A&A 390, 801-807 (2002)
DOI: 10.1051/0004-6361:20020740
Changhui Rao - Wenhan Jiang
Adaptive Optics Laboratory, Institute of Optics and Electronics, Chinese Academy of Sciences, PO Box 350, Shuangliu, Chengdu 610209, Sichuan, PR China
Received 20 June 2001 / Accepted 15 April 2002
Abstract
In order to maximize the compensation potential of adaptive optics system for
atmospheric turbulence, an appropriate observing wavelength should be selected on the basis of
system capability and the working conditions to improve the optical resolution of astronomical
telescopes. Based on the analysis of the wavefront residual error of the adaptive optics system, the optimum imaging observation wavelengths giving maximum imaging resolution of a partial
correction adaptive optics system are derived for short-exposure and long exposure imaging
respectively. The developed method is used to evaluate the optimum observing wavelength and the
corresponding imaging resolution for the 61-element adaptive optical system at the 1.2 m telescope
of the Yunnan Observatory.
Key words: telescopes - atmospheric effects - instrumentation: adaptive optics - methods: observational
It is well known that atmospheric turbulence (Roddier 1981) severely limits the resolution of large ground-based telescopes in the visible and near infrared bands. Adaptive optics (Jiang et al. 1995) techniques can be used to correct random optical wavefront distortions induced by the atmospheric turbulence in real time.
The performance requirements for adaptive optics systems (AOS) depend on their mission. In the visible band, large telescopes require very complex AOS with hundreds of correction channels in order to produce high-resolution object images. But the large telescopes with low-order AOS perform well in the near infrared band. The imaging observation wavelength is one of the most significant factors in the requirements of AOS. For ground-based solar telescopes (Rimmele & Radick 1998), high-resolution monochromic imaging observations are usually done at a single wavelength with a very narrow band because of strong enough sunlight. For nighttime astronomical telescopes, a range of wavelengths is often used for imaging observation. For nighttime astronomical adaptive optical systems, the observing wavelength during setting up an observation is generally confined to the end portion of the red visible (R and I bands), the non-thermal near IR (J and H bands), or thermal IR (K band) according to the practical requirements and system capabilities.
In selecting an imaging observation wavelength, two competing effects must be considered. On the one hand, as the imaging wavelength is increased, the wavefront residual error decreases, resulting in a sharper point spread function. On the other hand, diffraction increases with wavelength, producing the opposite effect. For telescopes with partial correction AOS, the appropriate observing wavelength should be selected on the basis of the system capability and the working conditions in order to achieve the best angular resolution.
In previous publications, Tyler (Tyler & Fender 1994) derived an expression for the wavelength giving maximum resolution for the telescopes with AOS. In his study, the imaging Strehl ratio is simplified as , where is the variance of the residual phase error. This is only valid for small residual phase error. For the partial correction AOS, this condition can commonly not be satisfied. In this paper, we derive the expressions of the optimum short-exposure and long-exposure imaging observation wavelength of astronomical telescopes with partial correction adaptive optics based on the analysis for the wavefront residual error of AOS. The paper is organized as follows. The parameters of atmospheric turbulence are briefly introduced in Sect. 2. In Sect. 3, the wavefront residual error of AOS is analyzed by considering the limitation factors of the practical AOS. Section 4 derives the optimum imaging observation wavelength on the basis of the relationship between the angular resolution and the wavefront residual error for the astronomical telescopes with partial correction AOS. In Sect. 5, the optimum imaging observation wavelength is computed for the 61-element adaptive optical system at the 1.2 m telescope of the Yunnan Observatory.
The effects of atmospheric turbulence on astronomical telescopes are commonly
characterized as the following atmospheric parameters: the turbulence coherence length, namely
Fried's parameter r_{0}, the Greenwood frequency ,
the Tyler frequency ,
and the anisoplanatic angle .
