Sample Projects

Unleash your “inner scientist!” Learn how easy it is to capture an exciting star spectrum using just just a standalone DSLR, or telescope with video camera or FITS camera.

Senior Sky & Telescope editor Dennis di Cicco talks with Tom Field of Field Tested Systems about the growing number of amateur astronomers doing backyard spectroscopy with simple equipment. “Most amateurs are astonished at how easy it is,” he says. Field also demonstrates his RSpec program, which transforms the image of a spectrum (including real-time video images) into a calibrated graph showing spectral features.

New to spectroscopy? Or already doing spectroscopy but want to do more? Watch the video below to see some of the easy projects that you can do with a small telescope:

Sample Spectroscopy Projects

The page below shows some examples of the kinds of projects that can be done with a low resolution diffraction grating, like our Star Analyser or the Rainbow Optics Star Spectroscope. With one or two clicks in our RSpec software, you can convert a standard FITS, jpg, RAW, or video image to scientific data like that below. Spectroscopy has finally become accessible to amateurs!

You can post questions about these projects on the RSpec Yahoo forums (link) or email us via our contact form (link).


Characterizing Star Types: You can use a telescope as small as 4″ or a DSLR to capture a collection of OBAFGKM spectra. When you compare them to one another, you will be able to discern differences in the absorption lines as shown below. You can also determine the star’s temperature and type by comparing their spectra to those in the RSpec Reference Library. This would make an excellent science project.

Below is a sample of some the excellent work done by Torsten Hansen, using a Star Analyser grating, an 8″ Newtonian, and just an astronomical video camera. If you have a FITS camera or DSLR, you can easily capture this kind of data!

Each row is a different star.

From top to bottom, the spectra are in temperature order. Notice for example, that the cooler stars near the bottom have some broad absorption bands in the red end of the spectrum. That’s the absorption from complex molecules that survive because the temperatures are so “low.”

Also notice, for example, that the Hydrogen Balmer (beta) absorption line at 4861 Angstroms is the strongest for the Type A star. This particular Hydrogen transition isn’t as prevalent in the hotter or cooler stars. See? There’s lots to learn here:



Different star types (OBAFGKM) are clear visible in these spectra


Detect the Emission lines on an Emission Nebula: An emission nebula is surrounded by a gas shell that is excited (like a florescent light). Below is a spectrum of the Saturn Nebula clearly showing its emission lines. The Orion Nebula (M42) would have a similar appearance.


Emission lines of a distant nebula!


Detect the Spectrum of a Super-giant: The super-giant P-Cygni shows distinct emission lines in the image below. Notice how they differ from the Saturn Nebula above. (Credit: François Teyssier)


Emission lines of a super-giant star!


Study Star temperature and structure: The Albireo double (see inset) is of course the beautiful blue-gold showpiece that many of us are familiar with. The image below shows the spectra of its two main stars. You can easily see the energy on hotter Albireo B is concentrated in the blue end of the spectrum. And the energy of the amber star is towards the cooler red end, peaking in the amber/yellow region as expected. Notice the emission line (circled) at 6562? That’s from a glowing disk of gas around surrounding Albireo, which is a “Be” star. Wow! (Credit: Ken Whight)



The cool and hot Albireo double stars


Detect the Methane atmosphere in Neptune or Uranus: The image below by Paul Tervit shows the absorption by Neptune’s atmosphere. You can capture Neptune’s spectrum with an 8″ scope, a FITS or astronomical video camera and our Star Analyser diffraction grating.


Neptune’s atmosphere is visible as deep dips


Detect the Red Shift of a Quasar that is 2 billion light years away. William Wiethoff’s spectra (below) of QSO 3C 273 shows the red shift due to cosmological expansion. Many amateurs capture this spectrum on 8″ telescopes with less than 15 minutes integration time.

Recommendation from Tom:

“This link has a very interesting transcript of an interview with Maarten Schmidt, the discoverer of this first quasar. It’s exciting and fun to read such a personal account by a world-known professional.

He describes in simple terms how he made is discovery and his persistence, his fear and self-doubts, jubilation, working with colleagues, and the celebration on the night of the discovery. Search the page at the above link for “December 1962″ for the relevant section. Frankly, I’ve never heard from a single visitor to our site that they followed the above link. I’d love to hear from you if you do, because it’s such a great story.”



The cosmological red shift of a quasar. 15 minute stacked with just an 8″ SCT


Measure the redshift of galaxies with a Star Analyser!

Want to measure the red shift of a galaxy? The image below shows the spectrum of Seyfert Galaxy UGC 545, a mag 14.1 galaxy with an Active Galactic Nucleus.

Not all galaxies are suitable for this measurement with a Star Analyser grating. The high luminosity of this one’s core makes it visible despite being at a significant distance from us. And the compact, almost stellar appearance allows the Star Analyser diffraction grating to be used.

Credit: Robin Leadbeater, 8″ telescope and just a webcam! Link.

Red-shift of a galaxy with a Star Analyser and 8″ telescope


Wolf-Rayet Stars: The spectrum below is a fascinating view of a Wolf-Rayet star by Janet Simpson using just a Canon 350D DSLR , 85 mm lens, 30-second exposure with AstroTrac mount. She used the Star Analyser 100 for a grating. (For mounting hints, see this link.)

Wolf–Rayet stars are a normal stage in the evolution of very massive stars, which continually eject gas into space, producing an expanding envelope of nebulous gas. Notice the wide Carbon emission bands! Their width is attributed to the Doppler effect because the gas surrounding these stars is moving with velocities of 300–2400 km/s along the line of sight.

