Issue 
A&A
Volume 505, Number 1, October I 2009



Page(s)  373  384  
Section  Astronomical instrumentation  
DOI  https://doi.org/10.1051/00046361/200912668  
Published online  28 July 2009 
Analytical computation of the offaxis effective area of grazing incidence Xray mirrors
D. Spiga  V. Cotroneo  S. Basso  P. Conconi
INAF  Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807, Merate (LC), Italy
Received 9 June 2009 / Accepted 20 June 2009
Abstract
Aims. Focusing mirrors for Xray telescopes in grazing incidence, introduced in the 70s, are characterized in terms of their performance by their imaging quality and effective area, which in turn determines their sensitivity. Even though the onaxis effective area is assumed in general to characterize the collecting power of an Xray optic, the telescope capability of imaging extended Xray sources is also determined by the variation in its effective area with the offaxis angle. The effective area, in general, decreases as the Xray source moves offaxis, causing a loss of sensitivity in the peripheral regions of the telescope's field of view.
Methods. The complex task of designing optics for future Xray telescopes entails detailed computations of both imaging quality and effective area on and offaxis. Because of their apparent complexity, both aspects have been, so far, treated by using raytracing routines aimed at simulating the interaction of Xray photons with the reflecting surfaces of a given focusing system. Although this approach has been widely exploited and proven to be effective, it would also be attractive to regard the same problem from an analytical viewpoint, to assess an optical design of an Xray optical module with a simpler calculation than a raytracing routine. This would also improve the efficiency of optimization tasks when designing the Xray optical modules. In this paper, we thereby focused on developing analytical solutions to compute the offaxis effective area of doublereflection Xray mirrors.
Results. We have developed useful analytical formulae for the offaxis effective area of a doublereflection mirror in the double cone approximation, requiring only an integration and the standard routines to calculate the Xray coating reflectivity for a given incidence angle. The computation is easily applicable also to WolterI mirrors (such as those of NeXT, NuSTAR, HEXITSAT, IXO) and the approximation improves as the fnumber of the mirror increases. Algebraic expressions are provided for the mirror geometric area, as a function of the offaxis angle. Finally, the results of the analytical computations presented here are validated by comparison with the corresponding predictions of a raytracing code.
Key words: telescopes  methods: analytical  space vehicles: instruments  Xrays: general
1 Introduction
Xray telescopes have been equipped with focusing optics since the 70s to endow them with imaging capabilities and concentration properties that enhance their sensitivity. The effective area of the optics is one of the most important parameter determining the minimum detectable flux: to date, the Xray telescope with the largest effective area in the soft Xray band (<10 keV) is NewtonXMM with 1450 cm^{2} per module at 1 keV, onaxis (Gondoin et al. 1998b). Beyond 10 keV, the effective area and the sensitivity of all focusing Xray telescopes drop off suddenly, because of the very low reflectivity of singlelayer coated mirrors at the grazing incidence angles in use. The situation is expected to change with the launch of imaging hard (>10 keV) Xray telescopes such as NuSTAR (Koglin et al. 2005), NeXT (Takahashi et al. 2008; Ogasaka et al. 2008), HEXITSAT (Pareschi 2004), and IXO (formerly XEUS, Parmar et al. 2004; Kunieda et al. 2008) that will extend the performances of presentlyoperating Xray telescopes beyond 10 keV, by means of shallow incidence angles (<0.25 deg) and wideband multilayer coatings (Joensen et al. 1995; Tawara et al. 1998).
On the other side, the study of extended Xray sources, such as galaxy clusters, and even cosmological surveys would benefit greatly from an increase in the field of view of Xray telescopes. For example, eROSITA (Predehl et al. 2006) will provide a wide field of view of 61 arcmin in diameter (Friedrich et al. 2008) by using double reflection mirrors. Previous mission concepts, such as WFXT (Citterio et al. 1993) and WFI onboard EDGE (Piro et al. 2008), have been proposed to increase the imaging quality of offaxis sources, by adopting polynomial profiles (Burrows et al. 1992; Conconi & Campana 2001). This type of mirror design provides a higher resolution for offaxis Xray sources than the Wolter's, at the expense of a small degradation of the HEW onaxis.
Nevertheless, not only the angular resolution, but also the effective area of grazingincidence Xray mirrors is known to be degraded as a source moves offaxis, due to geometrical vignetting and the variation in the incidence angles on mirrors. This can have important consequences for the observation, since the sensitivity of the telescope over its field of view can be severely compromised. Moreover, for telescopes with modules flying in formation (as was to have been the case for SIMBOLX, Pareschi et al. 2008), oscillations at random of the optical module might cause an unpredictable decrease in the effective area. Possible solutions to this problem have been studied (Cotroneo et al. 2009), although this example highlights the importance of the theoretical prediction of the effective area, on and offaxis, already at the design stage of the optical module development for an Xray telescope.
Another situation in which the theoretical computation of the effective area is necessary occurs whenever Xray mirrors are calibrated using onground facilities such as PANTER (Brauninger et al. 2004; Freyberg et al. 2006), where the Xray source is located at a large, but definitely nonastronomical, distance from the mirror. In such conditions, the measured effective area is affected by the imperfect collimation of the incident beam: the correct data interpretation must account for this effect (see e.g., Gondoin et al. 1998b), on and offaxis, to reliably reconstruct the mirror's effective area for an astronomical Xray source over all the field of view of the telescope.
While the prediction of the onaxis effective area for a doublereflection, grazingincidence mirror is rather simple, it becomes difficult in general for a source offaxis. Such evaluations have been completed so far using raytracing codes (see e.g., Mangus & Underwood 1969; Zhao et al. 2004), starting from the optical design of mirrors and the structure of the reflective coating. These codes are in general very efficient, but timeconsuming, computationally intensive, and affected by statistical errors related to the number of rays that can be traced. It would therefore be beneficial to develop a method for computing the effective area analytically, which would ease the assessment of the effective area and, among other things, the optical design of a wide field Xray telescope.
Few suitable analytical tools have been developed to date. Van Speybroeck and Chase (1972) found  by means of raytracing  that the geometric, collecting area of a WolterI mirror decreases with the offaxis angle
of the source, with respect to the onaxis geometric area
,
according to
where is the incidence angle for a source onaxis. However, we lack a general, analytical method to derive the effective area of an Xray mirror with a given reflective coating, as a function of the offaxis angle of the Xray source.
In this paper, we present a solution to that problem. We develop an analytical approach that can be applied to double cone grazingincidence Xray mirrors and, with reasonable accuracy, to WolterI mirrors (unless the fnumber is small). The limits of this approximation are discussed in Sect. 2. In Sect. 3, we derive general integral formulae (such as Eq. (25)) to compute the offaxis effective area for a doublereflection Xray mirror with shallow incident angles, for any reflective coating. As a particular case, in Sect. 4 we obtain some algebraic expressions for the geometric area and verify that the wellknown Eq. (1) can be derived as a particular case. In Sect. 5, the predictions of the analytical approach are validated, for some particular cases, by means of a comparison with the outputs of a raytracing routine. The results are briefly discussed in Sect. 6.
We note that we assume that the offaxis mutual obstruction of mirrors in densely nested mirror assemblies has a negligible effect. Therefore, the results are valid for either isolated double cone or WolterI mirrors, or for mirror modules known to be negligibly obstructed, such that their effective area simply equals the sum of the contributions of the individual mirrors. The quantification of the offaxis obstruction in mirror assemblies will be considered in future.
2 The double cone approximation in the computation of the effective area of a WolterI mirror
We consider, in a preliminary way, a grazingincidence WolterI mirror, and an onaxis photon source (Fig. 1). The optical axis is aligned with the z axis. We define to be the radius at the parabolic end (i.e., the maximum radius), R_{0} the radius at z=0 (the intersection plane), the radius at the hyperbolic end (i.e., the minimum radius), F the focal point, and f the distance of F from the intersection plane (i.e., the focal distance). In general, we refer to ``primary'' and ``secondary" segments, instead of ``parabola" and ``hyperbola". We denote with L_{1} the primary segment length along the z axis, and L_{2} that of the secondary. The polar coordinate is .
Because of the surface curvature, the incidence angles on the two surfaces vary in general with the z coordinate. We define
to be this angle on the primary (0<z<L_{1}) mirror segment, and on the secondary (L_{2}<z<0) mirror for a source on the optical axis, at infinite distance. In general (Van Speybroeck & Chase 1972), the incidence angle of rays close to z = 0, ,
is the same for both surfaces. Therefore, we have the wellknown relation
Since is shallow, we hereafter assume that the function can be approximated by itself.
Figure 1: Meridional section of a WolterI mirror, here in the case : a) source onaxis, at astronomical distance; b) source still onaxis, but located at finite distance (all angles are greatly exaggerated). 

