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BAA Articles

Observer's Challenge – Saturn vs Pluto

At the 2019 Winchester week-end, Paul Abel and Pete Lawrence presented a series of observing challenges which members might like to have a go at during the year. Some are relatively easy, some really are quite challenging indeed.

There are actually two challenges here; read on...

The first challenge is to try and observe Saturn and Pluto at the same time. Saturn is an easy target and currently resides in Sagittarius. Pluto is also in Sagittarius and on 1st June 2019 the two planets are just 3.3 degrees apart. The pair will be low in the southern sky as viewed from the UK. Despite the vast differences in brightness (Saturn magnitude 0.28 and Pluto magnitude 14.3) will anyone be able to capture them on an image in the same field of view?

The second part of this challenge is observing the variation of Iapetus. Iapetus is a 3rd largest moon of Saturn. It has an interesting two tone surface - one hemisphere is rather bright, the other is covered in a dark reddish material. As a result, Iapetus changes in magnitude considerably as it orbits Saturn. Iapetus is brightest when on the western side of Saturn and faintest when on the eastern side. Iapetus takes about 79 days to complete one complete orbit of Saturn, so about 40 days from one elongation to the opposite one. A good time to start this challenge is in early June when the moon is at it greatest eastern elongation, and again in mid July when it is at its greatest western elongation. Saturn comes to opposition on 9th July 2019, when it will appear no higher than about 16 degrees above the horizon as viewed from London.

Please do post any observations you make to your BAA Member Page

Paul G. Abel & Pete Lawrence

[Thumbnail image by Peter Tickner]

BAA Members can access the 2019 BAA Handbook here.

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BAA Articles

Noctilucent Cloud and What to Look For

In 1884 a gentleman called Thomas Backhouse was looking at cloud formations. It had been a good year for this, as the effects of the Krakatoa eruption were still showing in sunsets all over the world. He noticed a new type of cloud which was only visible after sunset. He kept observing these clouds even after the dust of Krakatoa had faded. These clouds became known as polar mesospheric clouds or Noctilucent clouds (popularly referred to by the abbreviation “NLC”) and are high atmosphere clouds which occur over summertime at mid latitude locations. They form at very high altitudes – around 82 km above sea level – and are, thus, a quite separate phenomena from normal weather or tropospheric cloud.

NLCs can be seen in the northern hemisphere from around late May to early August during the darkest part of a summer’s night when the Sun is between 6 – 16 degrees below the horizon. Typically, they will occupy the northern horizon, along the twilight arch, extending to an altitude of 10 – 15 degrees. Over the NLC “season” the bright star Capella dominates this part of the sky and serves as a good marker for the NLC observer. They used to be associated with northern UK but were seen as far south as southern France in 2018, and they seem to be spreading further south with each season.

So, what do you look for and when? You need to start looking from about 11pm BST and keep going till 3am BST. You need a clear northern horizon and clear skies for the best chance of viewing them. All low clouds will appear dark, and you should also be able to see stars, particularly Capella. The colour of the clouds will vary from white to an almost electric blue and will stand out quite markedly. There are several types, but the most common and easiest to recognise is the “herring bone” or rippling sand type pattern which looks like lots of curved lines drawn in parallel. At the start of the season you may get days with out NLC but as it builds you may see several displays on consecutive nights.

Photographing them is easy but you will need a tripod to ensure a stable platform. Modern digital cameras will capture NLC with an exposure of anything from 0.5 to 6 seconds but it is best to vary shutter speed and take as many as possible as display intensity will vary.

Observations of NLC remain of great value to professional scientists studying upper-atmosphere phenomena. Useful observations are very easy to make and require no special equipment.

So in finishing, I wish you clear skies and pleasant nights observing NLC and it's normally a lot warmer than observing aurora in winter.

Please do send me your results and also post them to your BAA Members Page.

