Tri-band and other narrow band imaging of emission nebulae with a colour camera

Narrow band filters, be they Dual-Band, Tri-band or Quad-Band filters enable images of emission nebulae to be captured using colour cameras under light polluted skies.

Emission nebulae are objects such as star formation regions like M42, the Orion Nebula, Planetary Nebula such as M27, the Dumbbell Nebula, and Supernova Remnants such as M1, the Crab Nebula.  These emit much of their light in four wavelengths, those of the Hydrogen Alpha (H-alpha) and  Hydrogen Beta (H-beta) spectral lines, two close Oxygen III lines and the Sulphur II spectral line.

These are often imaged using monochrome astro-cameras and a set of narrowband filters but it is both expensive to buy the suitable filters and somewhat complex  to make separate images through them and the combine the resulting images. Although, in principle, it does not take more time as mono cameras are more efficient with all pixels in use for each band.

Many astroimagers now use colour cameras; either colour astro-cameras or DSLR and mirrorless cameras that have been modified to be more sensitive (from 25% to ~95%) at the red H-alpha wavelength.  For imaging these objects from urban environments, one can now buy a variety of filters to pass two or more of these spectral line wavelengths but which greatly reduce the effects of sky glow either from terrestrial light pollution or moonlight.

The strongest lines are that due to H-alpha in the red and O III in the green parts of the visible spectrum.  Less strong is the H-beta line in the blue-green with the weakest being the Sulphur II line in the deep red.

At a cost of near £1,000 it is possible to acquire a ‘quad-band’ filter that has very narrow band passes at all four spectral lines.  This will essentially eliminate all sky glow and is, perhaps, the perfect choice.

Under very light polluted skies an excellent filter, at a cost of £179, would be the Optolong L-eXtreme dual band filter which employs two very narrow, 7 nm, bands to select just the O III and H-alpha spectral lines and which will also remove virtually all sky glow.

One can also purchase ‘Tri-Band’ (from ~£139 upwards for 2″ filters) or ‘Quad-Band’ (from ~£160 upwards for 2″ filters) filters such as those sold by Altair Astro (AA) in the UK.  Pedantically, one could argue that neither title is correct as both have only two pass bands.  Neither does ‘Tri’ or ‘Quad’  define the number of spectral lines acquired.   As seen in the diagram below, Tri-Band filters have a narrow pass band to select the H-alpha wavelength and a broader pass band which passes the two O III wavelengths along with the H-beta line.

In the case of the Quad-Band filter, the band in the red part of the spectrum is broadened so that it also encompasses the S II wavelength.  They do, however, correctly define the number of elements whose spectral lines are captured.

The total bandwidth of the AA Tri-Band filter is 47 nm compared to the visible bandwidth of from ~400 nm to ~700nm, so some 300 nm wide.  Given that the LED street lights in use are now are full spectrum, the amount of sky glow captured from them when using the filter should be significantly reduced as would also be the case when imaging in moonlight.  Perhaps it should be pointed out that if imaging from a very dark site with no Moon, such filters would not be needed.

A similar ‘Tri-Band’ filter is the IDAS N-1 filter costing £189.

An imaging example – the Witch’s Broom Nebula

This is part of the Cygnus Supernova remnant and lies adjacent to the star 52 Cygni.  This was the first object that I chose to image having acquired the AA Tri-Band filter.  The sky transparency was very poor so that the effects of light pollution were very marked.  It was, however, close to New Moon.  Using the ‘Blackwater Skies’ field of view calculator I found that it would be nicely encompassed when using a Teleskop Service (TS) 90 mm, f/6.6, triplet refractor allied to the Altair Astro 294c PRO cooled colour camera employing a Micro 4/3 sensor.  The superb TS 2″ field flattener was employed to remove the effects of field curvature.  This combination is capable of producing superb images showing no obvious chromatic aberration and pinpoint stars across the field – as that shown of the region surrounding Vega below.

A total of 211, 30 second exposure, ‘light’ frames were taken followed by 20, 30 second exposure, ‘dark’ frames.  Both sequences taken at a temperature of -15 Celsius.  No bias frames were required as both the exposure time and sensor temperature were the same.  With the 4/3 sized sensor, no ‘flat’ frames were required either.  The Astro-Physics mount’s tracking easily allows for up to 60 second exposures without guiding and, for these exposures, the image was moving across the sensor by  ~0.2 arc seconds during each exposure and so not materially affecting the sharpness of the single frames.

I aligned and stacked the light and dark frames using two programs; Deep Sky Stacker and Affinity Photo (a superb low cost program!).  Affinity Photo is quite processor intensive but, using an i7 desktop processor, it was able to stack the 211 frames in 5 minutes – having rejected three frames.  The AA 294c accentuates the green part of the spectrum hence the prominent green cast. Some evidence of the nebula is visible beneath the sky glow.

Comparing the stacked result from the two programs, it was apparent that the image of the bright star, 52 Cygni, was ‘tighter’ in the Affinity Photo result and so this was used for further processing.

Using the ‘Info’ tool it was possible to see that the sky glow was uniform across the field – perhaps not too surprising as the nebula was being imaged at high elevation.  This made it very easy to remove: the image was duplicated to give two layers, the upper layer was smoothed using a Gaussian Blur of 40 pixels, the paint brush was used to select the colour away from the nebula regions and then to paint the whole layer with this colour before, finally, the two layers were flattened using the ‘Difference’ blending mode.

The use of ‘levels’ or curves can then be used to lift up the fainter regions of the image to give the following result. 

In the Digest there is an article entitled ‘Using Starnet++ to help enhance Nebulae images‘ that describes how this program can separate the image into two; that containing just the nebula and that containing the stars as seen below.

The Nebula Image
The stars image

It is then possible to enhance the nebula using the ‘Unsharp Mask’ filter with a large radius and small amount and the ‘Smart Sharpen’ filter with a small radius and an amount adjusted to suit. 

The Nebula image

The ‘stars’ image in then overlaid over the enhanced nebula image and the two flattened using the ‘Screen’ blending mode to give the final result.

I was quite pleased with this image but was, in one respect, confused.  The OIII spectral line is towards the blue end of green and is stronger than the H-beta spectral line.  The colours of the nebula should thus be red, the H-alpha spectral line, and ‘teal’, the blue-green combination of the O III and H-beta spectral lines just as is shown in my image.   However, the majority of the images that one finds on the WEB show blue nebulosity where my image shows teal.  This cannot be correct.  It may be what is produced when using  a monochrome camera and  narrowband filters – though observing a white light source through my O III filter the image is definitely green.  I suspect that the blue-red combination is more attractive and so imagers have ‘adjusted’ the image colour to suit and are wrongly guided by what they see on the WEB.  I have posted my query into a ‘Cloudy Nights’ forum and the consensus is that the colours shown in the image above are correct.