Now, to correct for coma, we will adjust the radii of curvature of the first and fourth surface, (i.e. the first surface of the first lens and the second surface of the second lens). In order to keep the optical power unchanged, we would like to have (1/R1)+(1/R4)=const. So, increasing one radius will decrease the other one. We will repeat this process until an acceptable coma reduction is achieved.

Barlowlens 5x

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We will stop our discussion about optimization here.  As mentioned before, there are different ways to attack this problem, and there are more tools that we can use to analyze an optical system.  In future blogs, we will talk about ray intercept graphs and we can return to another example of optimization or simple analysis.

In the previous step, we calculated the focal length of each lens, but we still need to define the radii of curvature. So let’s define those before attacking coma. To simplify (and reduce the length of this article), we will assume symmetric lenses with equal radii of curvature in the front and back surfaces of each lens. A first approximation for our lenses can be found using the following equations:

For instance, if you have a 30mm, 24mm and 10mm eyepiece, having a Barlow in your collection effectively adds a 15mm, 12mm and 5mm eyepiece to your collection. Since one decent Barlow lens is much cheaper than three new eyepieces, it is really cost effective!

One thing to keep in mind while buying a Barlow lens is that if it fits the tube of your eyepiece. Most tubes come in one of two standard sizes, either 1.25 or 2 inch, so finding the one that fits won’t be a problem. You just need to make sure to get the right one.

You might know that the magnification of a telescope is the focal length of objective divided by the focal length of the eyepiece.

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We calculate some of the Seidel aberrations and look at the Ray Analysis graphs (we should talk about them at another time). We calculate a chromatic focal shift of 1.5 mm along the axis, a maximum spherical aberration of 4mm at 20-degrees, and a Seidel coefficient for coma (third-degree) of 0.157.

They contain a concave lens that is placed between your telescope’s objective lens or mirror and eyepiece. (Actually, they contain more than one glass element to reduce chromatic aberration).

The last aberration that we will correct for is spherical aberration. Once the first two aberrations are solved for, spherical aberration can be relatively simple to tackle. We may say that we have two tuning variables that we can modify to produce either a coarse or fine tuning. If we have a significant amount of spherical aberration, we can modify one of the internal radii of curvature of our lenses (i.e. surface two and three). If we have a small amount of spherical aberrations, we can modify the spacing between lenses.

In order to reduce chromatic aberration, we need to find a way to match the lens focal length regardless of the wavelengths we are using. A way to do this is by using an achromatic doublet. As mentioned before, the achromatic doublet has two lenses: a negative lens (concave) and a positive one (convex). The basic idea is that both lenses will compensate their respective dispersions and cancel each other.

Using a 20mm eyepiece on a telescope with a 1000mm focal length gives 50x magnification (1000mm / 20mm). Attach a 2x Barlow lens to that same eyepiece and you double its magnification to 100x!

With over 15 years of experience and 500+ unique optical systems designed, Optics for Hire specializes in advanced optical engineering. If it uses light, we've worked on it.

2. A large difference in Abbe number will help us to have lower curved surfaces and will help in optimizing coma and spherical aberrations

Barlowlens 3x

The reason we do is because more powerful Barlows don’t work well with smaller telescopes. Small scopes don’t pull in much light, so powerful Barlows deliver dim, disappointing images.

With over 20 years of experience and 800+ unique optical systems designed, Optics for Hire specializes in advanced optical engineering. If it uses light, we've worked on it.

Barlowlens vs eyepiece

One final advantage is that Barlows do not change the longer eye relief typical of lower power eyepieces (in fact, they actually increase it some in some cases). This allows eyeglass wearers to see a full field of view at high power without removing their glasses.

Jun 10, 2022 — Depending on the manufacturer, each anti-reflective lens will reflect a certain color. Most tend to be green or purple. Spectacle lenses with a ...

As backyarder astronomers, we have a big interest in equipment that makes our stargazing better without burning a hole in our pockets! The humble Barlow lens is a great example of such a piece of kit.

Barlowlens 2x

We will be using an achromatic doublet without referring to any specific application for this example. So we will be working with two common glasses: BK7 (abbe-number = 64.166 and n_green = 1.52237) and SF2 (Abbe-number = 33.819 and n_green = 1.6612). To calculate the radius of curvature for our lenses , we will be using equations 3 and 4.