Sandra Brantingham

Aurora & Noctilucent Cloud Section Director

This images was by Dave Hancox (55.32N 004.40W)- 24/25 Jun 2018 - 3sec @f4.5 -48mm- 400 ISO- Pentax K70

Mick Nicolls, Sheffield, captured this image on 19/20 Jun 2018 using a Canon 1100D

Colin Ebdon, Colchester, Essex captured this image on 2/3 Jul 2018

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BAA Articles

Observer's Challenge – Finding Einstein

Date: Early morning 2019 May 3rd & 4th, and again early morning 2019 June 1st & 2nd

The crater Einstein is a libration zone feature and only visible when the libration favours the Moon’s western limb.

The chart below gives its location and some favourable times in early May and again in early June. At these times the Moon is still very low above the eastern horizon and only 3-4% illuminated. The Moon is also only 20 degrees away from the Sun so do take care when using a telescope.

You can find other times using the free NASA ‘dial a moon’ programme available via or by using the Virtual Lunar Atlas which is available from

Please do post any observations you make to your BAA Member Page

Paul G. Abel

[Thumbnail image taken from Moonglobe for iPhone]

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BAA Articles

Campaign to observe the old nova HR Lyr

Introduction to HR Lyr: a century of observations

This year is the centenary of the discovery of Nova Lyrae 1919. HR Lyr, as it is now known, was a magnitude 6.5 nova discovered on 1919 December 6 by Miss Mackie at the Harvard College Observatory. The decline from outburst was fairly well observed and showed a rapid (t3 ~ 80 days) and smooth decline. A review of the photometric history of HR Lyr was present in the BAA Journal in 2007 [1], finding that the system has been relatively stable at V ~ 16 ever since occasional post-nova monitoring (initially visual observations) began in 1925. More recently, the 22-year light curve between 1991 and 2012 was presented [2] which showed the system varied over the range V= 15.3-16.3 with occasional excursions to V~17. One these fades, in 2010, was discussed in the BAA Journal [3] and a further fade occurred in 2016. The light curve variations often take the form of nearly linear rises and falls on a timescale of about 100 days. Occasional ~ 0.6 mag outbursts were also seen, with properties similar to those found in some nova-like cataclysmic variables. Overall, there was a decline of 0.012 ± 0.005 mag/yr, similar to that seen in other post-novae.

Recent data from ASAS-SN suggests a period of 613 days [4], but this might not be statistically significant.

Scope and objectives of the 2019 campaign

Apart from photometric monitoring, HR Lyr has not received much attention. The aim of this campaign, which will run until the end of 2019, is to deepen our understanding of the photometric behaviour, on a range of timescales, as well as attempting to characterise its spectroscopic properties and variations.

It would be wonderful to shed some light on HR Lyr’s behaviour some one hundred years after Miss Mackie’s discovery!

Observations requested

Nightly photometry (visual and CCD)

To determine the overall light curve of HR during 2019, nightly observations are requested to provide a “snap shot” of how the star is performing and to monitor for the ~0.6 stunted outbursts that have been seen previously.

Observations can be visual (if you have a sufficiently large telescope) or CCD. V-band photometry is preferred, but if you do not have a V-filter, then unfiltered will also be acceptable. In addition, B- and R-band measurements will also be appreciated to see if there are any colour variations over the course of the campaign.

Sequences for HR Lyr can be downloaded from the AAVSO Variable Star Plotter [5]. Observations should be submitted to the databases of the BAA Variable Star Section or the AAVSO, preferably as soon as possible after the observation is made.

Time resolved CCD photometry

Rather little time resolved photometry is available for HR Lyr, so a major aim of the programme is to carry out several long photometry runs to see if there are any periodicities or other significant variations on a timescale of minutes to hours. A team at the Wise Observatory observing in the 1990’s found quasi-periodic variations around the period 0.1d, which they speculated may be associated with the orbital period [6]. However, no independent measurement of the orbital period of HR Lyr has been published. Perhaps our work will confirm of refute this. Ideally, runs of several hours should be performed if we are to identify signals with a period of ~0.1.

Again V-band photometry is preferred (plus other bands if available), but if this is not possible, unfiltered is fine. Again, observations should be submitted to the international databases.