These parameters are usually specified at the visible wavelength of 0.55 m (Roddier 1981):
= | (1) |
= | (2) |
= | (3) |
= | (4) |
Most adaptive optics compensation systems apply the conjugate surface of the phase measured by WFS with a pair of active elements consisting of a high-speed TM and a DM. TM is usually used to correct the tilt component of the wavefront distortions induced by atmospheric turbulence. The figure (tilt-removed) component of the wavefront perturbation is compensated by DM. In the practical AOS, the compensation is not perfect because of the individual errors such as the uncompensated turbulence-induced error due to the finite bandwidth of the servo system and the measurement noise.
The main figure residual errors include: (1) uncompensated turbulence-induced figure error due to the bandwidth of the figure compensation servo system; (2) closed-loop figure noise error due to the measurement error of the wavefront sensor; (3) fitting error due to the finite corrector elements; (4) anisoplanatic error due to the angular anisoplanatism and the focal anisoplanatism.
The uncompensated turbulence-induced figure error depends on the temporal power spectrum
of the figure (tilt-removed) component of the turbulence
and the servo control transfer function
:
(5) |
(6) |
(7) |
For high-bandwidth figure compensation, the uncompensated turbulence-induced figure error
at the imaging wavelength
can be obtained with the high-frequency form of the figure
spectrum over the entire frequency range, so that (Li et al. 2000):
= | |||
(8) |
In AOS, the noise resulting from WFS mainly consists of the photon shot noise due to the
finite light intensity and the read-out noise of the detector such as a CCD. Assuming the noise is
white, the closed-loop figure noise error can be obtained as (Rao et al. 2000):
= | |||
= | (9) |
Note that the wavefront measurement noise
relates the noise power spectrum to:
(10) |
(11) |
The uncorrected phase error due to the figure (tilt-removed) component of turbulence at the
imaging wavelength ,
namely figure fitting error, is conveniently expressed in terms of the ratio of the subaperture spacing and the turbulence coherence length (Hardy 1998):
(12) |
When the beacon of AOS and the target object do not lie in the same direction, the error due
to angular anisoplanatism at the imaging wavelength
can be expressed as (Fried 1982)
(13) |
Furthermore, because the atmospheric turbulence is only partially detected by the beacon
light, the use of laser beacons in AOS produces the error due to focal anisoplanatism, which may
be expressed as (Tyler 1994)
(14) |
= | |||
(15) |
The total figure residual error of AOS with the unit of phase rad^{2} at the imaging wavelength
may be expressed as the sum of individual errors in the form
= | |||
= | |||
(16) |
In AOS, the tilt component of turbulence is often measure by quadrant detectors and centroid trackers. This tilt belongs to G-tilt, namely average gradient over the pupil. The main errors involved in compensating the tilt component of turbulence are: (1) uncompensated turbulence-induced tilt error due to the bandwidth of the tilt compensation servo system; (2) closed-loop tilt noise error due to the measurement error of the tracking sensor.
According to the tracking frequency
defined by Tyler (Tyler 1994), see Eq. (4), the uncompensated turbulence-induced tilt error at the imaging wavelength
can be expressed as
(17) |
Similar to the closed-loop figure noise error, the closed-loop tilt noise error at the imaging
wavelength
relates the tilt measurement error
,
the sampling frequency of the tracking system
and the closed-loop -3dB bandwidth of the tracking servo loop to
(18) |
The total tilt residual error with the unit of tilt rad^{2} at the imaging wavelength
is given by the sum of the uncompensated turbulence-induced tilt error and the closed-loop tilt noise error,
= | |||
= | (19) |
The effect of wavefront residual error of AOS on an optical image is to remove energy from the central peak, distributing it into a surrounding halo. The halo is absent for a perfect wavefront, but dominates the image structure in the presence of a wavefront error typical of uncompensated turbulence.