Open with DEXTER 
To obtain an analytical expression for the effective area of a WolterI mirror when a source is offaxis by an angle , we have to find algebraic expressions for:
 1.
 the variation in the incidence angles, on which the mirror reflectivities depend, over the primary and secondary mirror segment surfaces;
 2.
 the collecting area of the primary segment;
 3.
 the fraction of rays reflected by the primary segment that are incident on the secondary.
In the remainder of this section, we quantify the errors caused by the substitution of a WolterI profile with a double cone, by keeping R_{0}, ,
L_{1}, and L_{2} constant. The problems to be faced are related to the system geometry, rather than to the absolute size of the mirrors. Hence, it is convenient to report the results of this section in terms of both the fnumber,
,
instead of f itself, and
L_{1}' = L_{1}/(2R_{0}),
L_{2}' = L_{2}/(2R_{0}), which are normalized mirror lengths. Using Eq. (2),
can be written as
We mention that the true focal length of a double cone is slightly longer than that of a Wolter profile with the same R_{0} and , because of the different focusing properties. In all cases, we always refer to f as the focal length of the corresponding WolterI mirror, to ensure that Eq. (2) retains its validity.
2.1 The incidence angles
For a double cone profile, the incidence angles for an onaxis source at infinity are constant along a meridional plane, and equal to . For a WolterI profile, the slope of the mirror profile changes slowly with the z coordinate. Because of the concavity of profiles, on the primary segment, and on the secondary segment. We assume for simplicity that L_{1}=L_{2}=L, and define the (positive) angle variations and . For a WolterI profile, the ratio varies between 1 and 2, going from large to short . For this estimation, we assume that and we simply denote their value with .
Now consider a ray from an onaxis source at infinity (Fig. 1a). After being reflected firstly at z = +L, it undergoes the second reflection at
,
at a radial coordinate ,
and is focused at z = f. The total photon deflection at z =L is
;
therefore,
For small we also have that
(5) 
By comparing the last two equations, using Eqs. (2) and (3), with the definition of L_{1}' = L_{2}' = L', we derive the maximum variation in the incidence angles over the mirror profiles,
This equation provides the error in the incidence angles introduced by the double cone approximation. Such an error is computed for some practical cases and reported in Table 1. For example, we note that for NeXTHXT and SIMBOLX the error is only 0.4%. This means that, assuming deg at most, the angular variation along the profile is 4 arcsec, which has almost no practical influence on the reflectivity of wideband multilayers.
Figure 2: Percent accuracy of the primary segment crosssection area, as seen by a source onaxis from infinity, in approximating a WolterI profile with a double cone. 