HR Lyr is even less well characterised spectroscopically than photometrically! Its H-alpha profile in 1993 and in 2008 was composed of a sharp central peak having a FWHM of ~10 Å, plus a broad shallow base with typical FWHM of ~40 Å. In the 1993 spectra no changes were visible from night to night [2]. However, the line profile changed between the two adjacent 2008 nights. The H-alpha line showed a sharp central peak alongside a broader base which is not common among old novae, but is similar to the emission line profile described for the old nova DQ Her. There was no convincing evidence for a decline in the H-alpha line widths over the interval 1986–2008. The spectral appearance of HR Lyr during the 2010 dimming episode was quite different from that exhibited during normal quiescence; the spectrum 2010 spectrum was characterised by a smooth bluish continuum with superimposed strong emission lines [7].

Spectroscopy at various time during 2019 will be helpful to identify any changes in the spectrum (as found in 2008) and, if there are changes, whether these can be correlated with gross changes in the photometric light curve.

Spectroscopy of such a faint target represents a real challenge with amateur equipment. Almost certainly too faint for high resolution line profile measurements, it is probably just accessible with a low resolution instrument. It will be interesting to see whether it is possible to get worthwhile results.


Updates on the campaign will be given from time to time via the BAA VSS Alert email group [8] and on the Forum of the main BAA website.

[1] Shears J. & Poyner G., JBAA, 117, 136 – 141 (2007)

[2] Honeycutt R.K., Shears J., Kafka S., Robertson J.W. & Henden A., AJ, 147, 105 – 113 (2014)

[3] Shears J. & Poyner G., JBAA, 120, 380 (2010)



[6] Leibowitz E. M. et al., Baltic Astronomy, 4, 453 - 466 (1995)

[7] Munari U., Siviero A., Ochner P., & Dallaporta S., The Astronomer's Telegram, No. 9418 (2016)


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BAA Articles

Observer's Challenge – Occultation of M44 the Beehive Cluster by the Moon

Date: 2019 April 13th
Start Time: 2000 UT (2100 BST) to 2300 UT (Midnight BST)

On 2019 April 13th, a 62% illuminated waxing gibbous Moon will pass south of the Beehive Cluster (also known as M44) in the constellation of Cancer. From around 2000 UT (as the sky is starting to get darker) to 2300 UT, the Moon will pass in front (i.e. occult) a number of stars in the cluster (see Figure 1)

For those people who attended the Winchester Weekend on 5th-7th April, you will remember that this was one of 'Pete and Paul's Observing challenges'. Even if you weren't at Winchester, this is a lovely event to watch and requires only a pair of binoculars or a small telescope to view.

There are three stars that are in easy range of binoculars or a small telescope to watch out for and these are:

  • HIP 42327, a mag +6.7 star which will reappear from the bright limb at about 2025UT
  • HIP 42542, a mag +6.8 star which is occulted at 2040UT and re-appears at 2126UT
  • TYC-1395-2321-1, a mag +7.8 star which is occulted at 2045UT and re-appears at 2148UT

Figure 2 shows the location of these stars in the Beehive Cluster. The times given here will vary a little depending upon your location in the country. There are a number of free planetarium software now available which you can use to find out the timings of the occultations from your location.

Paul G. Abel

Please do post any observations of this to your BAA Member Page

[Thumbnail image taken from Stellarium]

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BAA Tutorials Intermediate

Filters for visual observing of the Moon and planets


If you are new to astronomy and wish to see as much detail as possible on the planets of the solar system, or even if one has been observing solar system objects for some time, it may come as a surprise to find that coloured filters can make a world of difference to your observing clarity. Using filters can revolutionize your observing as coloured filters bring out additional detail from the subtle shadings found on solar system objects. This tutorial builds on the excellent tutorial by Paul G. Abel, and looks in more depth at the filters most commonly used by visual observers of solar system objects.

