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Telescopes are instruments which use multiple lenses to produce magnified images of distant objects. It is unclear who invented the first telescope: lenses had been widely used in Europe to correct poor eyesight since the fourteenth century and I expect that, over time, the telescope was actually invented many times by different individuals, who discovered that combining different lenses could produce a magnified image.

In 1608 a spectacle maker called Hans Lippershey applied to the Dutch government  for a patent for a device for seeing at a distance. His application was refused and, in the resulting publicity, the Italian astronomer Galileo Galilei (1564-1642) became aware of the device. Galileo refined the early telescopes to produce instruments with better magnification and in 1609 he took the first recorded astronomical observations with a telescope.  Indeed, the first use of the word telescope, which is constructed from the Greek words ‘tele’ meaning ‘far’ and ‘skopos’ meaning ‘seeing’, is associated with Galileo’s instrument.


Galileo Galilei – image from Wikimedia Commons

How the Galilean telescope works

There are various combinations of lenses which can be used to magnify distant objects, but the simplest is the one which was used by Galileo when building his telescope.  Telescopes of this design are called Galilean telescopes and to understand how they work it is necessary to understand a little about lenses.

There are two main types of lens:

  • a converging lens, shown in the top of the diagram above, causes parallel light rays from a distant object, shown in red, to bend so that they converge at point known as its focus. The focal length of the lens is the distance between its centre and its focus.
  • a diverging lens, shown in the bottom of the diagram, causes parallel light rays from a distant object to bend and spread out so they appear to have come from its focus. Like a converging lens, the focal length is the distance between its centre and the focus. By convention the focal length of a diverging lens is negative.

The diagram below, which if you’ve studied physics at high school you will recall is called a ‘ray diagram’, shows that when the rays of light from a distant object pass through a converging lens, they form an inverted image, which is reduced in size compared to the object.

The rays of light, coloured red, from the object (A) are focused by the converging lens to produce an inverted image (B).

The ray diagram below shows that when rays of light from a distant object pass through a diverging lens they spread out, so that they appear to come from an image which is closer to the lens and reduced in size compared to the object. This is called a virtual image, because the rays of light don’t actually form an image.

The rays of light, coloured red, from the object (A) appear to diverge from the virtual image B.

A Galilean telescope consists of two lenses: a large converging lens of long focal length (known as the objective) and an eyepiece which is a diverging lens of a short focal length. Interestingly, as the diagrams above show, both of these lenses on their own produce a smaller image of a distant object. I’ll explain next how they work together to produce an image which is enlarged.

If we consider a distant object, such as that shown below, then its apparent size is how large it appears when viewed by an observer.  For larger astronomical objects the apparent size is often measured in degrees. For example, the apparent diameter of the Moon is roughly 0.5 degrees. A telescope makes the apparent size larger.

In the diagram above, the blue line shows a ray of light from the top of a distant object. The red line shows a ray of light from the bottom of the object. The apparent size (a) is the angle between the two rays.

If we put a converging lens in front of the distant object then it will focus the light rays and produce an inverted image, which will be positioned as shown below.


The diagram above shows a number of light rays from the distant object.

  • A light ray from the top of the object striking the top of the lens (labelled 1) and a light ray from the top of the object striking the middle of the lens (labelled 2) are both brought to a focus.
  • A light ray from the bottom of the object striking the top of the lens (labelled 3) and a light ray from the bottom of the object striking the middle of the lens (labelled 4) are both brought to a focus.

If we put a diverging lens with a short focal length in a position where it intercepts the light rays before they are brought to a focus, then the light rays are bent by the diverging lens and follow the path below.


Key to diagram above

As you can see from the diagram above. the apparent size of the distant object is increased to b, which much bigger than the original value a. The magnification of the telescope (M) is defined as:

M= apparent size of image divided by apparent size of object

For more detail on this see the notes at the end of this post.

Galileo’s discoveries

Using his telescope, Galileo made a number of important discoveries which revolutionised astronomy. He discovered the four brightest moons of Jupiter which are now called the Galilean moons.