Open with DEXTER 
Table 1: Some examples of approximation introduced by the double cone geometry.
We now consider the source onaxis at finite distance, with . For a double cone (Fig. 1b), the incidence angle on the primary segment becomes , for all . Similarly, the incidence angle on the secondary segment is also constant and equal to , provided that . Within the approximation of Eq. (6), this is also true for a WolterI mirror.
2.2 The maximum diameter
In terms of effective area, another concern of approximating a WolterI profile with a double cone of the same R_{0}, , L_{1}, and L_{2}, is the different crosssection of the primary segment. For a double cone profile, the maximum diameter is . For a WolterI mirror, because of the profile concavity, the maximum diameter is smaller by an amount that depends on L' and . Consequently, the geometric area of the primary segment is smaller for a Wolter profile than for a double cone with the same size and . However, the (negative) error caused by the substitution of a WolterI profile with a double cone, defined asis, in general, of a few percent as far as L' < 1 (see Fig. 2). In addition, its magnitude decreases rapidly for increasing , since it is expressed well by the empirical formula
of the same order of magnitude as the expression in Eq. (6). This approximation is also computed for some telescopes and reported in Table 1.
For an onaxis source at a finite distance, the area of the circular corona between and should be considered: the area is thereby increased by the same term 2 , for both Wolter and double cone. Hence, the approximation of the area is even better than the expression in Eq. (8).
2.3 Geometric vignetting for double reflection
We now consider the third problem. The case of a source onaxis, at a finite distance, represents the simplest case in which there is geometrical vignetting for double reflection. If the source is onaxis, at infinite distance (with ), all rays undergo two reflections and reach the focus of the mirror. If the distance is finite, not all photons reflected by the primary segment also hit the secondary: for instance, photons reflected at can miss being reflected by the secondary, so they are prevented from being focused, as depicted in Fig. 1. We can quantify this geometric effect by means of the vignetting factor V, which is defined to be the ratio of the number of photons reflected twice to the number of photons reflected by the primary segment (assuming, ideally, that the mirror reflectivity is 1). In this configuration, if the mirror profile is a double cone, we can compute V using the simple formula (see Appendix A for a derivation)valid if , otherwise V =1. If either or , then V =0. In Sect. 3, we see that this result can even be generalized to the case of a source offaxis.
If we consider that in this case
and
,
an alternative expression for Eq. (9) is
where we have used the definitions of and . Using Eq. (3) and normalizing the L's to the mirror diameter, we can also write Eq. (9) as
It is interesting to note that a formula similar to Eq. (10) for the effective area was empirically found by Van Speybroeck & Chase (1972), but with a 2.5f term instead of 4f.
Rigorously, Eqs. (9) to (11) hold only for a double cone mirror, but they are expected to be applicable also to WolterI mirrors of a sufficiently large . To determine the approximation that can be achieved, we computed by raytracing the exact V factor of a WolterI mirror as a function of , in the case of L'_{1} = L'_{2} = 0.5, for fixed values. In Fig. 3, the results are compared with the findings of Eq. (11). The vignetting for the double cone is independent of L', whereas for the Wolter's it depends markedly on L' only for small .
Inspection of Fig. 3 shows that
 for a fixed and not too large , V is larger for a WolterI mirror than for the corresponding double cone; therefore, the double cone approximation returns, in general, pessimistic predictions of the effective area;
 in double cone approximation, V<1 for all , i.e., there are always lost photons for double reflection. With a WolterI profile, V is 1 when becomes sufficiently small;
 for a fixed , the predictions of Eq. (9) approach the exact calculations as is increased. For large and large , where , the V factor of Wolter becomes slightly smaller than that of the double cone.
Figure 3: Vignetting due to the finite distance of the source onaxis, as a function of the fnumber, for L'_{1} = L'_{2} and 4 different values of . Solid lines are computed assuming a WolterI profile, dashed lines a double cone (Eq. (11)). The results for the double cone are completely independent of the choice of L': those for the WolterI are computed assuming L' = 0.5. 

Open with DEXTER 
Figure 4: Percent accuracy of the double cone approximation in the estimation of the vignetting factor for a source onaxis at finite distance, as derived from the curves of Fig. 3 (symbols). Lines are traced using the empirical Eq. (12) with L' = 0.5. 

Open with DEXTER 
From the curves of Fig. 3, we computed
,
the error in the vignetting factor when we apply Eq. (9) to a WolterI profile, as in the definition of Eq. (8). This quantity is plotted in Fig. 4 for the case L' = 0.5. It can be seen that, in the cases interesting for us, i.e., for sufficiently large
and not too large values of ,
is positive and of the order of a few percent. We repeated this exercise for several values of L' in the interval 0.251 to investigate the dependence of
on this parameter, and it turned out that this ratio, if positive and if
,
can be approximated very well by the empirical formula (see Fig. 4 and Table 1)
where is with very good approximation a constant in the explored range of L' values. This equation has the same kind of dependence as Eq. (6) for the slope variation along the profile of the mirror and Eq. (8) for the area of the primary segment.
For small values, Eq. (12) is not obeyed because of the saturation of V(Wolter) to 1, so the expression of should be interpreted as an upper limit. Finally, for very large the error deviates from Eq. (12) as it becomes negative, but this occurs only when , so its weight in determining the effective area is expected to be negligible.
We can therefore conclude that the error introduced by the double cone approximation, regarding the effective area, is definitively smaller than . In other words, the double cone approximation is valid when , a condition fulfilled in almost all practical cases. Within the limits of this approximation, we derive in the next section the effective area for a source on and offaxis.
3 The on and offaxis effective area of a WolterI mirror
3.1 Onaxis source
We assume that we can approximate the WolterI profile with a double cone profile, by adopting the tolerances estimated in Sect. 2. In the following, we adopt the convention to denote with the effective area of the mirror at the photon wavelength , for a source offaxis by , at a distance D (finite or infinite). When referring to the geometric area, we omit and use the notation . Firstly, we assume L_{1} = L_{2} = L. The geometrical, collecting area of the primary segment, as seen by a source onaxis at ``infinite" (i.e., astronomical) distance iswhere we use the approximation . In this case, all reflected rays also undergo an identical reflection on the secondary segment (Fig. 1), therefore . We now denote by the reflectivity of the mirror at the photon wavelength , for a generic incidence angle . The form of this function depends on the coating structure: for a single layer coating, which operates in total external reflection, it slowly decreases up to the critical angle for , followed by a sudden cutoff. If a multilayer coating is used, is a more complicated function and can be computed using one of the standard methods (e.g., Parrat 1954; Abelès 1950), by also including the effect of roughness using, e.g., the NévotCroce (1980) approach.
Since photons are reflected twice at the same angle ,
we multiply the geometrical area by the squared reflectivity to obtain the effective area at the photon wavelength
This is a well known result. We now keep the source onaxis, but at a finite distance D and assume more generally that (with L_{1} = L_{2} as a particular case). As already discussed in Sect. 2, all mirror sectors see the source offaxis by the same angle . The effective area of the primary segment thereby becomes
where . The effective area for a source at finite distance is then obtained from Eq. (15), times the vignetting factor of Eq. (9), times , the reflectivity of the secondary mirror segment,
where . If V<1, substitution of Eq. (9) yields
As one might expect, the geometric area is that of the secondary segment, projected onto the wavefront after the primary reflection. We note that by setting we retrieve the onaxis result, in Eq. (14). On the other hand, if , all the primary segment is effective in the double reflection, so V =1. This may occur with a divergent source onaxis, if . In the absence of a geometrical vignetting, the effective area becomes
Comparison of Eqs. (17) and (18) indicates that the effective area can be written as
which represents the general expression for the effective area seen by a source onaxis.
3.2 Offaxis source: integral formula
We can now compute the effective area for a source offaxis. Because of the axial symmetry of the mirror, we choose the x axis so that the source lies in the xz plane, on the side of the positive x axis (refer to Fig. 5). We define to be the angle between z and the source direction.With respect to the onaxis case, there are some additional difficulties. The ray no longer lies within a meridional plane of the mirror, so the polar angles of the impact positions on the primary and secondary mirror segment, and , differ in general, and the incidence angles and also vary with them.
Nevertheless, since the maximum distance of the two impact points is , the offplane linear displacement is at most: therefore, , which is in general negligible with respect to and themselves. This result can also be derived more rigorously (see Appendix B).
Figure 5: A grazingincidence double cone mirror, illuminated by an offaxis source: the dashed line is a ray path. The optical axis lies along the z direction and the x axis is chosen for the source S, at a distance , to lie in the xz plane. The source direction forms an angle with the z axis. The azimuthal positions of the reflection points are located along with the and polar angles. 