Many astronomical suppliers provide these filters, and all filters are identified firstly by their colour, and secondly by particular numbers or a # which are known as Wratten numbers. These allow the observer to choose which parts of the spectrum they are going to enhance in order to make planetary and lunar definition stand out. The principle of the filters come from black and white photography in which complementary or “opposite” colours enhance the contrast visible. When juxtaposed, complementary colours make each colour seem more vivid and defined, enabling particular coloured features to stand out against the background hues. So, a red or orange filter will enhance blue features and a blue filter will enhance red features.

The Wratten system was developed in Britain in the early 20th century by Frederick Wratten and Kenneth Mees who founded a company in 1906 that produced gelatin solutions for photography. Mees then developed gelatin filters dyed with tartrazine to produce a yellow filter, but soon developed other colours and a panchromatic process of photography. In 1912 they sold the company to the American company Kodak, with their British offices at Harrow in England and Mees moved to New York to found the Eastman-Kodak laboratories there. In honour of his partner and mentor, Kenneth Mees named the burgeoning number of coloured filters “Wratten” and introduced the complex numbering system that is still in use today. Not all the Wratten filters are suitable for astronomical use, but the main colours are still widely used in visual astronomy and are detailed in this tutorial.

These coloured filters are known as broadband or “longpass” in that they allow a wide range of wavelengths through but block wavelengths above or below a certain point in the electromagnetic spectrum. As the spectrum of visible light lies between 390 and 700 nanometers (nm), with the blue wavelengths being the shortest (~400nm) and the red being the longest (~700nm). Anything with a wavelength range above or below a particular filter will be blocked and increased contrast in compensating colours will be noticed.

Most astronomical suppliers sell complete sets of filters for solar system observing and naturally such sets are known as lunar and planetary filters. They generally have a range from red to blue across the spectrum and cover the broad bandwidths associated with such colours. A typical set will include a neutral density filter for lunar observing and a No. 25 red, No.12 yellow and No. 80A blue for as full coverage as possible. A typical filter set is shown here in figure 1. A more extensive set of astronomical filters with typical Wratten numbers can be seen here in figure 2.

This tutorial will introduce each filter and instruct the reader on which targets in the solar system each filter can be used and what features the filters will enhance Keep in mind that visual acuity does vary from observer to observer and that in the dark the sensitivity of the human eye shifts to the blue end of the spectrum. This is due to a phenomenon known as the Purkinje effect, named after the Czech doctor who discovered that the spectral sensitivity of the human eye does not enable red light to be seen clearly in the dark, but shorter blue wavelengths are detected.

Technical aspects of Filters
Filters can be separated into a few main groups that enable enhancement, lessened contrast or can be used for colour shift or balance. Colour subtraction filters work by absorbing certain colours of light, letting the remaining colours through. They can be used to demonstrate the primary colours that make up an image or can be seen in the features of our planetary neighbours. A colour correction filter makes a scene appear more natural by simulating the mix of colour temperatures that occur naturally, and subtly enhancing the middle ranges of the spectrum.

In addition to these filters, there are also colour temperature filters. Some filters change the correlated colour temperature of a light source. They can change the appearance of light from a bright white source so that it looks more yellow and natural to the eye. The term colour temperature comes from the natural phenomenon of coloured light emitted by warm objects. Warm objects, such as a flame from a fire, emit deep red and orange light. The temperature of such flames are roughly 1500K. If you increase that temperature the light emitted begins to look more blue as its wavelength changes to the shorter (hotter) or blue end of the spectrum.

Of course, optical filters don’t really change the temperature of the object emitting the light. Colour temperature filters simply remove some of the light of wavelengths of our choosing so we can absorb or reflect away some of the orange and red light emitted by the planets. This makes the remaining light look more blue and therefore has a higher colour temperature. Conversely, some filters can remove some of the blue light emitted by a planet, making the remaining light look more orange and thus apparently emitting a lower colour temperature.

Wratten filters and their uses
In the following tutorial, I have grouped the filters under their colour designation rather than put them in number order, as the colour of each filter is their most obvious feature when using them. All of these filters are available to purchase in 37.1mm (1.25”) or 50mm (2”) fittings and are commonly available from astronomical suppliers. For a fuller description of Wratten filters, please follow this link: In this tutorial, only those filters useful to astronomers will be described.

