Interstellar molecules are branching out

The molecule, iso-propyl cyanide, was discovered in Sgr B2, a star forming region close to the center of our galaxy that is a hot-spot for molecule-hunting astronomers. The branched structure of the carbon atoms within that molecule is unlike the straight-chain carbon backbone of other molecules that have been detected so far.

The discovery of iso-propyl cyanide opens a new frontier in the complexity of molecules found in regions of star formation, and bodes well for the presence of amino acids, for which this branched structure is a key characteristic.

While various types of molecules have been detected in space, the kind of hydrogen-rich, carbon-bearing (organic) molecules that are most closely related to the ones necessary for life on Earth appear to be most plentiful in the gas clouds from which new stars are being formed.

“Understanding the production of organic material at the early stages of star formation is critical to piecing together the gradual progression from simple molecules to potentially life-bearing chemistry,” says Arnaud Belloche from the Max Planck Institute for Radio Astronomy, the lead author of the paper.

The search for molecules in interstellar space began in the 1960's, and around 180 different molecular species have been discovered so far. Each type of molecule emits light at particular wavelengths, in its own characteristic pattern, or spectrum, acting like a fingerprint that allows it to be detected in space using radio telescopes.

Until now, the organic molecules discovered in star-forming regions have shared one major structural characteristic: they each consist of a “backbone” of carbon atoms that are arranged in a single and more or less straight chain. The new molecule discovered by the team, iso-propyl cyanide, is unique in that its underlying carbon structure branches off in a separate strand.

“This is the first ever interstellar detection of a molecule with a branched carbon backbone,” says Holger Müller, a spectroscopist at the University of Cologne and co-author on the paper, who measured the spectral fingerprint of the molecule in the laboratory, allowing it to be detected in space.

But it is not just the structure of the molecule that surprised the team – it is also plentiful, at almost half the abundance of its straight-chain sister molecule, normal-propyl cyanide (n-C3H7CN), which the team had already detected using the single-dish radio telescope of the Institut de Radioastronomie Millimétrique (IRAM) a few years ago. “The enormous abundance of iso-propyl cyanide suggests that branched molecules may in fact be the rule, rather than the exception, in the interstellar medium,” says Robin Garrod, an astrochemist at Cornell University and a co-author of the paper.

The team used the Atacama Large Millimeter/submillimeter Array (ALMA), in Chile, to probe the molecular content of the star-forming region Sagittarius B2 (Sgr B2). This region is located close to the Galactic Center, at a distance of about 27,000 light years from the Sun, and is uniquely rich in emission from complex interstellar organic molecules.

“Thanks to the new capabilities offered by ALMA, we were able to perform a full spectral survey toward Sgr B2 at wavelengths between 2.7 and 3.6 mm, with sensitivity and spatial resolution ten times greater than our previous survey,” explains Belloche. “But this took only a tenth of the time.” The team used this spectral survey to search systematically for the fingerprints of new interstellar molecules.

“By employing predictions from the Cologne Database for Molecular Spectroscopy, we could identify emission features from both varieties of propyl cyanide,” says Müller. As many as 50 individual features for i-propyl cyanide and even 120 for n-propyl cyanide were unambiguously identified in the ALMA spectrum of Sgr B2. The two molecules, each consisting of 12 atoms, are also the joint-largest molecules yet detected in any star-forming region.

The team constructed computational models that simulate the chemistry of formation of the molecules detected in Sgr B2. In common with many other complex organics, both forms of propyl cyanide were found to be efficiently formed on the surfaces of interstellar dust grains. “But,” says Garrod, “the models indicate that for molecules large enough to produce branched side-chain structure, these may be the prevalent forms. The detection of the next member of the alkyl cyanide series, n-butyl cyanide (n-C4H9CN), and its three branched isomers would allow us to test this idea”.

“Amino acids identified in meteorites have a composition that suggests they originate in the interstellar medium,” adds Belloche. “Although no interstellar amino acids have yet been found, interstellar chemistry may be responsible for the production of a wide range of important complex molecules that eventually find their way to planetary surfaces.”

“The detection of iso-propyl cyanide tells us that amino acids could indeed be present in the interstellar medium because the side-chain structure is a key characteristic of these molecules”, says Karl Menten, director at MPIfR and head of its Millimeter and Submillimeter Astronomy research department. “Amino acids have already been identified in meteorites and we hope to detect them in the interstellar medium in the future”, he concludes.

Original Paper:

Detection of a branched alkyl molecule in the interstellar medium: iso-propyl cyanide, by Arnaud Belloche, Robin T. Garrod, Holger S. P. Müller, Karl M. Menten, 2014 Science, September 26 issue: http://www.sciencemag.org/lookup/doi/10.1126/science.1256678 (after the embargo expires).

Scientific Contact:

Dr. Arnaud Belloche,
Max-Planck-Institut für Radioastronomie.
Fon: +49(0)228-525-376
E-mail: belloche@mpifr-bonn.mpg.de

Dr. Robin T. Garrod,
Center for Radiophysics and Space Research,
Cornell University, U.S.A.
Fon: +1(0) 607-255-8967
E-mail: rgarrod@astro.cornell.edu

Dr. Holger Müller,
I. Physikalisches Institut, Universität zu Köln.
Fon: +49(0) 221-470-4528
E-mail: hspm@ph1.uni-koeln.de

Press Contact:

Dr. Norbert Junkes,
Press and Public Outreach,
Max-Planck-Institut für Radioastronomie.
Fon: +49(0)228-525-399
E-mail: njunkes@mpifr-bonn.mpg.de

http://www.mpifr-bonn.mpg.de/pressreleases/2014/10