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We believe you’ll be better off with a decent Barlow lens most of the time, especially early on in your stargazing career, when simplicity and cost are big concerns.

The negative component is usually made of what is called “Flint glass”. Flint glass has some lead and a particular high chromatic aberration (described by an Abbe number below 50), and high refractive index (usually above 1.55). Some types of flint glass are: F, LF, SF, KF, BaF, BaLF. Lead-free flint glass usually has a “N” before their name. For example N-SF8.

What isBarlowlens in telescope

There are also different configurations of achromatic doublets you may want to consider, for example: Littrow, .Fraunhofer and Clark doublets.

The presented method is just one that may help you to do a simple optimization. More complicated methods involve reducing chromatic aberration for a specific line and calculating coma coefficients for each optical element, and minimizing their combined effect. This method gives a better starting point to reduce aberrations.

The diagram shows an effective increase in telescope focal length – the yellow light cone’s point is further along from the ‘diverging lens’ than the gray light cone’s point. The longer focal length of the yellow light cone is due to the impact of the Barlow lens.

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Zoom lenses provide a variable amount of magnification, whereas Barlow lenses have a fixed magnification level. Also, Barlow lenses generally have a smaller field of view than zoom eyepieces.

Before we start, we need to mention that there are different ways to optimize any design; there is no “formula” that an engineer can apply to yield the best results. It is a process that requires revisions and feedback. It is, in a sense, an art that benefits from the optical engineer’s technical knowledge. What is presented here is just a method we have used in the past with acceptable results.

where V1 and V2 are the Abbe numbers for the first and second elements, respectively. Solving for f1, and f2 from Eq. 1 and Eq. 2, we get:

Their effect is to increase the magnification of any eyepiece used with them, usually 2 or 3 times. As you’d expect, a 2x Barlow doubles your eyepiece magnification, whilst a 3x trebles it.

You can use C/CS Mount Converting Adapter when you put C Mount Lens on CS Mount Camera. P/N, Description, Outer Dia. (mm), Length (mm), Inner Dia.

We first need to be familiar with the concept of the Abbe Number (or V-number), a measure of the dispersion of glass; the higher the Abbe number, the lower the dispersion. Figure 1 shown the Abbe diagram where we can plot the V-number versus the refractive index for several types of glass.

The first aberration that we will try to correct for is chromatic aberration. This is, after all, one of the main reasons we will be using an achromatic doublet. As mentioned in the early article, an achromat is formed by using a flint glass and a crown glass. Using the right combination of glasses will reduce chromatic aberration but the choice of glass can be daunting. How do we know what type of glass to use?

But, since a Barlow is normally used to look at objects at high power in the center of the field (where the image is unaffected), this is not a dealbreaker.

It’s an essential piece of equipment every astronomer should have but, if you don’t know much about it, then this article will explain everything you need to know.

At this point, we will be changing the radius of curvature of the first and fourth surfaces. We’ll try to keep the focal length as close as possible to 50mm. There are different ways you can try to do this optimization. OSLO and Zemax have different algorithms that can be used for different kinds of optimizations. For this example, however, we will just change the values in small amounts.

Their changing focal length makes it harder to correct for aberrations, so zoom lenses have a combination of at least 4 glass elements. This makes them bigger and heavier than Barlow lenses.

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3. The negative lens (flint glass) should preferably have a higher refractive index than the positive lens (crown glass)

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From those equations we get an R_1 = 24.77 mm and R_2 = -59.33. At this point, we will have the same radii of curvature for the front and back surfaces, so we will have a biconvex and a biconcave lens, as shown in Fig 3

Barlow lensesreview

A Barlow lens is a tremendously useful instrument to have in your collection. In fact, we think they are an essential piece of equipment for every backyard astronomer!