One question commonly asked is "do filters block out too much light and make observing more difficult or less enjoyable?" It is true that filters do block out some light, but I hope you will see from this tutorial that by selectively blocking out certain wavelengths of light, and by altering the contrast of any surface features, the observer is often able to resolve finer or more subtle detail. In fact, in the case of bright objects the reduction in light transmission is an advantage. Let us examine this a little more technically.

The difference in contrast between the belts and zones on an object such as Jupiter can be so small that the human eye and brain just smear the whole and it can be difficult to discern details without a filtered system. Because Jupiter is a very bright object seen against a dark background, the differences in intensity of reflected light from light/dark zones on such planets is not really seen to advantage by the human eye.

Contrast in any system can be measured using the formula:

C = (b2 - b1) ÷ b2

Where C is the contrast and b1 and b2 are different areas of brightness on the surface of a planet. Bright areas on Jupiter have an intensity of 6 lumens  m-2 and the intensity of the darker zones have an intensity of 3 lumens m-2. This would give:

(6 – 3) ÷ 6 = 0.5

or a visual contrast 50% lower in the darker zones than in the brighter zones. A filter will enhance the contrast by permitting wavelengths representative of the redder or darker zones through whilst diminishing the blue contrast on the brighter zones. Surely a filter that would aid in the perception of subtle features is going to be a bonus to any observer?

This tutorial will convincingly show that the use of filters, despite their decrease in light transmission is actually very useful in visual astronomy. The use of filters assists primarily in enhancing contrast initially and although the reduction in light transmission is generally not favoured in astronomy, this is one area in which this general rule need not apply.

No. 25 Red
The No. 25 filter reduces blue and green wavelengths, which when used on Jupiter or Saturn, result in well-defined contrast between some cloud formations and the lighter surface features of these gas giants. However, it needs to be used judiciously as the light transmission is only 15% but for such bright planets this filter will enhance the observed detail even when used with small telescopes. This filter blocks light shorter than 580nm wavelength. This filter is also sometimes referred to as a Wratten 25A.

No. 23A Light Red
This is a good filter for use on Mars, Jupiter, and Saturn, and has proved useful for daylight observations of Venus as it has a 25% light transmission. The light red is an “opposite” colour to blue and therefore darkens the sky very effectively in daylight. Some astronomers report that it also works well on Mercury, but I would not recommend viewing this planet in general during daylight due to its proximity to the Sun. This filter blocks wavelengths of light shorter than 550nm.

No. 21 Orange
This orange filter reduces the transmission of blue and green wavelengths and increases contrast between red, yellow and orange areas on planets such as Jupiter, Saturn and Mars. It brings out the glories of the Great Red Spot on Jupiter very well under conditions of good seeing with a medium magnification (e.g. x100). It also blocks some glare from the bright planet and provides less of a contrast between a planet and the black background of space. A good all round planetary filter as it transmits about 50% of the light and blocks wavelengths short of 530nm.

No. 8 Light Yellow
This filter can be used for enhancing details in red and orange features in the belts of Jupiter. It is also useful in increasing the contrast on the surface of Mars, and can under good sky conditions aid the visual resolution on Uranus and Neptune in telescopes of 250mm of aperture or larger. The No. 8 cuts down glare from the Moon and works much better than the “moon filters” included with some cheaper telescopes. This filter allows 80% of the light through but blocks light short of 465nm.

No. 12 Yellow
This filter works on the principle of opposites described above, blocking the light in the blue and green region and making red and orange features on Jupiter and Saturn stand out clearly. Deeper in colour than the No. 8 filter, it is the filter most astronomers recommend for visual work on the gas giants. It has a 70% light transmission and cancels some of the glare on Jupiter when seen against a dark background sky. It blocks visible wavelengths short of 500nm.

