Issue 
A&A
Volume 499, Number 1, May III 2009



Page(s)  337  345  
Section  Astronomical instrumentation  
DOI  https://doi.org/10.1051/00046361/200811506  
Published online  08 April 2009 
Roughness scattering in Xray grazingincidence telescopes
F. E. Zocchi
Media Lario Technologies, Località Pascolo, 23842 Bosisio Parini (LC), Italy
Received 11 December 2008 / Accepted 26 February 2009
Abstract
In the framework of the scalar theory of diffraction, we determine the rms width of the angle spread function degraded by surface roughness in reflective grazingincidence optics of cylindrical symmetry for Xray astronomy. Our derivation does not rely on the small roughness approximation, is thus valid for arbitrary roughness values, and takes into full consideration the cylindrical symmetry of the mirrors. The dependence of the rms beam width on both the grazingincidence angles and the radiation wavelength is studied for both single and double reflection optics, the latter being more relevant to Xray telescopes. When the small roughness approximation is applicable, we also derive an expression for the angle spread function of the optical system in the presence of roughness scattering that provides the correct expression for the rms beam width.
Key words: Xrays: general  telescopes  scattering
1 Introduction
A factor limiting the resolution of grazingincidence optics for Xray astronomy is the scattering caused by the surface roughness of the telescope mirrors. A number of Xray space missions (Pareschi & Ferrando 2005; Gondoin et al. 1994; Bookbinder et al. 2008; Citterio et al. 1988; Friedrich et al. 2008; Aschenbach 1988; Weisskopf et al. 2000; Gehrels et al. 2004) have stimulated both theoretical and experimental research (Church & Takacs 1993; Spiller 1994; Harvey 1995a; Karabacak et al. 2000; Stearns et al. 1998; Harvey 1995b; Zhao & Spreybroeck 2003; Harvey et al. 1996; Church & Takacs 1995; Christensen et al. 1988) to understand and characterize in a more robust way the scattering of electromagnetic waves from rough surfaces. The typical resolution requirement at the focal plane of an Xray telescope is sharper than 20 half energy width at Xray photon energy between 0.1 and 80 , depending on the mission (Friedrich et al. 2008; Pareschi & Ferrando 2005; Gondoin et al. 1994), and at a grazingincidence angle in the range between about 0.1 and 1.5. Consequently, the contribution of roughness to the overall optical resolution is sufficiently low to require reflective surfaces polished down to roughness of about 0.2 0.5 rms, typically in the spatial frequency range between 0.01 and 1. Hence, the correlation between surface roughness and radiation scattering is essential to defining the surface quality required by the mirrors.
The interest in the field has been further boosted by other applications of the shortwavelength region of the electromagnetic spectrum, including EUV microlithography (Schellenberg 2008; Bakshi 2008) and EUV microscopy (Foltyn et al. 2004; Silk 1980; Schäfer et al. 2006), just to quote a few. The development of multilayer structures (Spiller 2003; Joensen et al. 1995; Barbee 1986; Yamashita et al. 1999) to enhance the optical reflectivity of mirrors at short wavelengths has also stimulated theoretical and experimental investigations in the field.
The configuration of choice for the optical design of Xray telescopes is based on the type I Wolter architecture (Wolter 1952b) in which the Xray radiation from distant sources is first reflected by a parabolic surface and then by a hyperboloid, both with cylindrical symmetry around the optical axis. The two surfaces are arranged in a coaxial configuration and share a common focus. The second focus of the hyperboloid is the image focus. To maximize the energy throughput, the telescope consists of a multitude of these doublereflection mirrors arranged in a nested configuration. All mirrors operate at grazingincidence angles low enough to assure high reflectivity from the coating material at Xray wavelengths. A mirror based on the Wolter architecture is known to satisfy approximately Abbe's condition (Braat 1997; Abbe 1873), assuring limited coma aberration for moderate field of view. A variation of the Wolter telescope, the WolterSchwarzschild configuration (Chase & Speybroeck 1973; Wolter 1952a), exactly satisfies Abbe's condition. Other designs are possible (Zocchi & Vernani 2007; Giacconi et al. 1969) but they all share the doublereflection feature at very small grazingincidence angle.