One of the most common optical structures is the achromatic doublet. It is used to reduce chromatic aberrations. At its most basic, it is a two lens system configuration where one lens is a concave lens, usually made of a flint glass, and the other is a convex element, usually made with crown glass.

where f1, and f2 are the focal length of the first, and second element, respectively, and feq is the equivalent focal length of the system. The second equation we need is:

Barlowlens Celestron

This video by David Fuller of Eyes on the Sky explains Barlow lenses in detail, including how to use them, and the types of Barlow which are available:

Once the glass types have been chosen, we can calculate the focal length of each optical element in our doublet with the following equations

The lenses used in SLR and DSLR cameras to vary the focal length (and hence zoom) are zoom lenses. Given below is an image taken while varying the focal length of a camera using a zoom lens:

How to installBarlowlens in telescope

Here we will show the process of achromatic doublet optimization. We’ll start with our requirements. We’re looking for a 50mm focal lens with a 20-degree FOV and 30 mm diameter.

At this point we will try to achieve two objectives: reducing spherical aberrations and keeping the focal point as close to 50 mm as possible.

From the spot diagram, we can see that there is significant coma (specially at full field) and some spherical aberration. Look at this entry to learn more about spot diagrams.

When correcting for one aberration, we need to keep monitoring the whole system: more often than not, lens optimization is a matter of compromising. Sometimes it is not possible to completely reduce all aberrations simultaneously.

We still see significant coma and spherical aberration at this point: the chromatic focus shift however has decreased from 1.5 mm to less than 0.1 mm. There are no significant changes on spherical or coma at this point. So we will try to correct for coma next.

Figure 3 shows the changes on the first and fourth surfaces. We changed the first surface from 24.77mm to 23.8mm and the fourth surface from 59.33mm to 60.2mm. After these changes, the chromatic aberration is still under 0.1mm as before, but the Siedel Coma coefficient has been reduced to 0.0305 (from our original 0.157). Also the spherical aberration has been reduced to almost 2mm at 20-degrees, so we will try to improve it next.

Barlow lenses come in different magnifications. The most common are 2x, but lenses that offer 3x or 5x are also available.

Instead of inserting an eyepiece into the focuser, you place in the Barlow lens. Your eyepiece is then inserted into the Barlow, like the example, left, from Celestron.

Let’s change the spacing between the first and second lens, and also the radius or curvature of the first surface of the second lens. We keep this iteration going until we reach the following lens combination.

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If we can correct the lens shown in Fig. 1 with an equivalent achromatic doublet, we will set feq to 50 mm and choose two materials for our lenses. For the flint glass, we choose N-SF8 with an Abbe number of 31.31 and for crown glass, we choose N-BK7 with an Abbe number of 64.17. Substituting these values into Eq. 3 and Eq. 4, we obtain values of 25.61mm and -50.48 for f1 and f2, respectively. Figure 2, shows a chromatic aberration using these numbers (note: the lens is not optimized).

The Barlow lens was invented in the 19th century by Peter Barlow, A mathematician, optician, astronomer and a member of the Royal Society of London.

We start by assuming that we have the goals of our designs, that is, we have the focal length, wavelength range, aperture diameter, FOV already defined. Based on this information, we have several variables that we can manipulate, those are:

Crown glass on the other hand is used to fabricate the positive component. Crown glass has a low dispersion (with an Abbe number above 50) and low refractive index (usually below 1.5), although some glass like BK7 has a refractive index that overlaps with some flint glass. Crown glass names usually include a “K” at the end (form the german “kron”, crown). Some types of crown glass are: K, SK, BK, LaK, LaSK and many others.

We can see that our focal length is closer to our required 50 mm. We also still have our coma coefficient around 0.02 (just a little bit lower than before) and the spherical aberration less than 3 mm at 20-degrees.

Lower-priced Barlows have fewer or lower quality lenses. These can show minor astigmatism and spurious color at the field edges with fast (smaller than f/6) focal ratio scopes.

First, we need to understand what is chromatic aberration and why it occurs. Chromatic aberration is the effect caused by the change in refractive index for a given material at different wavelengths. For example, BK7 has a refractive index of 1.5228 at 480 nm (blue) and of 1.5131 at 700 nm (red). That basically means that if we have a biconvex lens made with BK7, it will focus red and blue light at different points, resulting in chromatic aberration. This is shown in Figure 1.

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The combination of unique materials (flint glass and crown glass) and the lens shapes of the doublet, an optical engineer can use the science of light to deliver lens solutions without chromatic aberrations.