Hydrocarbons in the Horsehead mane (21 February 2005)

Observing the edge of the famous Horsehead Nebula with the IRAM interferometer located on the Plateau de Bures (France), a team of French and Spanish astronomers discovered a large quantity of small hydrocarbon molecules. This is a surprise because the intense UV radiation illuminating the Nebula should destroy the small hydrocarbons near the edge. The astronomers suggest that these molecules might result from the fragmentation of giant molecules, called “polycyclic aromatic hydrocarbons” (PAHs).

 

More than 120 molecules have been observed in the interstellar medium, of which about twenty are small hydrocarbons. These hydrocarbons are an important component of the interstellar chemistry as they furnish a carbon skeleton needed to build more complex molecules. However, these small hydrocarbons are easily broken apart by the UV radiation from young stars. Therefore, astronomers try to understand how these molecules are regenerated in spite of their destruction by UV radiation.

In addition to these small hydrocarbons, giant molecules, called polycyclic aromatic hydrocarbons (PAHs), were detected in the early 1980’s, at infrared wavelengths. PAHs are aggregates made of tens to hundreds of mainly carbon and hydrogen atoms. Previous theoretical studies suggested that radiative fragmentation of the PAHs lead to small hydrocarbons. Jérôme Pety (IRAM, France) and his colleagues [1] have now provided one major step toward validating this theoretical hypothesis. They observed the famous Horsehead Nebula with the IRAM Interferometer (Plateau de Bures, France) [2], to search for hydrocarbons and to compare their location with that of PAHs detected a few years ago with the ISO satellite in the same region.

The Horsehead Nebula is one of the most famous and easily-recognizable shapes in the sky. In addition, for astronomers, its light-bathed silhouette is above all a fantastic interstellar chemistry laboratory where high density gas and stellar light interact. More precisely, the Horsehead appears as a dark patch against a bright region (named IC 434). It also undergoes strong ultraviolet radiation that mainly comes from the nearby star σ Orionis. Thanks to the high spatial resolution of the IRAM interferometer, the team was able to explore the edge of the nebula, “the horse mane”, where the gas density increases and the temperature and illumination decrease within a few hundredths of a light-year.

The team discovered three small hydrocarbons (C₂H, C₃H₂, C₄H) in the illuminated edge of the nebula. The abundance of these molecules is close to that measured inside interstellar dark clouds. The team was very surprised by the high abundance of C₂H, C₃H₂, C₄H in the Horsehead “mane”: these molecules should be destroyed by the intense UV radiation in the edge of the nebula.

Where do the hydrocarbons come from? In their article, Jérôme Pety and his colleagues compare the places where the hydrocarbons have been detected to the places where the ISO satellite detected PAHs. The correspondence between the hydrocarbons’ and the PAHs’ sites is very good and confirms the hypothesis that the hydrocarbons come from the fragmentation of PAHs. Under strong interstellar radiation, PAHs might be eroded and free a large number of small hydrocarbons. This mechanism would be more efficient in regions similar to the edge of the Horsehead Nebula, named “photo-dissociation regions”, in which UV radiation is stronger. This scenario now has to be confirmed by laboratory experiments, such as the experimental set-up PIRENEA in Toulouse (France) [3], for the study of the chemical reactions in the interstellar medium.

In the overall picture of the Horsehead Nebula (copyright ESO), the white frame shows the region observed using the IRAM Interferometer. The upper right panel shows the emission of the C₂H molecule, which is typical of small hydrocarbon emissions. The observed C₂H emission is very similar to the PAHs emission, as observed in the same region by the ISO infrared satellite (lower right panel).

[1] The team is made of J. Pety (IRAM, Grenoble, France), D. Teyssier (Madrid, Spain), D. Fossé, M. Gerin (Paris, France), E. Roueff (Meudon, France), A. Abergel (Orsay, France), E. Habart (Firenze, Italy), and J. Cernicharo (Madrid, Spain).

[2] For additional information: http://www.iram.fr

[3]For additional information: http://www.cesr.fr/~joblin/PIRENEA/

Are PAHs precursors of small hydrocarbons in PDRs? The Horsehead case
by J. Pety, D. Teyssier, D. Fosse, M. Gerin, E. Roueff, A. Abergel, E. Habart, J. Cernicharo
Published in Astronomy & Astrophysics (DOI number: 10.1051/0004-6361:20041170)