Open with DEXTER 
In the limit of small , we can henceforth assume with good approximation : for this reason, in the remainder of this section we denote with the nearlycommon value of the two angles. In Appendix B, we also derived other important results:
 1.
 analytical expressions for
and
can be found with some algebra. For a small angle ,
these functions reduce to the simple expressions
which generalize the expressions for the incidence angles of Sect. 3.1, to the case of an offaxis source;  2.
 always in the limit of small ,
,
,
the vignetting for double reflection (Sect. 2.3) can be calculated using a generalization of Eq. (9),
Here the V factor varies with because it depends on (Eq. (20)) and (Eq. (21)). As in Eq. (9), Eq. (22) is valid only if . If V exceeds 1 at some , then all the primary segment sector is effective and . If either or is negative at some , no reflection occurs on the optical side of the mirror and .
We now draw our attention to a small mirror sector between
and
,
when
.
Equations (20) and (21) can then be used to compute the local incidence angles, and Eq. (22) to compute the local vignetting factor. We assume, initially, that
and
;
therefore V>0. If
,
we can repeat the passages in Sect. 3.1 for a mirror sector at
according to Eqs. (17). Otherwise
,
all the primary segment sector is effective, so we can write the sector area according to Eq. (18). Finally, we obtain for the effective area of the infinitesimal sector,
where . In Eq. (23), we omitted the explicit dependence of and on : in the following, we adopt the same convention to simplify the notation.
The expression for
is correct as long as the incidence angles are nonnegative. If either
or
become negative at some ,
no contribution to the effective area can be given by that sector, so
is zero at that .
We can then write without restrictions that
The effective area of the entire mirror is then given by integration over
where the factor of 2 comes from the symmetry of the mirror with respect to the offaxis plane. In the particular case L_{1} = L_{2}, Eq. (25) becomes
where if positive, and zero otherwise. Using Eqs. (20) and (21), we can conveniently write in the compact form
which is valid also for . Finally, for a source at infinity there is additional symmetry with respect to the y axis, and, if , we can write Eq. (26) in an even simpler form,
4 Applications to the geometric area
An upper limit to the effective area is represented by the geometric area, , obtained by simply setting the mirror reflectivity to 1, for all and . In the most common case, L_{1} = L_{2}, the expression of the geometric area iswhere is given by Eq. (27). In this section we solve this integral explicitly and provide analytical expressions for .
4.1 Source at infinity
For a source at infinity with , it is more convenient to use Eq. (28) withwhich can be immediately solved
Recalling Eq. (14) for the onaxis area , we obtain
which is exactly Eq. (1) found by Van Speybroeck and Chase (1972), after approximating .
For offaxis angles larger than ,
Eq. (32) is no longer valid. An extension of the curve
for
can be obtained from Eq. (30), after setting the integrand to 0 when
,
according to Eq. (27). The result is a nonlinear function of the
ratio,
which is identical to Eq. (32) for ; this is correct because the geometrical vignetting must be a continuous function of . We note that, for sufficiently large , Eq. (33) can be approximated well by .
A complete vignetting curve for is shown in Fig. 6 (solid line). The predicted deviation from linearity is verified in Sect. 5 by means of an accurate raytracing routine.
4.2 Source at finite distance
We now consider the variation in the geometric area, for a source at a finite distance (). In this case, the integration depends on whether or not.
We consider firstly the case
.
We then assume initially
.
With these conditions,
for all ,
therefore Eq. (27) becomes
Substituting this expression into Eq. (29) and solving, we derive the area
that is, (see Eq. (17)). In other words, the mirror geometric area is constant as far as . This is often observed in optics calibrations at onground facilities (see, e.g., Gondoin et al. 1998b).
We now increase
beyond .
Since
by hypothesis, we can consider the case
.
We are therefore allowed to write Eq. (29) as
where the integrands are always positive. This yields
We note that for , Eq. (37) reduces to Eq. (32), and for to Eq. (35), as expected.
We now suppose
.
In this case, the integration returns some more terms
This equation, as expected, returns the same result as Eq. (37) at , and is valid for offaxis angles in the interval . Therefore, for it reduces to Eq. (32) and (33) for the single point .
Figure 6: Normalized geometric area, , for a double cone mirror with a deg, as a function of the offaxis angle, for different angles due to the finite distance of the source. The curves are traced using the analytical formulae reported in Sect. 4. 