Although a significant number of scientific publications have appeared in which the degradation of the performance of optical systems by scattering from surface roughness has been analyzed, the theoretical determination of the angular width of the scattered beam has received much less attention. The relation between the halfenergy width in grazingincidence telescopes and the roughness variance was studied in (Spiga 2007) by applying the DebyeWaller expression for the total integrated scattering (Spiller 1994) in 1dimensional geometry. In the framework of the scalar theory of diffraction (Gaskill 1978; Born & Wolf 1980; Goodman 1968; Harvey 1995b), an exact derivation of the rms width of the angle spread function from the corresponding optical transfer function (Harvey et al. 1988; Gaskill 1978; Born & Wolf 1980; Goodman 1968; Smith 1963) in 2dimensional geometry was reported in (Zocchi 2009), in which the contribution of scattering to the rms width of the angle spread function was shown to depend on only the variance of the roughness slope. However, even in these two papers (Spiga 2007; Zocchi 2009), the cylindrical symmetry of an Xray telescope was not taken into account.
In this work, the rms width of the angle spread function of grazingincidence optics with cylindrical symmetry is derived for arbitrary values of the roughness variance in the framework of the scalar theory of Fourier diffraction. In the following, we simply refer to the rms width of the angle spread function as the beam width. No further approximations are introduced into the derivation apart from the assumption that the angle between the axial profile of the optics and the optical axis is small. It is found again that the contribution of scattering to the width of the angle spread function depends only on the variance of the roughness slope. However, in the extreme case in which both the tapering angle of the optics and the grazingincidence angle are small, the proportionality factor between the roughness slope and the beam width is half of that found for the reflection on an almost flat surface.
When the small roughness approximation is valid, it is also shown that the angle spread function can be written in a standard form as the convolution of the angle spread function of a perfectly smooth optics with an effective power spectral density expressed by a line integral of the true power spectral density of surface roughness of the mirrors. Finally, for an isotropic powerlaw dependence of the power spectral density on the spatial frequency, the behavior of the beam width as a function of the radiation wavelength and the grazingincidence angle is also studied. If m is the exponent of the powerlaw power spectral density, the contribution of scattering to the beam width is proportional to .
The paper is organized as follows. Section 2 briefly reviews the standard approach used to derive the angle spread function of a rough mirror in the framework of Fourier optics within the small angle approximation, when the angle between the principal ray and any other rays in the optical system is small. This approximation limits the application to mirrors of low ratio of the diameter to the radius of curvature. The results and methods summarized in Sect. 2 are then used in Sect. 3 to derive the width of the angle spread function in grazingincidence optics with cylindrical symmetry. Finally, in Sect. 4 we derive an expression for the angle spread function when the small roughness approximation is valid. In this last section, the dependence of the beam width on the radiation wavelength and the grazingincidence angle is also studied for an isotropic surface characterized by a powerlaw expression for the power spectral density. The paper ends with two Appendixes. The first presents some mathematical derivations, and in the second we discuss the range of validity of Fourier optics treatment of scattering from surface roughness, and consequently of the content of this paper, and its relation to the small roughness approximation.