No. 15 Deep Yellow
This filter can be used to bring out Martian surface features, especially the polar caps and can be used to bring out detail in the red areas of Jupiter and Saturn. Some astronomers also have reported some success using this filter to see low-contrast detail on Venus. I have used this filter on Venus during the day to add more contrast to the image and it generally works well. This filter is particularly useful for visual observations of Venus as it is a very bright object and the filter can considerably reduce the glare of this very bright planet in evening or morning apparitions despite its 65% light transmission. The No 15 blocks light short of 500nm.

Although at this point it may feel like every filter suits Jupiter and Saturn, the variegated nature of their surfaces and their extreme brightness at opposition or during favourable apparitions enables a wide range of filters to bring out different details. Some of the details may be subtle, but can be explored better by an experienced observer equipped with a range of filters.

No. 11 Yellow-Green
This darker filter is a good choice to enable the observer to directly see surface details on Jupiter and Saturn. It can also be useful on Mars if you are using a large aperture telescope in the 250mm range. At times of steady atmospheric seeing, this filter darkens the surface features and makes areas such as Acidalia and Syrtis Major stand out and the polar caps and occasional features such as clouds appear quite marked. The No. 11 filter allows 75% light transmission can be used to darken some features on the Moon.

No. 56 Light Green
I have used this filter for observing the ice caps of Mars during its close encounter in 2003 and found that despite the low altitude of Mars from the UK during that apparition the filter worked well in bringing out these features and even hinted at rocky features on the planet’s surface during periods of clear seeing. I have to admit that the orange No 21 filter did work surprisingly well in rendering colour and detail on the red planet, but the contrast with the No 56 filter was quite good. This filter allows most wavelengths through but does have a peak around 500nm.

With its 50% light transmission this filter is a favourite of lunar observers as it increases the contrast while reducing the glare. It is also a filter that is well tuned to the wavelengths of the human eye and the greenish cast can almost be ignored during visual observation. This is a colour correction filter with all wavelengths equally affected. The effect can be seen on the first quarter moon in figure 3 photographed here in ordinary white light and then through the Wratten No 56 filter.

No. 58 Green
This filter blocks red and blue wavelengths of light and many observers find that it slightly increases contrast on the lighter parts of the surface of Jupiter. I have also used it on Venus where it does add to the contrast and reduces glare a little but it must be admitted that it is not easy to visualize any detail in the clouds.

The No 58 filter has a 25% light transmission, and it is a colour correction filter rather than a longpass. Such filters alter the colour temperature of the incoming light, enhancing contrasting colours in the object by allowing specific wavelengths through that correspond to the temperature of the light. This is a complex subject but to put it simply, the colour of light not only corresponds to particular wavelengths but also to particular colours where blue is cooler and red is hotter. Note that this is more of a perception than anything else as in reality blue light is “hotter” (has a higher frequency and shorter wavelength) than red light.

No. 82A Light Blue
This is almost a multipurpose filter as it does enhance some features on Jupiter, Mars and Saturn and also works very well in enhancing some features on the Moon (figure 4). It is commonly referred to as a “warming” filter that increases the colour temperature slightly and allows the red wavelengths through due to the complementary colours that we discussed above. With a light transmission of 75% it can be used on any aperture telescope and can even make some difference to deep sky objects such as M42 and M8 though the effects can be quite subtle. 

No. 80A Blue
Although this is quite a dark filter, it is as versatile as the No 82A in that it enhances features in the red on planets such as Jupiter, Saturn and Mars. It is also good for lunar observation as it reduces the glare and provides good contrast for some features such as ejecta blankets, ray systems and lava fronts. Some astronomers report success in its use on binary star systems with red components such as Antares and α Herculis as the contrast enables the observer to split the two components well. The No. 80A filter has a 30% light transmission and also acts as a colour conversion filter enhancing wavelengths around 500nm.

