Plan an Observation | The Schools' Observatory

Planning an observation for a telescope is quite a tricky thing. You may know that you want to observe a galaxy, but which of the many millions we know of? And exactly what do you need the telescope to do to get the image or data that you want?

The Go Observing pages will help you through all the decisions you need to make, but here you can learn a bit more about all the details.

Coordinates: Where is it?

As the Earth spins around each day, and orbits around the Sun each year, the part of the sky that can been seen from any place on Earth changes.

To help work out if something is visible at a telescope at any particular time, we use coordinates.

Every star and galaxy has its own coordinate which tells us where it is in the whole sky around the Earth. At any time we can use that coordinate to work out where a telescope like the Liverpool Telescope (LT) would need to point to observe it.

3D depiction of the celestial sphere with the sky "wrapped" around Earth at the center. The full equatorial coordinate system is shown, along with locations of the Sun in the sky at equinoxes and solstices. — Equitorial Coordinate System

There are three main things that coordinates tell us:

North/South: Some objects are in the sky a long way to the south of the equator and so can only be seen from the southern hemisphere. They can never be observed by the LT on La Palma. Others are quite far south and so only ever get a little bit above the horizon from the LT, making them more difficult to observe.
Time of year: As the Earth orbits around the Sun, different parts of the night sky appear to move away from the Sun. This is the bit of sky that is "up" during the night. We can use the coordinate to work out when during the year an object is visible at night, and not hidden by the bright daytime sky.
Time of night: As the Earth spins, it makes the stars look as though they move across the sky, with some rising and setting just like the Sun. Using an object's coordinate we can work out the best time each night to observe it, usually when it is high in the sky.

This is all a bit more complicated for the Moon, asteroids, and planets that are orbiting around the Sun as their coordinates do not stay the same. However, we can calculate what their coordinates are at a particular time, so we can still work out when they can be observed.

The coordinates of objects are used to help to make the coloured bars that you might see as you Go Observing.

Instrument: What do you want to find out?

Professional telescopes usually have several different instruments. Which instrument you use will depend on what you want to learn from your observation.

If you want to measure the size of a galaxy, or the brightness of a star you would use a camera to get a nice image, but if you want to find out what something is made of, you would use a spectrograph or spectroscope.

Photograph of a scientific instrument setup featuring optical components and prisms, with light being dispersed into a spectrum, used for astronomical observations or experiments. — The inside of the FRODOSpec spectrograph on the LT

The Liverpool Telescope (LT) has quite a few instruments, and they are often upgraded or replaced with newer, better ones. Most of the observations taken for The Schools' Observatory use a camera called IO:O. There are other instruments as well that can be used for different kinds of science.

Optical Cameras: These are rather like the camera you might have on a phone, but a bit more sophisticated, a lot bigger and much more sensitive (which means they can get images of very faint things).
Infra-red Cameras: Some of the things we want to study in the universe make light that we cannot see - other parts of the electromagnetic (EM) spectrum. One particularly interesting kind of EM light is infra-red. This is made by things that are a bit less hot than stars. It can be seen through big clouds of dust in space.
Spectrographs: Spectrographs split the light into all the different colours like a rainbow. Astronomers use these sorts of observations to measure lots of different things: chemical composition, temperature of stars, redshift of distant galaxies and much more.
Fast-readout cameras: Sometimes astronomical objects change very quickly. There might be explosions near a giant black hole as a star falls in, or a neutron star that is spinning very fast. To measure these quick changes, special cameras are used that can take lots of images very fast.
Sky Cameras: Sometimes it is useful to look at a large part of the sky, or even all of it. This might be to try to find unusual, rare kinds of object, or just to monitor the weather. The LT has several SkyCams.

Field-of-View: How big is it?

Although stars appear as dots in the sky, other kinds of object like galaxies or nebulae can look quite big. How big an object looks depends on both how big it actually is, but also how far away it is. The further away, the smaller it will look.