2 Angle spread function of rough optics
In this section, we briefly review the treatment of radiation scattering from surface roughness in the framework of the scalar theory of diffraction (Harvey et al. 1988; Gaskill 1978; Born & Wolf 1980; Goodman 1968; Smith 1963). In this theory, the optical transfer function
of the imaging system is given by the normalized autocorrelation of the generalized complex pupil function
in the exit pupil plane (Harvey 1995b; Stearns et al. 1998),
where is the wavelength of the electromagnetic radiation and where is assumed to be normalized to unit integral. Equation (1) also defines a function for later use. The description of the behavior of an optical system by Eq. (1) is valid if the pupil function can be considered independent of the position of the object point (Born & Wolf 1980). In the simplest case, is just the pupil function multiplied by the surface reflectance or transmittance but it may also include a phase factor describing the optical aberrations of the system. The effect of surface roughness can also be included in as a phase factor. When the radiation is incident on the reflecting surface at near normal incidence, the complex pupil function can be written as
where is the height of the surface roughness at position and is the complex pupil function of the optical system when roughness is neglected. When offnormal incidence is considered with a grazingincidence angle , Eq. (2) must be modified accordingly. Assuming the exit pupil plane to be normal to the principal ray, is also the angle between the normal to the pupil plane and the normal to the rough surface (Stearns et al. 1998). The height of surface roughness is projected onto the normal to the pupil plane by means of a factor . In addition, distances across the optical surface are also projected onto the pupil plane by a factor (Harvey 1995b; Stearns et al. 1998). Hence, Eq. (2) becomes
where r_{1} and r_{2} are the components of and where, for definiteness, the plane of incidence is assumed along the 1axis. The effect of roughness is obtained by substituting Eq. (3) into Eq. (1) and by averaging the result over the roughness height (Harvey 1995b; Stearns et al. 1998), to obtain
The final step consists in assuming that is a Gaussian stationary and ergodic stochastic process (Papoulis 1965) and in ignoring multiple scattering and shadowing effects (Harvey 1995b; Stearns et al. 1998). Without loss of generality, we can remove the average of and include it into the deterministic phase factor of . A standard calculation of multivariate Gaussian casual variables then gives (Papoulis 1965)
where is the covariance of surface roughness and is the corresponding variance. Because of the assumption that the stochastic process is stationary and ergodic, the righthand side of Eq. (5) is independent of . In addition, in the small angle approximation, when the angle between the principal ray and any other rays in the optical system is small, the angle can also be considered to be independent of (Harvey 1995b; Stearns et al. 1998). Hence, Eq. (5) can be taken out of the integral in Eq. (4) and the optical transfer function simplifies to
where is the optical transfer function of the system when roughness is or can be ignored. Before proceeding, we summarize the conditions under which Eq. (6) holds: a) the angle between any ray in the optical system and the principal ray is small; b) multiple scattering and shadowing effects can be ignored; c) the pupil function is independent of the position of the object point; d) surface roughness can be described by a stationary ergodic 2dimensional stochastic process.
Figure 1: Geometry of the grazingincidence optics with cylindrical symmetry: conceptual 3D drawing ( left) anf optics cross section ( right). 

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The inverse Fourier transform of the optical transfer function is the angle spread function (Harvey 1995b). When dealing with scattering phenomena, the use of the angle spread function is more convenient than the point spread function since the former is also applicable to large scattering angles (Harvey 1995a,b). In this formalism, the Fourier variable conjugate to the dimensionless frequency vector
appearing in Eq. (6) is the vector of direction cosines
of components
and
in the image plane. Because of the Fourier transform relation between the optical transfer function
and the angle spread function
,
the integral of the latter is normalized to unity,
The integration in the above equation should be performed in the domain but, in this case, the integral would no longer be equal to H(0). We, instead, assume that decreases sufficiently rapidly with for the integration to be extended over the entire plane of the direction cosines. The radiant intensity per unit solid angle is related to by (Harvey 1995b). Thus, the total radiant power is also normalized to unity,
where the first equality follows by taking into account the expression for the infinitesimal solid angle .
The width of the reflected and scattered beam can be defined to be the root mean square value of the scattering angle weighted by the angle spread function,
The full angular width of the beam is then . In the following, we simply refer to as the angular width of the beam. It is again assumed that the angle spread function decreases fast enough at high value of to extend the integration in Eq. (7) over the whole plane of the direction cosines. Because of the Fourier transform relation between the optical transfer function and the angle spread function, the integral in Eq. (7) can be expressed in terms of the value at the origin of the derivatives of . Since the inverse Fourier transform of is , the integral in Eq. (7) is
where is the 2dimensional Laplace operator. Inserting Eq. (8) into Eq. (7), we obtain
The righthand side of Eq. (9) can be calculated in terms of and the power spectral density of surface roughness by means of Eq. (6). The result, as reported in Zocchi (2009), is
where
are the variances of roughness slope along the direction of the incidence plane and normal to the incidence plane, respectively. In Eq. (10), is the rms beam width when roughness is ignored. Thus, only takes into account the effects of diffraction and aberrations in the optical surface. The power spectral density in Eqs. (11) and (12) is defined as the bilateral Fourier transform of the covariance .
