The Ring Nebula in 3D

Title: Studies of NGC 6720 with Calibrated HST WFC3 Emission-Line Filter Images-I: Structure and Evolution
Authors: C. R. O’Dell, G. J. Ferland, W. J. Henney, and M. Peimbert
First Author’s Institution: Department of Physics and Astronomy, Vanderbilt University, Nashville, TN, 37235

The Ring Nebula


The ring nebula. The semi-major axis runs from the upper left corner to the lower right, whereas the semi-minor axis runs from the upper right corner to the lower left.

Though any small telescope, the Ring Nebula looks like a cheerio on the sky.  It has always been the archetypal planetary nebula – the remnant of a star that has run out of fuel and thrown off its outer layers. But recent images from the Hubble Space Telescope reveal a much more complex structure than previously thought.

O’Dell et al. observed the Ring Nebula with Hubble’s Wide Field Camera 3 (WFC3).  The WFC3 camera possesses a wide variety of filters including narrow-band filters that isolate many of the brightest emission-lines of gaseous nebulae. Specifically, the team used filters centered on the He II, O III, and N II emission lines.

Let’s jump to the main conclusions of this 50-page paper.


The hot core of a planetary nebula emits ultraviolet radiation. This radiation ionizes the ejected outer layers of the nebula as they expand outward. An ionization front then propagates outward, away from the central core.  This is the classical interpretation – with a single ionization front.


O’Dell et al. found multiple asymmetric ionization fronts within the Ring Nebula. The structure may be seen in Figure 2 – there is  gas filling the central nebula, which is then surrounded by multiple rings. Let’s take a deeper look.

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Figure 2 – The observed line surface brightness along the semi-major axis.

Along the semi-major axis:

Ionized helium gas surrounds the central star.  It fills the inner nebula and is bounded 25 arcseconds from the star.  Beyond that lies ionized oxygen gas, bounded at 36 arcseconds from the star.  Finally ionized nitrogen and sulfur gases compose the main ring and are bounded at 44 arcseconds.  This is a much more complex structure than the previous picture, which had one ionization front located at 42 arcseconds only.

Along the semi-minor axis:

Ionized helium is bounded at 21 arcseconds, ionized oxygen at 28 arcseconds, and ionized nitrogen and sulfur at 33 arcseconds.  The previous picture had one ionization front located at 30 arcseconds. The multiple ionization fronts are clearly asymmetric with respect to the semi-major and semi-minor axes.

Another surprising feature are dense dark knots of gas embedded within the nitrogen ring.  These knots have resisted the blasts of stellar winds and radiation. They can be seen via their shadows – spikes of light pointing away from the bright, main ring.

Many nearby planetary nebulae have shown these knots, but their origin is still unknown.  Within the Helix nebula these knots are symmetric, suggesting that they could originate within the upper atmosphere of the precursor star. The knots within the Ring Nebula, however, are asymmetric.  The distribution of them is largely along arcs, resting along an ionization front.  They may likely be a product of ionization front instability.

The 3-D Model

O’Dell et al. created a 3-D model of the Ring Nebula, which is based both on its elliptical appearance on the plane of the sky and its velocity structure.  Here, the team relies on photometric and spectroscopic studies.

Take another look at Figure 1.  Notice that the minor axis appears much brighter than the major axis. Why? Brighter regions likely represent where the ionization fronts are tilted more nearly along the line of sight.  As such, the nebula is tilted toward Earth so that we see the ring face on.

The main ring has a fairly low velocity – the emission lines are shifted by 9 – 19 km/s.  The central core has a much higher velocity – its emission lines are shifted by 20 – 37 km/s.  These velocity measurements are drawn from the Doppler effect – we are only measuring velocity along our line of sight.  As such the central core appears to be pointing toward us, whereas the main ring is not.

The central core of Helium gas can be described as two polar lobes, which point toward and away from the observer. These lobes rest within the perpendicular main ring. We are seeing this ring face-on.

Finally, there is an outer faint halo.  This is almost certainly fossil radiation – gas that was photoionized during an earlier evolutionary state.

Figure 2. – The 3-D image of the Ring Nebula. Note that the observer is above (and a little to the left) of this image.  In a sense it is a bird’s eye view.

Figure 3. – The 3-D image of the Ring Nebula. Note that the observer is above (and a little to the left) of this image. In a sense it is a bird’s eye view.

Concluding Thoughts

O’Dell et al. presents us with an unprecedented view of the Ring Nebula.  It is no longer a simple cheerio on the sky but a complex 3-D structure of lobes and rings, with multiple ionization fronts and knots. Future studies will help us pin down the exact 3-D shape and therefore further understand the complexities of planetary nebulae – the future fate of our own Sun.

About Shannon Hall

While writing for astrobites I was a graduate student at the University of Wyoming working on exoplanet research. Previously, I graduated from Whitman College with two degrees: one in physics-astronomy and one in philosophy. I am now working toward my career goals in science journalism and education. Feel free to visit my website.


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