For the astronomical telescope with AOS, the image resolution is most affected. To investigate
the image quality of AOS, it is useful to begin with the extended Marechal approximation, which
provides a relationship between the figure error and the Strehl ratio under weak-turbulence
conditions
(20) |
Assuming all of the energy lost from the central core of the beam is scattered over a region of
width
,
a composite short-exposure image Strehl ratio (Parenti & Sasiela 1994) for partial correction AOS can be shown as
(21) |
(22) |
(23) |
(24) |
Figure 1 presents the short-exposure imaging resolution of AOS versus the observing wavelength for different figure residual root mean square errors. It can be seen from Fig. 1 that for a certain figure residual error, the imaging resolution improves with increasing observing wavelength as the observing wavelength is relatively shorter. When the observing wavelength is longer, the imaging performance gradually becomes worse with the lengthening of the wavelength. Note that there exists an optimum observing wavelength in which the imaging resolution is highest for a certain figure residual error. The larger the figure residual error, the longer the optimum wavelength. So in astronomical telescopes with adaptive optics, the appropriate imaging observation wavelength need to be selected based on the system capability and its mission in order to exploit fully the compensation function of AOS for atmospheric turbulence.
Figure 1: The imaging resolution vs. observing wavelength for adaptive optical systems. | |
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The optimum wavelength would maximize the imaging resolution of the astronomical
telescopes with adaptive optics. For convenience of analysis, a new function
is defined to
used to optimize the imaging observation wavelength of AOS,
(25) |
For short-exposure imaging, the imaging resolution depends mainly on the figure residual
error of AOS, so that
can be written as
= | |||
(26) |
(27) |
(28) |
A= | |
(29) |
= | |
(30) |
(31) |
Figure 2: Optimum short exposure observing wavelength and the corresponding image resolution. | |
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Figure 3: Optimum long exposure observing wavelength and the corresponding image resolution. | |
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Taking the first order derivative for the function
and letting it be equal to zero, we
can write:
(32) |
(33) |
(34) |
= | (35) |
For long-exposure imaging, the imaging resolution depends not only on the figure residual
error but also on the tilt residual error of AOS, Thus
can be simplified as
(36) |
(37) |
(38) |
= | |||
(39) |
Figures 2 and 3 present optimum imaging observation wavelength and the corresponding image resolution for short-exposure imaging and long-exposure imaging respectively. It can be seen from Figs. 2 and 3 that the optimum imaging observation wavelength of AOS depends directly on the wavefront residual error of AOS. The larger the wavefront residual error, the longer the optimum imaging observation wavelength is. Especially, the optimum imaging observation wavelength for short-exposure imaging, see Eq. (33), can be explained as the corresponding wavelength under the condition that the figure residual error is 1 rad^{2}.
Furthermore, the optimal observing wavelength and the corresponding short-exposure imaging resolution according to Tyler and Fender's (Tyler & Fender 1994) result, see Eq. (34), are also presented in Fig. 2. Note that the optimal wavelength derived by Tyler and Fender (Tyler & Fender 1994) is larger than that in this paper. The imaging performance according to Tyler and Fender's result is inferior to the result of this paper. The interpretation is that the imaging short-exposure Strehl ratio in Tyler and Fender's derivation (Tyler & Fender 1994) is approximated as . If the required precision is 10%, the figure residual error should be less than 0.14 rad^{2}. When the figure residual error is equal to 0.6 rad^{2}, the precision can only attain 27%. In contrast with the results of this paper, the percentages of the departure of the optimal wavelength derived by Tyler and Fender (Tyler & Fender 1994) and the corresponding imaging resolution are 41.4% and 10% respectively. Evidently, the imaging resolution based on the calculated optimal observing wavelength in this paper is superior to that according to the optimal wavelength derived by Tyler and Fender (Tyler & Fender 1994). This result shows also that the calculation in this paper is more precise and more effective than the rough estimate carried by Tyler and Fender (Tyler & Fender 1994).
