Tutorial : image position, magnification and numerical aperture - thin lens

For optical systems working in Gauss conditions, the paraxial image P_i of a plane P perpendicular to the optical axis is also a plane perpendicular to the optical axis.

Accordingly, for a segment joining two points A and B in the plane P, the conjugated segment A_iB_i is contained in P_i and is perpendicular to the optical axis. The transverse magnification m ( currently called "magnification" ) is the ratio A_iB_i/AB where AB and A_iB_i are the algebric lengths of the considered segments. Consequently, m is an algebric value.
m is constant whatever the points A and B in the plane P.
It is negative when AB and A_iB_i have opposite signs (which means that object and image are oriented in opposite directions). It is positive when AB and A_iB_i have the same sign ( which means that object and image are oriented in the same direction ).

m depends on the paraxial parameters of the optical system ( focal lengths, principal planes location ) and P position.

An optical system is in general made of several reflecting or refracting surfaces. The paraxial image of an object can be determined with a step by step process by calculating first the intermediate paraxial image of the object by the first surface, then calculating the conjugate of this intermediate image by the second surface and so on. This process is tedious. However, it is used for calculating the paraxial parameters detailed in the "paraxial parameters" tutorial as the principal planes, focal planes and focal lengths. Once these parameters determined, they are used in simple formulas to define the conjugation between an object and its paraxial image through the optical system.

The position of the paraxial image through an optical system can be obtained geometrically considering two characteristic rays (ray (1) and ray (2)) coming from an off-axis object. The first ray (1) is parallel to the optical axis and the second one (2) goes through the front focal point. Both rays (1) and (2) intercept the primary principal plane at the respective heights h₁ and h₂ (h₁ and h₂ being respectively the object height and the image height). Therefore, emerging rays (1') and (2') respectively from rays (1) and (2) intercept the secondary principal plane at the same height than their incident ray on the primary principal plane. ray (1') focuses on the back focal point while ray (2') is parallel to the optical axis. The paraxial image of the object is the intersection of ray (1') and ray (2'). The plane passing through this point and perpendicular to the optical axis is the conjugated by the optical system of the plane perpendicular to the optical axis and passing through the object.

When the refraction indexes of the object and image spaces are the same, one can consider a third ray (3) coming from the object and intercepting the object nodal point (also front or primary nodal point). After passing through the optical system, the third ray (3') passes through the image nodal point (also back or secondary nodal point) and its direction is unchanged. Obviously, this third ray (3'), ray (1') and ray (2') are intersecting at the same point (corresponding to the paraxial image) of the object. In the general case where refraction indexes before and after the optical system are not the same, the direction (3') is not parallel to the direction (3).


According to the paragraph above, the position of the paraxial image plane is given by the position of its intersection A_i with the optical axis. A is the intersection of the object plane with the optical axis. s_i is the algebric distance from the secondary nodal point N_i to A_i and can be calculated from the following formula :

.

s is the algebric distance from the primary nodal point N to A, f and f_i are respectively the front and back effective focal lengths. n₀ and n₁ are the refraction indexes respectively in the object and in the image space.

The magnification is .

Note that in the case where the refraction indexes before and after the system are the same :

In the case of a mirror where the emerging rays propagate against the incident rays direction, .

A_i position can also be calculated with x_i the algebric distance from the vertex of the last optical surface to A_i.
x_i is then a function of x, f ( or f_i ), n₀, n₁, l and l_i where x is the algebric distance from the vertex of the first optical surface to A, l is the algebric distance from the vertex of the first optical surface to the primary nodal point N and l_i is the algebric distance from the vertex of the last optical surface to the secondary nodal point N_i.

Sometimes, it can be useful to calculate z and z_i which are respectively the algebric distances FA and F_iA_i (F and F_i being respectively the front and back focal points) : .

The aperture is supposed to be the only surface of the system stopping light rays. This surface can be in the object space, in the image space or in an intermediate space.

In any case, it is possible to define the aperture in the object space: it is the conjugate of the aperture by the sub-system formed with the preceding components and used in the reverse way. Also, it is possible to define the aperture in the image space which is the conjugate of the aperture by the sub-system formed with the following components. The aperture in the object space enables to defines the solid angle inside which the rays are launched from the field(s). The aperture in the image space enables to eventually calculate the Wave Front Error and the associated parameters as well as the diffraction limit of the system.

Note that in some cases, vignetting can appear. Indeed, some rays coming from off-xis objects may be stopped by another surface than the said aperture surface. This can affect the aberrations, limit the system resolution and create some shadows on the image. In general, one try to avoid vignetting and this case is not considered in the rest of the tutorial.

An optical system is represented in the pictures below with different aperture positions. Theoretically, the chief rays (chief rays are defined further in this tutorial) coming from different objects (fields) intersect the aperture surface at the same point. This point is the aperture center.

In the left picture, the aperture is defined by the first surface. In the right picture, the aperture is defined by a surface in the middle of the optical system.

In the left picture, the system is telecentric (aperture at infinity) in the object space as the chief rays in the object space are all parallel. In the right picture, the system is telecentric in the image space as the chief rays in the image space are all parallel.

The aperture can be defined in several ways.

It can first be specified by the diameter D of the aperture itself.

It can also be defined by the half aperture angle θ_M in the object space. θ_M is the angle with the axis of a ray coming from the on-axis object and passing at the edge of the aperture in the object space (called marginal ray). θ_M is often used to specify the aperture of illumination optics. For these systems, θ_M may be larger than 90°.

The aperture is commonly specified with the numerical aperture in the object space NA.

where n is the refraction index in the object space.

The aperture is also often defined with the F number (common notation: F/N, F#, F_number). It is currently the case for many systems as for instance camera lenses.

.

. is the numerical aperture in the image space (n' is the refraction index in the image space). The larger the aperture, the larger the numerical aperture and the lower the F number. For optical systems with small aperture and working for objects located at infinity, the F number is approximately the ratio of the focal length f_i to the diameter D of the stop surface : .

In Gauss conditions, θ'_M is the angle with the optical axis of the marginal ray after transmission through the optical system according to the rules of the paraxial conjugation. Therefore, the marginal ray intercepts the on-axis paraxial image on one side and the secondary principal plane on the oher side at the same height than the incident marginal ray on the primary principal plane.