646660
  24. 24. StroudP. D1996Anisoplanatism in adaptive optics compensation of a focused beam with use of distributed beacons.J.Opt.Soc.Am.A,134868874
  25. 25. TylerG. A1994Bandwidth considerations for tracking through turbulence.J.Opt.Soc.Am.A,111358367
  26. 26. Tyler, G. A. (1994). Rapid evaluation ofd0- the effective diameter of a laser-guide-star adaptive-optics system.J.Opt.Soc.Am.A,11(1): 325-338.
  27. 27. TylerG. A1994Wave-front compensation for imaging with off-axis guide stars.J.Opt.Soc.Am.A,111339346
  28. 28. TysonR2011Principles of adaptive optics (3rd Edition ed.), CRC Press, Boca Raton.
  29. 29. WallnerE. P1977Minimizing atmospheric dispersion effects in compensated imaging.J.Opt.Soc.Am.,673407409
  30. 30. WelshB. MandC. SGardner1991Effects of turbulence-induced anisoplanatism on the imaging performance of adaptive-astronomical telescopes using laser guide stars.J.Opt.Soc.Am.A,816980
  31. 31. WhiteleyM. RM. CRoggemannet al1998Temporal properties of the Zernike expansion coefficients of turbulence-induced phase aberrations for aperture and source motion.J.Opt.Soc.Am.A,1549931005
  32. 32. WhiteleyM. RB. MWelshet al1998optimal modal wave-front compensation for anisoplanatism in adaptive optics.J.Opt.Soc.Am.A,15820972106
  33. 33. WilsonK. E1994An overview of the Compensated earth-Moon-earth laser link (CEMERLL) experiment. Bellingham.Proc. SPIE.21236674

Written By

Jingyuan Chen and Xiang Chang

Submitted: May 3rd, 2012 Published: December 18th, 2012