2 images of galaxies side by side, each against a black background with white dots of stars randomly scattered around in various sizes. On the left, the galaxy is small and sits centre-left, a white glowing sphere in the middle and the rest of it appearing as a fuzzy oval. On the right, the galaxy is centre and much larger, taking up most of the image. It has a glowing, white middle and fuzzy grey arms that spiral around it. — Comparing a small galaxy (NGC 23, left) and a large one (Messier 74, right)

Every instrument will have a Field-of-view or FoV, which is how much of the sky it can see. If you want to make sure you get the right measurements, you must check that the object you are observing fits into the FoV of your chosen instrument. If it doesn't, you will either have to choose a different object, change instrument, or take several observations to stick together.

Because how big an object looks depends on both its size and how far away it is, astronomers do not always use things like kilometres to measure sizes. Instead they use the angular size, how big something looks measured as an angle. So, if you want to know if an object is suitable, you can compare its angular size to the field-of-view of the camera.

For example, the FoV of the main camera on the LT (called IO:O) is 10 arcminutes, which is 1/6th of a degree. The Andromeda galaxy is about 6 degrees across, so far too big to be observed by IO:O. However, the Fireworks Galaxy is just over 9 arcminutes across and fits in the FoV very well.

There are many galaxies, nebulae, and so on in the universe. It can be quite difficult to find out or measure their size. In Go Observing, we have selected objects that fit into the FoV well.

Exposure Time: How long to look?

One of main reasons why telescopes have such big mirrors and lenses is to gather as much light as possible. This means that very faint things can be observed.

Observations can be made even better by looking for a very long time. The longer you point a telescope at something, the more light you will collect. This is called the exposure time.

2 side by side images of the same grey, bubble-like nebula against a black ground with a few stars appearing as bright, white circles. On the left, the nebula is faint and barely visible. On the right, the nebula is slightly brighter and has more detail. — Observations of a nebula with different exposure times (left: exposure time of 30 seconds, right: exposure time of 120 seconds)

Working out the best exposure time for an observation can be quite tricky. Obviously if you have a telescope entirely to yourself, and you only want to get one observation, then you can simply take all night.

However, professional telescopes are used by many astronomers, and they usually want to get as many things done as possible. You have to make sure the exposure time is long enough to find out what you want to learn, but not any longer as that would waste telescope time.

To work out the exposure time, you need to consider lots of different things:

Brighter objects need shorter exposure times. A bright star will need less time to get a measurement than a faint one.
You need to know how sensitive the instrument is (which tells you how much of the light that reaches the camera is actually detected by it). A normal digital camera in a smartphone might detect less than half of the light that hits it. The cameras on large telescopes are kept very cold which means they can detect as much as 98% of the light.
Finally, you have to decide how good you need the data to be. If you just want to find out where something is, then as long as you can see it in the observation, would be good enough. You might only need a short exposure time to acheive this. However, if you want to measure a very small change in how bright it is, you will need much better data and so a longer exposure time.

Because calculating exposure times is quite complicated, Go Observing will do the work for you. However, for some of the more advanced observations you may get to choose different exposure times to see how that changes your images.

Filters: What colour?

Most cameras on professional telescopes only measure the brightness of things. They are not able to measure colour at the same time. However, colour can tell you a lot about the universe. For example hot, blue stars are usually bigger and brighter than small red ones.

To find out about these colours, astronomers use special coloured glass filters. These only let through light of a particular range of colours, for example red. By looking at the differences between images taken using filters, you can find out a lot about the colours of the objects. For example, a blue star will be brighter in an image taken through a blue filter than in one taken through a red filter.

Filters on professional telescopes are very carefully made to let through an exact range of colours. This means that filters on different telescopes are the same and astronomers can easily compare images from different telescopes.