For nighttime astronomical telescopes with adaptive optics, the imaging observations are mostly done at a range of wavelengths. Figure 4 presents the percentage of the short-exposure imaging resolution departure from the optimum resolution as function of the percentage of the observing wavelength departure from the optimum wavelength. As AOS is not operated in the optimum wavelength but just 10% longer or shorter, the resolution degrades only about 1%. This result shows that the derived optimum observing wavelength in this paper can be applied not only in the monochromic observation with very narrow band but also in the nighttime observation with a certain range of wavelength.
Figure 4: The percentage of the short-exposure imaging resolution departure from the optimum resolution as a function of the percentage of the observing wavelength departure from the optimum wavelength. | |
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We have built a 61-element adaptive optical system at the 1.2 m telescope of the Yunnan
Observatory (Jiang et al. 1998) for astronomical observations in the visible range. It consists of a
61-element deformable mirror, a Shack-Hartmann wavefront sensor with 8^{*}8 subapertures and a
digital wavefront processor. The detector of the Shack-Hartmann wavefront sensor is an
intensified CCD with frame rate of 838 Hz. The effective diameter of the system is 1.06 m and the
time delay is 2.8 T (T is the sampling period of the system). Figure 5 shows the experimental
results of the measurement noise of WFS for the measured photoelectrons and its fitting curve.
The measurement noise may be expressed as
(40) |
Figure 5: The measured wavefront noise r.m.s. value vs. photoelectrons per subaperture and per frame. | |
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For this system, Fig. 6 presents the optimum short-exposure imaging observation wavelength and the corresponding image resolution as a function of the measured photoelectrons for the closed-loop bandwidth of 30 Hz, 60 Hz and 120 Hz respectively. During the computation, the anisoplanatic error is not considered and the following atmospheric parameters according to the statistial values at this site are taken: cm, Hz.
Figure 6: Optimum observing wavelength and the corresponding image resolution as a function of photoelectrons per subaperture and per frame for different closed-loop bandwidths. | |
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It can be seen from Fig. 6 that for the reference beacon with high brightness, the larger the closed-loop bandwidth, the shorter the optimum imaging observation wavelength is, and the higher the corresponding resolution. For the reference beacon with low brightness, the reverse is true. This is due to the fact that the uncompensated turbulence-induced error, decreasing with the increasing closed-loop bandwidth, dominates over the total wavefront residual error in contrast with the closed-loop noise error, which is proportional to the closed-loop bandwidth, induced by the measurement error of the wavefront detector for the reference beacon with high brightness. For the reference beacon with low brightness, the closed-loop noise error is larger than the uncompensated turbulence-induced error. In this case, the wider the closed-loop bandwidth, the larger the total wavefront residual error.
In this paper, the figure residual error and the tilt residual error for adaptive optics systems are analyzed. The optimum imaging observation wavelengths giving the maximum resolution of a partial correction adaptive optics system are expressed as the function of the wavefront residual errors for short-exposure and long exposure imaging respectively. As an example, the optimum observing wavelength and the corresponding imaging resolution for the 61-element adaptive optical system at the 1.2 m telescope of the Yunnan Observatory are presented. The results show the optimum imaging observation wavelength of AOS depends directly on the wavefront residual error of AOS. The larger the wavefront residual error, the longer the optimum imaging observation wavelength.
Furthermore, it is necessary to note that the discrete nature of atmospheric transmission bands, the noise characteristics of the detector and its quatumn efficiency etc. must be considered for the selection of the practical imaging observation wavelength of astronomical telescopes with adaptive optics.
This work may be useful not only in designing adaptive optics system for astronomical telescopes but also in planning the experiments for astronomical telescopes with AOS.
Acknowledgements
This work is funded by the Hi-tech Project of China and National Natural Science Foudation of China (No. 19789301). The authors acknowledge the reviewers for valuable suggestions.