Open with DEXTER 
Now, consider the case
,
unlike we have hitherto assumed, but still that
.
This time
:
the condition
is insufficient for avoiding negative values of
in Eq. (34), therefore Eq. (35) is valid only if
.
Beyond this limit and up to
,
Eq. (37) should be replaced by
which, unexpectedly, is an increasing function of in the interval . When , the geometric area again follows Eq. (38), which for exhibits a maximum at
such a maximum is not present if .
In a similar fashion, one can easily compute the total geometric vignetting for , even if the resulting expression would be too long to report here, and it is also possible to derive similar expressions for the unusual case . To provide the reader with a qualitative visualization of the overall trend of the expressions we just derived, we traced in Fig. 6 some curves of total vignetting as a function of , for deg and different values of . To do this, we used Eqs. (32) and (33) and Eqs. (35) to (39) in the respective intervals of validity, and also the expression for , which is not reported here.
To summarize the results presented in this section, from Fig. 6 we can draw some conclusions:
 if , the geometric area decreases linearly up to , then approaches zero as is increased beyond ;
 if , the geometric area remains constant for , then decreases monotonically to zero;
 if , the geometric area remains constant for , then increases, reaches a maximum and eventually decreases to zero;
 if , the geometric area is zero for , then increases, reaches a maximum and eventually decreases to zero.
5 Validation with raytracing results
We verify the formulae derived in previous sections by means of a comparison with the results of a raytracing routine. To make the comparison easier, we consider the case of a single WolterI mirror. A first point to be checked is the geometric area, which was extensively analyzed from the analytical viewpoint in Sect. 4. In particular, the curves of Fig. 6 are easily verifiable along with a raytracing routine, without any assumptions about the reflective coating. The comparison is interesting especially when testing the analytical formulae in the nonlinear regions, which are usually not exploited in Xray optics.We displayed in Fig. 7 the comparison between 3 representative analytical curves of normalized geometric area (from Fig. 6) and the findings of a raytracing run on a WolterI mirror with the same value of (0.2 deg), corresponding to . For the raytracing simulation, we adopted the reasonable value L' = 0.5, whereas the analytical curves are largely independent of this parameter, as long as the double cone approximation is applicable. More exactly, from the discussion of Sect. 2 the approximation that we introduce is not larger than . As can be noted, the agreement between the two methods is complete, also for large offaxis angles where the vignetting ceases to be linear, and even for . On the other hand, the analytical computation, with a nearlycontinuous sampling, corresponded to a few lines of IDL code, whilst the raytracing routine is a complex program, which requires the acquisition of more than 10^{4} photons to reach a statistical error of a few percent for each point.
Figure 7: Comparison between some analytical curves of Fig. 6 (lines), and the results of an accurate raytracing (symbols) for a WolterI mirror with the same (0.2 deg) and L' = 0.5. To avoid confusion in the figure, not all curves were represented. Note the very good matching of the two methods, within the error bars of the raytracing. 

Open with DEXTER 
Figure 8: Comparison of effective areas of the largest WolterI mirror of NewtonXMM, as computed from raytracing (symbols) and from Eq. (26) (lines). The source is supposed to be at infinity (). The agreement is very good to within a few percent. 

Open with DEXTER 
We now wish to compare the predictions of Eq. (26) for the effective area, as a function of the photon energy, with the results of the raytracing. As a first case, we check the results for the largest mirror shell of a NewtonXMM optical module (Gondoin et al. 1998b), with f = 7.5 m, R_{0} = 346.2 mm ( = 0.66 deg), and L = 300 mm. The errors in the primary mirror segment area and the incidence angle variation along the profile introduced by the double cone approximation are less than 1%, and the error in the vignetting for double reflection is 4% at most (see Table 1), so Eq. (26) can be reliably applied to compute the effective area of the mirror, both on and offaxis.
The comparison between the results obtained from a raytracing (symbols) and from the application of Eq. (26) (lines) is shown in Fig. 8, for a source at infinity and 4 different values of the offaxis angle. For both computational methods, the reflectivity of the Gold coating was computed by assuming the same surface roughness rms of = 4 Å, regardless of the photon energy and the incidence angle. This is not completely correct, because the spectral window of the roughness power spectrum effective for Xray scattering changes with , , , and the size of the region over which the image is integrated. A variable , computed from the power spectrum of roughness in a variable frequency range, should be adopted (Spiga et al. 2009). Nevertheless, this has no relevance to the present comparison and we retain as a constant.
As can be noted from Fig. 8, the comparison provides a good agreement between the two methods, at all considered energies and offaxis angles. The analytical method underestimates the raytracing findings by only 3.7% at most, as foreseen, an amount close to the statistical error for the raytracing. This confirms the correctness of the analytical formula (Eq. (26)) for WolterI mirrors within the approximation limits stated in Sect. 2.
Finally, as an application to the hard Xray band (>10 keV), we consider the case of a long focal length (f = 20 m) Xray mirror with a wideband multilayer coating. Because of the complex dependence of multilayer reflectivity on the photon energy and the incidence angles, this example places the analytical method to the test, because any departure of the incidence angles from the true values would result in a displacement of the reflectance peaks. As simulation parameters, we assumed R_{0} = 296.2 mm, and L_{1} = L_{2} = 300 mm, deg. The geometrical area for a source onaxis, at infinity, would be 5.17 cm^{2}. The ratio expressing the departure of the double cone from the Wolter's, , is only 1.5%. The multilayer coating is supposed to consist of 200 pairs of Pt/C layers. The layer thickness decreases from the coating surface towards the substrate, according to the wellknown powerlaw for the dspacing  i.e., the sum of the thicknesses of two adjacent layers  d_{j} = a(b+j)^{c} (Joensen 1995), with j =1, 2, ..., 200 and a, b, c, parameters with values depending on the desired reflectivity. In the present example we adopted , b = 0.9, and c = 0.27, for a constant thickness ratio of Pt to the dspacing, . The outermost layer is Pt. Finally, the surface roughness of the mirror is assumed to have the constant value .
Figure 9: Comparison of effective areas of a multilayercoated WolterI mirror, as computed from a raytracing (symbols) and from Eq. (26) (lines). The source is supposed to be at infinity (). The error bars of the raytracing outputs are not shown. The accord between the curves is within a few percent onaxis (triangles) and 6 arcmin offaxis (circles). 