A rectangular steel plate with four rows of circles. Each row has five circles along it, and each circle is a different colour, though these colours are less noticeable where it is darker towards the left of the image. Some more noticeable colours are red, pink, orange, dark green, light green, and yellow. — The filters on NASA's Roman Space Telescope

On the Liverpool Telescope, the main filters are:

I filter: This is the reddest filter, and includes quite a lot of infra-red light.
R filter: The red filter. This is a good one to use for most stars and galaxies.
V filter: V stands for "visual" and this covers most of the middle of the rainbow. It picks up lots of green light.
G filter: Although it may sound like this is the best green filter, it actually contains quite a lot of blue light as well.
B filter: The blue filter. For some fainter objects, the G filter is slightly better for blue light.
U filter: This includes a bit of ultra-violet (UV) light. It is quite good for very blue objects, but the camera is less sensitive for UV light than visible light, so exposure times need to be a lot longer.
H-alpha filter: This is a special "narrow" filter that only lets through a very small range of colour in the red part of the spectrum. This is exactly the colour of light that the element Hydrogen can make when it gets hot. As hydrogen is the most common element in the universe, this filter is a good when you are hunting for hot gas.
Neutral Density filters: Neutral Density (or ND) filters are ones that have no particular colour but which stop a certain amount of all colours. While this is normally a bad idea, for the very brightest objects like the Moon or bright planets, you might need an ND filter to stop the camera getting overwhelmed (or saturated). The LT has two ND filters: NDI-V which lets through about 1/30th of the light, and NDIII which only lets through 1/1000th! Using both at the same time only lets through 1/30,000th of the light. This is needed to observe very bright things like Venus.

For most observations in Go Observing we have chosen the best filters. However there are some advanced options where you can experiment with different filters.

Seeing: How blurry can your image be?

"Seeing" is what astronomers call the "blurring" of astronomical pictures by the atmosphere. The amount of blurring changes, and observations that need the sharpest possible images can only be done at certain times.

Although the seeing above the LT on La Palma is usually much better than most other places in the world, it can vary. When planning your observations, you need to think about how blurry it can be before it stops you learning what you want to find out.

If you need the very best conditions, then the telescope can wait until the seeing is at its best. That will of course mean you might have to wait a long time. You may also have to work around other observations that need the same, rare high-quality seeing. On the other hand, if you let the telescope observe at any time, your observation might be done more quickly, but it could be very "blurry".

When you choose an observation in Go Observing, unless it asks you to choose the seeing conditions you want, it will choose a good balance between getting the observations done as quickly as possible and not being too blurred.

Students can learn more about the effects of astronomical seeing using our Seeing Workshop.

Sky Brightness: How faint can you go?

While some things in the night sky are quite bright like the Moon or some stars, many of the things we want to observe are quite faint. Even with a big mirror and a long exposure time, some faint objects are still difficult to observe, especially if the sky is not really dark.

Fortunately on La Palma we do not need to worry about light pollution, but some other things, like twilight or the Moon, can make the sky too bright to observe the faintest objects.

Two circular images side by side showing a partial view of a telescope, though most of the image shows the night sky. On the left, there are small white dots of stars and the dusty band of the Milky Way stretches in a slightly curved vertical line from top to bottom. On the right, there is a large white sphere to the right of the centre, and the sky is just dark. — SkyCamA images above Liverpool Telescope on different nights. On the left, the Milky Way is visible. But on the right, the moon is too bright for it to be seen.

Twilight: Just after the Sun has set, and again as dawn is approaching, the sky gets brighter. Even when you might not be able to see the difference with your own eyes, the special cameras on the telescope can tell the difference. For any objects that are not bright we need to avoid what is called "Astronomical Twilight".

Moon: The Moon is bright enough that it can make the whole sky glow. How bright the sky is around your object depends on the phase of the Moon (the full Moon is obviously brighter) but also on how far apart the object and the Moon appear to be. For fainter, fuzzy objects like galaxies and nebulae this can be very important. Often it means that they cannot be observed near to full Moon.

The effect of sky brightness can be predicted, so it is used to help to make the coloured bars that you might see as you Go Observing.

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