The four brightest moons of Jupiter – image from Wikimedia commons

He studied the way that the Moon was lit and how this changed over time and correctly deduced that this was due to shadows of lunar mountains and craters. Galileo turned his telescope to the Milky Way and discovered that it consisted of a vast number of stars, each too faint to be seen individually with the naked eye. When viewed from Earth these stars are so closely packed together they appear to be clouds. However, the discovery which had the greatest impact on his life was the phases of Venus, which I’ll talk about next.

Venus’s phases 

As seen from the Earth,  Venus goes through a full set of phases in a similar way to the Moon.  However, because Venus appears so small, these are only visible through a telescope. Galileo was the first person to see them.

Venus Phases

At point A in the diagram above, when Venus is between the Earth and the Sun, the sunlit part of Venus faces away from us making the planet almost invisible. The amount of the sunlit part of Venus we can see gets larger or waxes through to a crescent phase (B), to a half Venus (C)  and then to a full Venus at point D, when the whole sunlit side facing the Earth is illuminated.  It then gets smaller or wanes back to a half Venus (E) , then to a crescent (F) and then finally back to being almost invisible back at point A.

As readers of a previous post will know, in 1543, just before his death, Nicolas Copernicus (1473-1543) had published the theory of heliocentrism which states that the planets orbit the Sun. However, in Galileo’s time, the teaching of the Catholic church favoured geocentrism, the widely held view that the Earth was the centre of the Universe and the stars, planets, the Sun and the Moon were in orbit around it. Indeed certain verses of the bible could be interpreted as supporting that viewpoint, such as Psalm 104:5:

‘the Lord set the earth on its foundations; it can never be moved’

However, the phases of Venus which Galileo had seen can only be explained by Venus orbiting the Sun, not the Earth.  Therefore, Galileo concluded that the geocentric theory was incorrect.   Unfortunately for Galileo, in 1616 the Catholic church declared heliocentrism to be heresy. Heliocentric books were banned and Galileo was ordered to refrain from holding, teaching or defending heliocentric ideas.

Despite this ruling Galileo continued to defend heliocentrism, and in 1633 the Roman Inquisition found him ‘vehemently suspect of heresy’, sentencing him to indefinite imprisonment. Galileo was kept under house arrest until his death in 1642.

Improvement to telescope design

Galileo’s telescope could only magnify objects 30 times before the image became distorted. It also had a narrow field of view. In 1610 Johannes Kepler began investigations into the way that different combinations of lenses could work together to produce a magnified image. He invented a new type of telescope with a converging lens as the eyepiece This new design became known as the Keplerian telescope. It  enables a higher magnification with less distortion than a Galilean telescope, although it produces an upside down image, which this doesn’t really matter for astronomy.  Today the Galilean telescope design is only used in cheap low power binoculars.

Keplerian telescope – image from Wikimedia Commons


Keplerian and Galilean telescopes are both example of refractors where lenses are used to collect and focus light. Nowadays virtually all large telescopes are reflectors where curved mirrors, rather than lenses, are used.  Reflectors have a number of advantages over refractors.  One of them is that reflectors don’t suffer from chromatic aberration. This happens in refractors because different colours of light are bent very slightly differently as they pass through the lens, which results in a blurred image.  Chromatic aberration can be overcome by using achromatic lenses, which consist of two or more lenses made out of different types of glass joined together to form a compound lens, but this is expensive and technically difficult when constructing larger lenses. The main advantage of reflectors is that it is much easier to produce a large mirror than a large lens. A large lens many metres in diameters would be very thick, very heavy and difficult to manufacture to the quality needed in a telescope. It would also tend to sag, becoming deformed under its own weight,  producing a blurred image.

For these reasons the largest refractor used in professional astronomy is the one at Yerkes Observatory. It has an objective lens which is 1 metre in diameter. All telescopes larger than this are reflectors. Yerkes Observatory is based at Williams Bay, Wisconsin and it operated by the University of Chicago.  Sadly, it is due to close this year after an impressive 120 year history.

Yerkes Observatory – Image from University of Chicago


To calculate the magnification of a Galilean telescope, we divide the focal length of the objective by the focal length of the eyepiece. So, if the focal length of the objective is 200 cm and the focal length of the eyepiece is 10 cm, the magnification of the telescope would be 20.