No. 38A Dark Blue
Again, a good filter to use on a planet such as Jupiter because it blocks red and orange wavelengths in such features as the belts and in the Great Red Spot. Some astronomers report that it also adds contrast to Martian surface phenomena, such as dust storms, and makes a better contrast for observing the rings of Saturn. Try using it for observations of Venus as some report that using this filter increases the contrast, leading to the visual observation of some dusky cloud features. This filter has about a 15% light transmission. It absorbs red, green and UV light and is commonly referred to as a minus green, plus blue filter. The difference can be gauged in figure 5.

No. 47 Violet
A very dark filter which strongly blocks the red, yellow, and green wavelengths. I would highly recommend it for Venus observation due to its low light transmission of about 5% providing great contrast and enhancing cloud features. Try using it on the Moon to decrease the glare when observing features at a 10-12 day old phase. Some observers report that features in the Schroeter Valley and Aristarchus crater are clearer due to the lack of glare. Recommended for the Moon, especially if you are using a large aperture telescope! This is another colour separation filter that enhances the blue or shorter wavelengths of the spectrum at 450nm.

Additional filters that also are helpful in visual observing are the polarizing filter and the neutral density filter. Both are longpass filters that usually transmit all wavelengths of light but can cut down on glare and contrast.

Non Wratten Filters
Neutral Density Filters
A neutral density (ND) filter transmits light uniformly across the entire visible spectrum and is an excellent filter to use to reduce glare in such objects as the Moon and planets, but especially the Moon. Due to its bright glare many lunar and planetary astronomers keep an ND filter on their favourite eyepiece and add on other filters as necessary. Neutral density filters come in a variety of densities that reduce the glare in the image based upon the amount of light transmission each ND filter allows. Commonly they come in numbers such as 50, 25 and 13 that signify the amount of light they transmit; 50%, 25% or 13%.

Polarizing filters
Although it does not work at any specific wavelength, the polarizing filter allows light of any wavelength through but blocks those with random scattering patterns allowing only light waves in a flat “plane” through, which has the effect of increasing the contrast, reducing glare and slightly enhancing the saturation of colour in an object. Such filters are very useful on bright objects such as the Moon and some planets.

Neodymium Filter
The Neodymium filter is an interesting addition to the filter armoury as it filters the yellow light of the spectrum, rendering most objects a faint blue colour. It is useful for observations of Venus and for Jupiter and Saturn too. Some astronomers report that this is a useful filter for observing in light polluted areas as it cuts through sodium light pollution somewhat, although it is not as effective as a Light Pollution Reduction filter.


Many planetary observers rely on filters and they report that they really do make a difference in seeing faint details. Filters also reduce the glare of objects like Jupiter, Saturn and the Moon and render a better contrast between their sunlit surface and the dark background sky.

Observers can also be affected by a phenomenon known as prismatic or atmospheric dispersion. This is most evident when a star or planet is seen near the horizon. It results from atmospheric refraction occurring less for the longer wavelength red light where the red appears clearer nearer the horizon and the light shifts to the violet toward the zenith. This is the reason that most astronomers prefer to observe an object when it is near or at culmination (the highest point in the sky as seen from an observers latitude) so that this effect is lessened. Use of red or blue filters on an ascending object may make the difference between seeing details such as the Great Red Spot for example.

I hope that this tutorial shows that coloured filters are a very useful tool in visual astronomy. Using such, I hope that this tutorial gives the reader some tips on which filters to use to observe any of the planets of the solar system and our moon. Most features on planetary surfaces may be quite subtle and filters can make a great difference between seeing or recording a feature or missing it completely in the sky background. For more information on using filters for visual observing or for astrophotography, please see my book Choosing and Using Astronomical Filters.

Martin Griffiths

Martin is the Director of the Brecon Beacons Observatory and an astronomer at Dark Sky Wales

[The graphical plots in this tutorial have been prepared using copyright free spectroscopic data]

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BAA Observing Sections Comet

Comet 21P approaches the North America Nebula

It will be a challenging observation due to midsummer skies and a First Quarter Moon but the periodic comet 21P/Giacobini-Zinner will be passing the bright emission nebula NGC7000 (the North America Nebula) in Cygnus between June 19 and June 21. The comet is currently around 13th magnitude but will brighten over the summer to become a potentially 6th magnitude object by September. At present the comet is a small fuzzy spot with a short tail to the south west and it will be completely overwhelmed by the large nebula but it will be interesting to compare the two objects. A chart showing the encounter is here. Please send any observations to the Comet Section.

