Has graphene been detected in space?

Planetary nebulae originate from stars similar to our sun that have reached the end of their lives and are shedding shells of gas into space. In this case, the planetary nebulae are located in the Magellanic Clouds, two satellite galaxies to our own Milky Way, that are best seen from the Southern Hemisphere. At the distance of the Magellanic Clouds, planetary nebula appear as small fuzzy blobs. However, unlike planetaries in our own Milky Way Galaxy whose distances are very uncertain, the distance to planetaries in the Magellanic Clouds can be determined to better than 5%. With such accurate distances, the research team determined the true luminosity of the stars and confirmed that the objects are indeed planetary nebulae and not some other object in the astrophysical zoo.

Fullerenes, or Buckyballs, are known from laboratory work on earth, and have many interesting and important properties. Fullerenes consist of carbon atoms arranged in a three dimensional sphere similar to the geodesic domes popularized by Buckminster Fuller. The C₇₀ fullerene can be compared with a rugby ball, while C₆₀ is compared to a soccer ball. Both of these molecules have been detected in the sample. Graphene (planar C₂₄) is a flat sheet of carbon atoms, one atom thick, that has extraordinary strength, conductivity, elasticity and thinness. Cited as the thinnest substance known, graphene was first synthesized in the lab in 2004 by Geim and Novoselov for which they received the 2010 Nobel Prize in physics. "If confirmed with laboratory spectroscopy – something that is almost impossible with the present techniques – this would be the first detection of graphene in space," said team member García-Hernández.

The team has proposed that fullerenes and graphene are formed from the shock-induced (i.e., grain-grain collisions) destruction of hydrogenated amorphous carbon grains (HACs). Such collisions are expected in the stellar winds emanating from planetary nebulae, and this team sees evidence for strong stellar winds in the ultraviolet spectra of these stars. “What is particularly surprising is that the existence of these molecules does not depend on the stellar temperature, but on the strength of the wind shocks” says Stanghellini.

The Large Magellanic Cloud Planetary Nebula SMP48, one of the star systems in the present study. The reason for the name “planetary nebula” is obvious from this image of a planetary nebula, which is much fainter and further away than the first ones seen in our galaxy. Image credit: HST

The Small Magellanic cloud is particularly poor in metals (any element besides hydrogen and helium, in astronomers’ parlance) but this sort of environment favors the evolution of carbon rich-planetary nebulae, which turns out to be a favorable place for complex carbon molecules. The challenge has been to extract the evidence for graphene (planar C₂₄) from Spitzer data. “The Spitzer Space Telescope has been amazingly important for studying complex organic molecules in stellar environments,” says Stanghellini. “We are now at the stage of not only detecting fullerenes and other molecules, but starting to understand how they form and evolve in stars.” Shaw adds “We are planning ground-based follow up through the NOAO system of telescopes. We hope to find other molecules in planetary nebulae where fullerene has been detected to test some physical processes that might help us understand the biochemistry of life.”

The accompanying image includes an artist’s conception of these molecules superimposed on the well known Helix Nebula. The smaller image shows one of the objects from this study in which fullerene has been detected in the Large Magellanic Cloud (SMP 48, from the catalog by Sanduleak, MacConnell, & Philip) The name “Planetary Nebula” was applied to these star systems because their shell of surrounding gas made them appear like the disks of Jupiter, Saturn and Uranus as observed in 18th century telescopes. The reason for this name is obvious from the modern image.

More information: These results are presented in a paper published by the Astrophysical Journal Letters, Volume 737, Issue 2, article id. L30 (2011) The team includes D. A. García-Hernandez, S. Iglesias-Groth, J. A. Acosta-Pulido, A. Manchado, P. García-Lario, L. Stanghellini, E. Villaver, R. A. Shaw and F. Cataldo

Provided by National Radio Astronomy Observatory