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Barlow MJ, Swinyard BM, Owen PJ, et al. Detection of a noble gas molecular ion, 36ArH+, in the Crab Nebula. Science. 2013;342(6164):1343-5doi: 10.1126/science.1243582.
Barlow, M. J., Swinyard, B. M., Owen, P. J., Cernicharo, J., Gomez, H. L., Ivison, R. J., Krause, O., Lim, T. L., Matsuura, M., Miller, S., Olofsson, G., & Polehampton, E. T. (2013). Detection of a noble gas molecular ion, 36ArH+, in the Crab Nebula. Science (New York, N.Y.), 342(6164), 1343-5. https://doi.org/10.1126/science.1243582
Barlow, M J, et al. "Detection of a noble gas molecular ion, 36ArH+, in the Crab Nebula." Science (New York, N.Y.) vol. 342,6164 (2013): 1343-5. doi: https://doi.org/10.1126/science.1243582
Barlow MJ, Swinyard BM, Owen PJ, Cernicharo J, Gomez HL, Ivison RJ, Krause O, Lim TL, Matsuura M, Miller S, Olofsson G, Polehampton ET. Detection of a noble gas molecular ion, 36ArH+, in the Crab Nebula. Science. 2013 Dec 13;342(6164):1343-5. doi: 10.1126/science.1243582. PMID: 24337290.
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Science. 2013 Dec 13;342(6164):1343-5. doi: 10.1126/science.1243582.

Detection of a noble gas molecular ion, 36ArH+, in the Crab Nebula.

Science (New York, N.Y.)

M J Barlow, B M Swinyard, P J Owen, J Cernicharo, H L Gomez, R J Ivison, O Krause, T L Lim, M Matsuura, S Miller, G Olofsson, E T Polehampton

Affiliations

  1. Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK.

PMID: 24337290 DOI: 10.1126/science.1243582

Abstract

Noble gas molecules have not hitherto been detected in space. From spectra obtained with the Herschel Space Observatory, we report the detection of emission in the 617.5- and 1234.6-gigahertz J = 1-0 and 2-1 rotational lines of (36)ArH(+) at several positions in the Crab Nebula, a supernova remnant known to contain both molecular hydrogen and regions of enhanced ionized argon emission. Argon-36 is believed to have originated from explosive nucleosynthesis in massive stars during core-collapse supernova events. Its detection in the Crab Nebula, the product of such a supernova event, confirms this expectation. The likely excitation mechanism for the observed (36)ArH(+) emission lines is electron collisions in partially ionized regions with electron densities of a few hundred per centimeter cubed.

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