Here’s what Wikipedia has to say about Wolf-Rayet stars:

“The characteristic emission lines are formed in the extended and dense high-velocity wind region enveloping the very hot stellar photosphere. This produces a flood of UV radiation that causes fluorescence in the line-forming wind region. This ejection process uncovers in succession, first the nitrogen-rich products of CNO cycle burning of hydrogen (WN stars), and later the carbon-rich layer due to He burning (WC & WO stars). Most of these stars are believed finally to progress to become supernovae of Type Ib or Type Ic.” (Credit: Wikipedia link)

Yes, it doesn’t take a ton of gear, skill, and dark skies to capture fascinating spectra like this one! It’s images like this that we find so enormously exciting.



The carbon emission near the core of a Wolf Rayet star


Solar Spectroscopy: If you work with the sun, you can have fun doing astronomical spectroscopy and still get a good night’s sleep! Use a ball bearing or a sewing needle with a dark backdrop to get a spectrum of the sun. Be careful of your eyes. Never look directly at the sun or its reflection.

David Haworth has published a creative and inexpensive apparatus that you can easily build to capture spectra of the sun. (For details, see his site: link.)


Using a sewing needle to capture a solar spectrum


The above spectrum, when processed in RSpec, clearly shows the sun’s Fraunhofer lines:


The Sun’s Fraunhofer lines


Changes in a variable LL Lyr star: This wonderful animation is just one evening‘s worth of images. Done by Umberto Sollecchia in Italy with just a 110mm refractor and our Star Analyser grating. Watch how the temperature of the star changes and how the Hydrogen beta line (at 4861) and others come and go! This amazing and exciting animation by Mr. Sollecchia shows the exciting kinds of observations that can be made by amateurs with small telescopes.



Comet spectra: This spectrum of ISON shows how easy it is for amateurs to study astronomical spectra. Vikrant Kumar Agnihotri in India captured this wonderful spectrum of ISON using a just an 80 mm refractor, simple Star Analyser grating, and a DSLR. It clearly shows the green glow from glowing Carbon (the so-called “Swan bands” – Wikipedia link) This image was captured from a rooftop in Rajasthan, and then processed in the RSpec software:



The spectrum of a icy comet


Below is a great spectrum of a comet captured with a slit spectrograph. Notice the variety of complex molecules. These complex molecules are thought to have provided the raw material that formed the building blocks of life when they pelted the Earth during its early history. (Credit: Rainer Ehlert)


Comet Spectrum showing detailed composition


Supernova: Below is a wonderful spectrum of a supernova imaged by David Strange in the UK. The deep absorption marked as Silicon II is an indicator that this is a Type Ia supernova. At the time he took took this image and created the profile, David had been using RSpec for just over a week.

What continually amazes people is how little integration time is needed to capture spectra. This spectrum was captured on a 9″ SCT, with only 30 twenty-five second images! We’re not talking about hours of integration time here, nor large aperture. Dark sky sites aren’t required either – spectroscopy is considerably less affected by urban light pollution than visual imaging.



Supernova spectrum shows the fingerprint of a Type Ia

To download the original FITS image that was used to create the above profile (courtesy of David Strange), right-click this link.

To view a video that discusses how the above spectrum was calibrated, click this link.


A final comment on the above spectrum and calculation: this is jaw-droppingly exciting stuff. Imagine: a backyard telescope measuring the Doppler shift of a supernova!


Observe the changes in a supernova over a few weeks: Below is a a series of spectra taken of a recent supernova during the days and weeks after the event. These were taken with just a 4″ refractor!

Here’s the full description (pdf) as it appeared in Sky & Telescope Magazine: link.



Nova Spectrum: Below is the spectrum of Nova Del 2013. Alfred Tan captured this image in Singapore, using his just 90 mm Williams Optics APO and an Imaging Source astronomical video camera. The Hydrogen emission lines are very clear and typical for this type of nova.


The emission lines of a nova star


Study Nova Evolution: Below is a poster that was presented at the 2014 American Astronomical Society meeting. Using a Star Analyser grating and RSpec, a team at the University of Minnesota captured 44 spectra of Nova Delphini 2013 over a period of four months. Major phases of the nova evolution can readily be identified. Click on this link to download the complete poster.



Carbon Stars: Below are some wonderful image spectra showing the C2 Swan bands on several Carbon stars. Notice how much stronger the signal is in the right-hand, red end of the spectrum. Read more about Carbon stars at this Wikipedia link. Credit: Torsten Hansen with just a 20 cm (8″) telescope, a Star Analyser grating, and an astronomical video camera.


Carbon star spectra


It’s likely that you already have the telescope, camera and skill that would allow you to capture these kinds of exciting spectra! Have you always wanted to do a bit of science? Astronomical spectroscopy is surprising easy and a good way to unleash your “inner scientist.”

Gas Tube or Standard House-light spectroscopy: You don’t need to buy a telescope or expensive grating to do spectroscopy! Check out our video spectroscope: link.

Flame Emission Spectroscopy: No, it’s not astronomy either, but you can do it in the comfortable indoors during the winter! Check out our video spectroscope: link. The final portion of the video there shows how you can easily do flame spectroscopy!

Do you have an spectrum we could post here? Low Resolution spectroscopy can also be used to identify variable stars types, novae and the occasional bright super-novae (as shown above with SN2011fe). If you have samples of this kind of work, or other low resolution spectra of any type that you’d like to see posted here, contact us.

All images used with the permission of their respective authors.