3 Width of the angle spread function in Xray telescopes
The results presented in the previous section are valid for almost flat mirrors. The theory is now extended to the case of grazingincidence optics with cylindrical symmetry. We still assume the validity of the small angle approximation: in each plane containing the optical axis, the angle between any two rays reflected along a mirror profile is much smaller than the average grazingincidence angle.
The analysis is based on the geometry shown in Fig. 1. It is assumed that the grazingincidence optics consists of a mirror with just one reflection that can be approximated by a cone forming an angle with the optical axis. The extension to two or more reflections will be considered later. The rays reflected from the optics form a grazingincidence angle with the optical surface and are contained in planes through the optical axis. The exit pupil plane is perpendicular to the optical axis, which is also the axis of the cone. The largest radius R of the cone is projected onto the exit pupil plane as a circle of radius R_{0}. The position on the optical surface is defined by a coordinate z_{} along a profile of the cone and a coordinate along circles at the intersection of the optical surface with planes normal to the optical axis. In addition, we form the vector of components z_{} and . We use polar coordinates in the pupil plane: with a point in this plane identified by a position vector , we associate its modulus r and its anomaly . We finally assume that the pupil function has cylindrical symmetry and depends only on the modulus r of .
The relation
between the vector
on the optical surface and the vector
on the pupil plane is obtained by inspection of Fig. 1 as
The analysis is much simpler if we assume that the angle and the length L of the optics are such that . In this case, we can ignore the term dependent on z_{} in the second equation in Eq. (13), which simplifies to
where . The scaling factor of the roughness height is again and Eq. (4) reads
By assuming that the angle is small enough for the optical surface to be locally considered a cylinder, the average in Eq. (15) gives
where . The functional dependence of on and is determined from Eq. (14):
Equation (18) is valid when the anomaly of is higher than the anomaly of . Otherwise, a minus sign appears in front of Eq. (18). However, since the covariance is an even function of its arguments, we can ignore this change of sign.
An important conclusion can be derived from Eqs. (16)(18). Since the pupil function A_{0}(r) has cylindrical symmetry, the dependence of the integrand on the anomaly of the vector is expressed by the scalar product or, equivalently, by the function . By making the change of integration variable , we see that the optical transfer function depends only on the modulus f of the vector and, consequently, has cylindrical symmetry. We note that no assumptions have been made about the isotropy of the roughness covariance . Regardless of the angular dependence of , the optical transfer function and angle spread function inherit the cylindrical symmetry of the optics geometry.
A further observation can be made about the power spectral density of surface roughness. Since the covariance function is a periodic function of of period , the power spectral density is discrete in the conjugate variable . Only multiple values of are allowed. However, this has limited practical implications since at this spatial frequency the entire formalism in which roughness is considered to be a stationary stochastic process breaks down. The theory is only applicable at spatial frequencies much higher than .
According to Eq. (9), to calculate the width of the angle spread function, we must evaluate the value of the Laplacian of the optical transfer function with respect to
at the origin. This calculation is simplified by noting that the gradient
vanishes at the origin, as shown in Appendix A. By taking into account that
and
H_{0}(0)=1, it follows from Eq. (16) that
The first integral in Eq. (19) is simply and, by means of Eq. (9), is equal to , where is the angular width of the diffracted beam when scattering is ignored. The calculation of is reported in Appendix A, which gives
where actually means , etc. Since the pupil function has cylindrical symmetry and depends only on the modulus r of the vector , the second term in Eq. (20) vanishes after integration over because it is proportional to . The other two terms give a factor upon integration over and, consequently,
The second derivatives at the origin of can be related to the power spectral density of surface roughness. Since the Fourier transform of is equal to , we obtain
where and are the variances of roughness slope along the direction of the optical axis and along circles normal to the optical axis, respectively. Inserting Eqs. (22) and (23) back into Eq. (21) and then Eq. (21) into Eq. (19), we obtain
The first integral in Eq. (24), multiplied by , reduces to H_{0}(0)=1. To calculate the second integral in Eq. (24), we assume that the pupil function is constant and nonzero only for . Since A_{0}(r) has squared modulus normalized to unit integral, it is for and A_{0}(r)=0 elsewhere. Thus, we obtain
By combining Eqs. (9), (24), and (25), the width of the angle spread function becomes
where we have taken into account that . The total angular width of the reflected and scattered beam is then given by the quadratic sum of the beam width when surface roughness is ignored and a specific contribution due to roughness. Since we have assumed that , we also obtain . Consequently, we can approximate and . Thus, by defining g=R/R_{0}, Eq. (26) simplifies to
to first order in d_{0}/R_{0}. Equation (27) is independent of d_{0}. When both and are small, Eq. (27) simplifies further to
By comparison with Eq. (10), we note that the contribution of roughness to the width of the angle spread function is half that found for the reflection on an almost flat surface.