Open with DEXTER 
Figure 10: Comparison of effective areas of a multilayercoated WolterI mirror, as in Fig. 9, but with the source at a finite distance ( = 5 arcmin, m). The error bars of the raytracing outputs are not shown. The accord between the curves is within a few percent onaxis (triangles) and 4 arcmin offaxis (circles). 

Open with DEXTER 
The results of this test are shown in Fig. 9 for a source at infinity, and in Fig. 10 for a source at a 102 m distance from the mirror. The results for a 10^{4} ray tracing for each energy value (1 keV steps) are plotted as symbols, whereas the results for the application of Eq. (26) are plotted as lines. The statistical error of the raytracing results is of a few percent at low energies and close to 8% at high energies, where the reflectivity is lower. We note the excellent matching of peak positions and shapes in both cases. A mismatch of a few percent can be observed at low energies, even at , which is probably still related to the double cone approximation (Eq. (12)).
From these examples, we also note that, even onaxis, the effective area is heavily reduced by the source at a 102 m distance from the mirror. This occurs because = 0.083 deg is close to = 0.106 deg, although still smaller, thus the onaxis geometric area is only 12% of the one we would have with (see Eq. (9)). For the case = 0, the effective area also decreases with almost everywhere, as predicted by Eq. (32). The opposite effect is observed for a source at a 102 m distance, in agreement with Eq. (39), which predicts an increase in the geometric area with when , as in the case that we considered. Finally, we also note how the reflectance features are smoothed out when the source moves offaxis, because of the variation in incidence angles over the reflecting surfaces.
6 Final remarks and conclusions
We have shown how the problem of computing the effective area of a WolterI mirror with can be reduced to the computation of an integral (Eq. (25), or Eq. (26) as a particular case), on the only condition that we are able to compute , the mirror reflectivity as a function of the photon wavelength and the incidence angle. This can easily be achieved numerically for a source at infinity, as in astronomical cases, or for a source at finite distance, as usually done for onground calibrations. For the ideal case of a constant reflectivity r =1, we could solve the integral and obtain algebraic expressions for the geometric area of the mirror. Finally, we presented some examples of the application of the formalism, and checked that its predictions agree with those of a detailed raytracing routine.The analytical approach undoubtedly has several advantages. In general, the multilayer reflectivity computation is the Achilles' heel of a raytracing program that is aimed at determining the offaxis effective area of a mirror: although conceptually simple, the reflectivity computation consists of summing up the contribution of several layers to the reflectivity, so it requires a significant amount of computation time. A raytracing routine often requires photons to return sufficient statistics for each photon energy, and the reflectivity routine has to be called for each of them. Hence, the total computation time can reach several hours. If the optic is still to be designed, the entire simulation needs to be run several times, adjusting the parameter values every time, until the optimal solution is reached: the optimization process can thereby take several days.
In contrast, the analytical approach presented in this work is completely unaffected by statistical errors. Its accuracy is limited only by the applicability of the double cone approximation (discussed in Sect. 2) and by the accuracy of the computation of the integral in Eq. (25). In practice, the reflectivity can be computed with, say, a 5 arcsec step of the incidence angle, without noticeably affecting the reflectivity of the multilayer. This means that, even for a very large offaxis angle, e.g., 10 arcmin, we need to compute the multilayer reflectivity only 500 times, at most, instead of more than 10^{4} times as required by a raytracing.
For these reasons, the approach presented in this work might be extensively used to compute the effective area of grazingincidence WolterI astronomical mirrors, on and offaxis, whenever applicable. On the other hand, as already stated in Sect. 1, it would not be applicable to very short focal lengths, or to systems of densely nested mirror shells, obstructing each other in the field of view: in this case a raytracing is, as of today, the only viable computational technique. Clearly, a raytracing is always necessary to investigate the angular resolution, especially whenever mirror deformations are present.
We note that, if analytical expressions for were available, it would be possible to solve explicitly the integral in Eq. (25) in the most general case, and obtain algebraic formulae for the effective area of a WolterI mirror. In this respect, an analytical approach for obtaining of a multilayer was developed by Kozhevnikov et al. (2001), but a concise expression for the reflectivity appears still to be unavailable. However, if this is achievable, the computation of the effective area, and consequently the optical design and optimization, for any astronomical Xray mirrors of sufficiently large might be simply reduced to the application of a handful of algebraic equations.
Acknowledgements
This research is funded by ASI (the Italian Space Agency). The authors acknowledge for useful discussions G. Pareschi, G. Tagliaferri, S. Campana, A. Moretti (INAF/OAB).
Appendix A: Vignetting for double reflection  onaxis source at finite distance
We derive Eq. (9), which returns the geometrical vignetting of a doublereflection mirror, caused by the finite distance of the source. We consider a radial section of a WolterI mirror (Fig. 1), in the xz plane, with the primary and secondary segment surfaces intersecting at a angle. We suppose that, as far as the effective area is concerned, the mirror profile can be approximated by a double cone. If the source were at infinity and onaxis (Fig. 1a), the incoming rays would impinge the primary and secondary segment at . We now move the Xray source to a finite, although large, distance D. The beam is no longer collimated, since it has a nonzero halfdivergency , where R_{0} is the radius at the intersection plane (z=0) of the mirror. Because of the small crosssection of the mirror as seen by the distant source, can be considered as a constant.
In this configuration, inspection of Fig. 1b shows that the incidence angle on the primary segment becomes
,
and that on the secondary one,
.
We consider a ray striking the primary segment at
,
with z_{0} <L_{1}. The angle formed by the ray direction with the optical axis, after the first reflection, is
:
the equation of the reflected ray is then
where, as usual, we approximate the functions with the respective small arguments. If z_{0} is sufficiently large, the ray misses the second reflection (Fig. 1b). The last reflection on the secondary mirror segment occurs if the reflected ray passes by the point . Substituting these coordinates into Eq. (A.1), and solving for z_{0}, we obtain Z_{0}, the maximum value of z_{0} for which we have a double reflection
regardless of R_{0}. Then the fraction of the primary segment that is effective for double reflection is V = Z_{0}/L_{1}, i.e.,
We now consider the entire mirror, obtained by a rotation of the profile in Fig. 1 about the optical axis. If the source is still onaxis, at a distance D, the vignetting given by Eq. (A.3) is easily applicable to all sectors of the mirror, and we obtain Eq. (9) exactly. In Appendix B, we see that this result can easily be generalized to a source offaxis.
Appendix B: Incidence angles and vignetting for double reflection  detailed calculation for a source offaxis at finite distance
We consider a double cone mirror (Fig. B.1), with optical axis aligned with z and the intersection plane at z=0. We define R_{0} to be its radius at z =0, the incidence angle for an onaxis source placed at infinity, and L_{1}, L_{2}, lengths of the primary and secondary mirror segments. We assume to be shallow and that the source is at the finite distance . If the source is onaxis, the beam impinges the primary segment with a nearly constant halfdivergency . We denote with r_{1}, , and z_{1} the radial, azimuthal, and axial coordinates of the impact point on the primary segment, and r_{2}, , and z_{2} on the secondary. We now assume the source to be moved offaxis by an angle , and choose the direction in the tilt plane of the source (the xz plane, like in Fig. 1). Our scope in this appendix is to determine analytically the incidence angles on the two mirrors, and , and the vignetting for double reflection, V, as a function of , , , , more generally than we did in Appendix A.
Figure B.1: Double reflection of an offaxis ray (dashed line) on a double cone mirror. Also shown are the direction vectors of the ray, and the normal vectors to the surface, and , at the impact points, and . 