The image at left shows the comet on the morning of 2018 June 13. The field of view is around 11 arcmin square. More images of this comet are available in the Section's archive here.

Update on 2018-06-18 - Here is an image of the comet approaching the nebula taken from New Mexico.

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BAA Tutorials Starting out

Noctilucent Clouds – a beginners guide

Noctilucent clouds (popularly referred to by the abbreviation “NLC”) are high atmosphere clouds which occur over summertime at mid latitude locations. They form at very high altitudes – around 82 km above sea level – and are, thus, a quite separate phenomena from normal weather or tropospheric cloud. They appear as thin streaks of “cloud”, often a pearly-blue colour, reminiscent of “mares-tail” cirrus cloud formations.

NLCs can be seen from around mid May to early August during the darkest part of a summer’s night when the Sun is between 6 – 16 degrees below the horizon. Typically, they will occupy the northern horizon, along the twilight arch, extending to an altitude of 10 – 15 degrees. Over the NLC “season” the bright star Capella dominates this part of the sky and serves as a good marker for the NLC observer. They used to be associated with northern UK but have been seen as far south as central France and they seem to be spreading further south with each season.

Observations of NLC remain of great value to professional scientists studying upper-atmosphere phenomena. Useful observations are very easy to make and require no special equipment.

The following information lists the important details you should include in your report:

LOCATION: Give the latitude and longitude of the place observations were made. Alternatively, give the name of the nearest town or city.
DATE: Use the “double-date” convention as used in reporting aurorae. That is, “June 21-22″ would refer to the night of the 21st and the early hours of the 22nd.
TIME: Try to use universal time (UT) even though British Summer Time (BST) will be in civil use for UK observers. Remember, UT = GMT = (BST – 1 hour).

The following features and details should be recorded at 15 minute intervals (i.e. on the hour, quarter past, half past and so on):

AZIMUTHS If you see NLC measure the left (western) and right hand (eastern) extent of the display. This is measured in degrees with west = 270, north = 000, east = 90 and south = 180. Polaris defines the northern point of your horizon. Azimuths can be gauged by using a clenched fist, held at arms length, as a measure of 10 degrees.
ELEVATION If possible, measure the angle subtended by the uppermost part of the display. A simple alidade can be made from a protractor and plumb line for this purpose.
BRIGHTNESS NLC brightness is measured on a three point scale with 1 = faint; 2 = moderate; 3 = very bright.

NLC forms are classified into 5 easily identified structures. Any combination of the following is possible:

Type 1: Veil – A simple structureless sheet, sometimes as background to other forms.
Type 2: Bands – Lines or streaks, parallel or crossing at small angles.
Type 3: Waves – Fine herring-bone structure like the sand ripples on a beach at low tide. Very characteristic of NLC.
Type 4: Whirls – Large-scale looped or twisted structures.
Type 5: Amorphous – Isolated patches of NLC with no definite structure.

Simple sketches of the NLC can be very useful. These are best made in negative form with the darker parts of the sketch corresponding to the brighter NLC.

Photographs of NLC can easily be taken with a digital camera firmly fixed to a tripod; using 400 ISO gives good results. An exposure of 3-6 seconds with a lens aperture setting of f3.4 will normally suffice. However, it is always best to take several shots of different exposures, and pick the best exposure. Once this is done you can try a panorama by taking several overlapping photos. Make sure the camera is level, then move it about 20 degrees after each shot, starting just beyond one end. This makes sure that you will get it all, because the camera will see more than you can.

Sandra Brantingham

Sandra is the Director of the Aurora and Noctilucent Cloud Section of the BAA.

A selection of observatorions of noctilucent clouds which BAA members have uploaded to their Member pages can be found here.

[Thumbnail image by Gordon Mackie]

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