As an example, we determine the roughness contribution
to the rms beam width
in the case of a single reflection mirror with surface roughness described by the isotropic power spectral density
(Church 1988). If
is the half field of view, the cutoff spatial frequencies in Eqs. (22) and (23) are
along the direction of the optical axis and
along the curved orthogonal direction, respectively. Here we assume that
and
.
Equations (22) and (23) then imply that
where we applied the change of integration variable in the second equality and then integrated in polar coordinates. The last integral in Eq. (29) equals . Hence, from Eq. (28) we obtain that
For 1, 0.1, S_{0}=10^{2} , and 1.24, corresponding to photon energy of 1, Eq. (30) implies that 39 8.
The extension of Eq. (27) to multiple uncorrelated surfaces is straightforward since the integrand in Eq. (16) is simply multiplied by an exponential factor for each surface (Stearns et al. 1998). In the presence of N surfaces, each of roughness covariance
,
variance
,
slope variances
and
,
incidence angle
,
tapering angle
,
and scaling factor g_{k}, the optical transfer function becomes
and the beam width is now
4 Approximation of the angle spread function
Equation (16) defines the optical transfer function as a complicated integral of the pupil function and the roughness covariance. In this section, we first develop a simpler approximation of the optical transfer function that provides the same expression as Eq. (27) for the beam width . In the small roughness approximation, we also derive the angle spread function and express it in terms of an effective power spectral density obtained from the roughness power spectral density. Finally, the dependence of the rms beam width on the radiation wavelength and the grazingincidence angle is studied in more detail.
4.1 Approximate optical transfer function
To develop an approximation to the optical transfer function that provides the correct expression given by Eq. (27) for the beam width ,
we first note that we can approximate
,
since A_{0}(r) is nonzero only in a thin annulus between R_{0} and
R_{0}+d_{0}. In addition, the factor
is equal to
for f=0 and decreases with increasing f, becoming very small for
.
We thus assume that
is independent of
for
and is negligible for
.
We then write
where H_{0}(f) starts at 1 for f=0 and decreases to zero at . Thus, Eq. (16) can be simplified to
where we have performed the integration over r. Since and , then , and consequently we obtain, to first order in (see also Eqs. (A.4) and (A.5) in Appendix A),
Equation (31) then becomes
In the small roughness approximation, when , Eq. (32) further simplifies to
The optical transfer function is then written in a rather standard form (Harvey 1995b; Stearns et al. 1998) as the sum of a term describing the diffraction pattern when surface roughness is ignored and a term accounting for roughness scattering. It is easy to verify that the expression of the beam width calculated from Eqs. (32) or (33) is identical to Eq. (27).
4.2 Angle spread function and effective power spectral density
When the small roughness approximation is valid, the angle spread function can be expressed in terms of an effective power spectral density obtained from the roughness power spectral density. By taking the 2dimensional inverse Fourier transform of Eq. (33), we obtain
where * denotes convolution and where is the inverse Fourier transform
In the above equation, J_{0}(x) is the Bessel function of the first type of order zero (Watson 1966). In a sense, is an effective power spectral density that can be written in terms of the true power spectral density of surface roughness. The covariance in Eq. (34) corresponding to is
so that
By inserting Eq. (35) into Eq. (34), we obtain
Finally, by taking into account the identity (Watson 1966)
and by using polar coordinates for , Eq. (36) becomes
Thus, the effective power spectral density is given by the line integral of the roughness power spectral density along the ellipse of halfaxes in the direction of the optical axis and along the curved orthogonal direction.