Open with DEXTER 
The two conical surfaces are described in polar coordinates by the equations
The normal vectors to the two segments, directed inwards, are
if the double cone approximation is valid, the normal vectors are only a function of the 's angles. If the source were onaxis, the initial direction of the ray would have the expression
Since the source is offaxis by , we have to tilt by an angle about the y axis. The application of the rotation matrix returns the expression for the initial direction of the offaxis photon, ,
If is the incidence angle of the first reflection (measured from the surface), we can write the scalar product
which becomes, after some algebra,
In the limit of small , , , we can approximate the cosines with 1 and the sines with their arguments, yielding
that is exactly Eq. (20).
To derive the incidence angle on the secondary mirror segment, we need to trace the exit direction of each ray,
,
after the first reflection. This is obtained from the vector equation
because the parallel component to the surface is conserved, whilst the normal component reverses its sign in the reflection process. By substitution of the Eqs. (B.5) and (B.3), one obtains, as always in the small angles limit,
A ray reflected at the generic point of the primary segment has equation , with t>0. Therefore, the reflected ray intersects the secondary segment at a position fulfilling the condition , i.e., for some t. This is equivalent to constraining the two vectors to be parallel:
where denotes a cross product.
Using both Eqs. (B.1) and (B.2), Eq. (B.11) can be developed into 3 scalar equations, only 2 of which are mutually independent, i.e.,
When , Eq. (B.10) infers and . In this case, the solution is barely and r_{2} = 4R_{0}3r_{1}.
We now search for a perturbative solution of these equations, of the kind
and
,
with
and
.
Substituting these expressions into Eqs. (B.12) and (B.13), neglecting terms in
,
and using Eq. (B.10) for the components of
,
we obtain a linear system in
and
,
whose solution is
For small offaxis angles, , , and , must then be of the order of or less, as expected from the simple argument presented in Sect. 3.2.
We can now derive the incidence angle on the secondary mirror segment, .
To this end, we write the scalar product
where is provided by Eq. (B.3). This would require the computation of and , which would yield a complicated expression. Nevertheless, all terms in are of second order, so they can be neglected in small angles approximation. We are then allowed to assume that and obtain after some passages , that is,
so we have found Eq. (21). This concludes the calculation of the incidence angles for an offaxis source.
Finally, we proceed to compute the vignetting factor for double reflection, in the general case of an offaxis source. In the following, since
,
we suppress the subscript and denote with
their nearlycommon value. From the value of
(Eq. (B.14)), and using Eq. (B.17), we derive r_{2},
Reflection on the secondary mirror segment occurs if , i.e., (see Eq. (B.2)). Substituting Eq. (B.18) into this inequality, using Eq. (B.1), and solving for z_{1}, we derive
where we indicate explicitly the dependence of the incidence angles on the azimuthal angle. So the fraction of the primary mirror segment effective for double reflection, at the polar angle , is Z_{0}/L_{1} or
The last equation generalizes Eq. (A.3) to the case of a source offaxis: it is Eq. (22), which we used for the computation of the offaxis effective area in Sect. 3.2.
References
 Abelès, F. 1950, Annales de Physique, 127, 597 (In the text)
 Bräuninger, H., Burkert, W., Hartner, G. D., et al. 2004, in Proc. SPIE, 5168, 283 (In the text)
 Burrows, C. J., Burg, R., & Giacconi, R. 1992, ApJ, 392, 760 [NASA ADS] [CrossRef] (In the text)
 Conconi, P., & Campana, S. 2001, A&A, 372, 1088 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
 Citterio, O., Campana, S., Conconi, P., et al. 1999, in Proc. SPIE, 3766, 198 (In the text)
 Cotroneo, V., Conconi, P., Cusumano, G., et al. 2009, AIP Conf. Proc., 1126, 88 [NASA ADS] (In the text)
 Freyberg, M., Bräuninger, H., Burkert, W., et al. 2006, Exper. Astron., 20, 405 [NASA ADS] [CrossRef] (In the text)
 Friedrich, P., Bräuninger, H., Budau, B., et al. 2008, in Proc. SPIE, 7011, 70112T (In the text)
 Gondoin, P., Aschenbach, B., Beijersbergen, M. W., et al. 1998a, in Proc. SPIE, 3444, 278
 Gondoin, P., Aschenbach, B., Beijersbergen, M. W., et al. 1998b, in Proc. SPIE, 3444, 290 (In the text)
 Joensen, K. D., Voutov, P., Szentgyorgyi, A., et al. 1995, Appl. Opt., 34, 7935 [NASA ADS] [CrossRef] (In the text)
 Koglin, J. E., Christensen, F. E., Craig, W. W., et al. 2005, in Proc. SPIE, 5900, 266 (In the text)
 Kozhevnikov, I. V., Bukreeva, I. N., & Ziegler, E. 2001, Nucl. Instr. Methods Phys. Res. A, 460, 424 [NASA ADS] [CrossRef] (In the text)
 Kunieda, H., Takahashi, T., Kokubun, M., Nakazawa, K., & Ogasaka, Y. 2008, in Proc. SPIE, 7011, 70110D (In the text)
 Mangus, J. D., & Underwood, J. H. 1969, Appl. Opt., 8(1), 95 (In the text)
 Névot, L., & Croce, P. 1980, Revue Phys. Appl., 15, 198 (In the text)
 Ogasaka, Y., Kunieda, H., Mizyawa, T., et al. 2008, in Proc. SPIE, 7011, 70110P (In the text)
 Pareschi, G. 2004, Mem. Soc. Astron. Ital. Supp., 5, 362 (In the text)
 Pareschi, G., Attiná, P., Basso, S., et al. 2008, in Proc. SPIE, 7011, 70110N (In the text)
 Parmar, A., Arnaud, M., Barcons, X., et al. 2004, in Proc. SPIE, 5488, 388 (In the text)
 Parrat, L. G. 1954, Phys Rev., 95, 359 [NASA ADS] [CrossRef] (In the text)
 Piro, L., Den Herder, J. W., Ohashi, T., et al. 2009, Exper. Astron., 23, 67 [NASA ADS] [CrossRef] (In the text)
 Predehl, P., Hasinger, G., Böringer, H., et al. 2006, in Proc. SPIE, 6266, 62660P (In the text)
 Spiga, D., Basso, S., Cotroneo, V., et al. 2009, AIP Conf. Proc., 1126, 41 [NASA ADS] (In the text)
 Takahashi, T., Kelley, R., Mitsuda, K., et al. 2008, in Proc. SPIE, 7011, 70110O (In the text)
 Tawara, Y., Yamashita, K., Kunieda, H., et al. 1998, in Proc. SPIE, 3444, 569 (In the text)
 Van Speybroeck, L. P., & Chase, R. C. 1972, Appl. Opt., 11, 2 [CrossRef], 440 (In the text)
 Zhao, P., Jerius, D. H., Edgar, R. J., et al. 2004, in Proc. SPIE, 5165, 482 (In the text)
All Tables
Table 1: Some examples of approximation introduced by the double cone geometry.
All Figures
Figure 1: Meridional section of a WolterI mirror, here in the case : a) source onaxis, at astronomical distance; b) source still onaxis, but located at finite distance (all angles are greatly exaggerated). 