4.3 Dependence of the beam width on the radiation wavelength
To investigate the dependence of the scattered beam width on the radiation wavelength, we first note that depends linearly on . Since , where is the normalized autocorrelation of the complex pupil function defined by Eq. (1), and since is independent of , Eq. (9) implies that is proportional to the wavelength. The dependence of and on is more difficult to analyze and is related to the extreme spatial frequencies of surface roughness contributing to scattering. In the small roughness approximation, the angle spread function depends linearly on the effective power spectral density , evaluated at . In this case, the effective power spectral density is understood to be cutoff at both high and low spatial frequencies. The absolute maximum occurs at , when . The corresponding cutoffs of the power spectral density are at along the direction of the optical axis and along the curved orthogonal direction. The integration domain is an ellipse with shortaxis and longaxis .
As an example, we consider an isotropic powerlaw dependence of the roughness power spectral density on the spatial frequency,
(Church 1988). The integrals in Eqs. (22) and (23) then give, assuming ,
,
and m<4,
where we have used polar coordinates after the substitution . By making the change of integration variable , the last integral in Eq. (37) becomes
where is the last integral in Eq. (38) and is a slow varying function of . For m=1 and , the integral is approximately equal to . For , we can ignore the term in Eq. (38) and then . This value is exact for m=2 and m=4. Inserting Eqs. (37) and (38) back into Eq. (28) gives
The scattering contribution is suppressed by a factor and is proportional to . Since we can assume that normally 1<m<3, this contribution is a decreasing function of the wavelength. Taking into account that is proportional to the wavelength, Eq. (39) can be written as
where is a constant independent of the wavelength that depends only on the roughness power spectral density and the ratio of the beam width when roughness is ignored to the radiation wavelength . By means of Eq. (40), it is possible to study the dependence of the beam width on the radiation wavelength and the grazingincidence angle. The use of the normalized quantities and simplifies the study and the graphical representation of the scaling property of with respect to .
Equation (40) is now studied in more detail for a grazingincidence mirror with one and two reflections, respectively. For a mirror with a single reflection and an object at infinity,
,
where
is the angle of the principal ray at the focal plane with respect to the optical axis. Assuming that
is small, Eq. (40) gives
The ratio is plotted in Fig. 2 as a function of for a few values of m when 1. In a type I Wolter mirror for Xray astronomy, instead, there are two reflections, for which . In this case, Eq. (40) is extended to
where again is assumed to be small in the second equality. There is a reduction by a factor 2^{(3m)/2} in the scattering contribution to the beam width between Eqs. (41) and (42). The function given by Eq. (42), again for 1, is shown in Fig. 3.
Figure 2: Normalized beam width as a function of the normalized wavelength for a single reflection optics with 1 and a power law expression of the roughness power spectral density. m is the exponent of the power law. 

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Figure 3: Normalized beam width as a function of the normalized wavelength for a two reflections optics with 1 and a power law expression of the roughness power spectral density. m is the exponent of the power law. 

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5 Conclusions
In the framework of the scalar theory of Fourier diffraction, we have derived the width of the angle spread function of a grazingincidence optical system with cylindrical symmetry in the presence of roughness scattering. The derivation does not introduce further approximations in the theory except for assuming that the angle between the axial profile of the optics and the optical axis is small. Consequently, the results presented in this paper are more relevant to Xray astronomy than other applications, such as EUV microlithography, that also use grazingincidence mirrors with cylindrical symmetry but are characterized by quite large angles between the mirror profile and the optical axis.
When the small roughness approximation is applicable, the angle spread function itself can be expressed in a standard form as the convolution of the angle spread function of a perfectly smooth optics with an effective power spectral density related to the true power spectral density of surface roughness by line integration along an ellipse. This approximate expression for the angle spread function provides the correct expression for the width of the reflected and scattered beam and can be used for more accurate analyses of the scattering effects in Xray telescopes. For example, it can be used to determine the encircled energy in the focal plane as a function of the encircling angular diameter.
Appendix A: Calculation of
We first show that the gradient of
vanishes at the origin. We work in polar coordinates for ,
a vector of modulus f and anomaly
.