Open with DEXTER  
In the text 
Figure 2: Percent accuracy of the primary segment crosssection area, as seen by a source onaxis from infinity, in approximating a WolterI profile with a double cone. 

Open with DEXTER  
In the text 
Figure 3: Vignetting due to the finite distance of the source onaxis, as a function of the fnumber, for L'_{1} = L'_{2} and 4 different values of . Solid lines are computed assuming a WolterI profile, dashed lines a double cone (Eq. (11)). The results for the double cone are completely independent of the choice of L': those for the WolterI are computed assuming L' = 0.5. 

Open with DEXTER  
In the text 
Figure 4: Percent accuracy of the double cone approximation in the estimation of the vignetting factor for a source onaxis at finite distance, as derived from the curves of Fig. 3 (symbols). Lines are traced using the empirical Eq. (12) with L' = 0.5. 

Open with DEXTER  
In the text 
Figure 5: A grazingincidence double cone mirror, illuminated by an offaxis source: the dashed line is a ray path. The optical axis lies along the z direction and the x axis is chosen for the source S, at a distance , to lie in the xz plane. The source direction forms an angle with the z axis. The azimuthal positions of the reflection points are located along with the and polar angles. 

Open with DEXTER  
In the text 
Figure 6: Normalized geometric area, , for a double cone mirror with a deg, as a function of the offaxis angle, for different angles due to the finite distance of the source. The curves are traced using the analytical formulae reported in Sect. 4. 

Open with DEXTER  
In the text 
Figure 7: Comparison between some analytical curves of Fig. 6 (lines), and the results of an accurate raytracing (symbols) for a WolterI mirror with the same (0.2 deg) and L' = 0.5. To avoid confusion in the figure, not all curves were represented. Note the very good matching of the two methods, within the error bars of the raytracing. 

Open with DEXTER  
In the text 
Figure 8: Comparison of effective areas of the largest WolterI mirror of NewtonXMM, as computed from raytracing (symbols) and from Eq. (26) (lines). The source is supposed to be at infinity (). The agreement is very good to within a few percent. 

Open with DEXTER  
In the text 
Figure 9: Comparison of effective areas of a multilayercoated WolterI mirror, as computed from a raytracing (symbols) and from Eq. (26) (lines). The source is supposed to be at infinity (). The error bars of the raytracing outputs are not shown. The accord between the curves is within a few percent onaxis (triangles) and 6 arcmin offaxis (circles). 

Open with DEXTER  
In the text 
Figure 10: Comparison of effective areas of a multilayercoated WolterI mirror, as in Fig. 9, but with the source at a finite distance ( = 5 arcmin, m). The error bars of the raytracing outputs are not shown. The accord between the curves is within a few percent onaxis (triangles) and 4 arcmin offaxis (circles). 

Open with DEXTER  
In the text 
Figure B.1: Double reflection of an offaxis ray (dashed line) on a double cone mirror. Also shown are the direction vectors of the ray, and the normal vectors to the surface, and , at the impact points, and . 

Open with DEXTER  
In the text 
Copyright ESO 2009
Current usage metrics show cumulative count of Article Views (fulltext article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 4896 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.