Since the optical transfer function, Eq. (16), has cylindrical symmetry and thus is independent of
,
we can simply ignore
and just set
.
The gradient of
is given by
where and where summation over is assumed. Equation (A.1) must be evaluated at f=0,
where means . These partial derivatives, actually the components of the gradient of , vanish at the origin. If is regular at the origin, this is simply because has its maximum at the origin. If, instead, has discontinuous derivatives at the origin, the quantity must be understood to be the average of as . Since is an even function of , it follows again that vanishes. To see that this is the correct interpretation, we note that the Fourier transform of is , where is the power spectral density of surface roughness. Hence, the value at the origin of is
Since is an even function of , the integral in the last equation vanishes as expected.
We next calculate the Laplacian of
at the origin, again ignoring
.
Using Eq. (A.1), we find that
When we evaluate the above expression at the origin, the first two terms in the second line vanish because of the above argument about the value of the gradient of at the origin, and consequently
To calculate the righthand side of Eq. (A.3), we use Eqs. (17) and (18) and we obtain
Evaluating these expressions at f=0 gives
When Eqs. (A.4) and (A.5) are inserted back into Eq. (A.3), we obtain
which is Eq. (20) in the text.
Appendix B: Validity of the shadowing effects approximation
Figure B.1: Limit of validity of the multiple scattering and shadowing effects approximation (solid trace) and of the small roughness approximation (dashed trace). A relaxed limit of validity of the approximation is also plotted (dotted trace). 

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The theory that leads to Eq. (6) and on which the present paper is based, requires, to remain valid, some assumptions about the properties of the optical system under consideration and the statistical properties of surface roughness. These assumptions, which are listed in Sect. 2, include the requirement that multiple reflections and shadowing effects can be ignored. In this Appendix, some considerations are discussed about the range of validity of this assumption and its relation to the small roughness approximation.
We can assume that multiple reflections and shadowing effects can be neglected if the grazingincidence angle
is larger than the rms slope error
in the direction of the optical axis, or
Since is given by Eq. (22), it follows that
where . Hence, Eq. (B.1) becomes , or
The limiting curve is plotted in Fig. B.1 as a function of the normalized surface roughness / (solid trace). Inequality (B.3) is valid above the curve. In the figure, the limiting curve for the validity of the small roughness approximation is also plotted (dashed trace). This is derived from the condition by assuming the equation to be the limiting boundary. The small roughness approximation is valid below the dashed curve. The intersection of the two curves occurs at / and 50.
It must be remarked that the above discussion is not limited to the analysis of the validity of the results presented in this paper but is applicable to the entire theory of the Fourier optics treatment of scattering from rough surfaces. Below , the theory is always applicable, irrespective of the value of the incident angle. Above / , instead, the grazingincidence angle above which the theory is valid increases rapidly with /. In particular, for grazingincidence optics, the theory is not applicable even if the small roughness approximation holds. However, condition (B.3) is quite pessimistic because of the inequality sign in Eq. (B.2). Condition (B.3) also follows from Eq. (B.1) in the case of a single sinusoidal wave with rms value and spatial frequency /. If a less restricting value of is used in Eq. (B.2), the limiting curve for the application of the theory shifts to higher values of the ratio /. As an example, the curve obtained by substituting with into Eq. (B.2) is also plotted in Fig. B.1 (dotted trace).
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All Figures
Figure 1: Geometry of the grazingincidence optics with cylindrical symmetry: conceptual 3D drawing ( left) anf optics cross section ( right). 

Open with DEXTER  
In the text 
Figure 2: Normalized beam width as a function of the normalized wavelength for a single reflection optics with 1 and a power law expression of the roughness power spectral density. m is the exponent of the power law. 

Open with DEXTER  
In the text 
Figure 3: Normalized beam width as a function of the normalized wavelength for a two reflections optics with 1 and a power law expression of the roughness power spectral density. m is the exponent of the power law. 

Open with DEXTER  
In the text 
Figure B.1: Limit of validity of the multiple scattering and shadowing effects approximation (solid trace) and of the small roughness approximation (dashed trace). A relaxed limit of validity of the approximation is also plotted (dotted trace). 

Open with DEXTER  
In the text 
Copyright ESO 2009
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