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ALMA detection and astrobiological potential of vinyl cyanide on Titan

Abstract:
Recent simulations have indicated that vinyl cyanide is the best candidate molecule for the formation of cell membranes/vesicle structures in Titan's hydrocarbon-rich lakes and seas. Although the existence of vinyl cyanide (C2H3CN) on Titan was previously inferred using Cassini mass spectrometry, a definitive detection has been lacking until now. We report the first spectroscopic detection of vinyl cyanide in Titan's atmosphere, obtained using archival data from the Atacama Large Millimeter/submillimeter Array (ALMA), collected from February to May 2014. We detect the three strongest rotational lines of C2H3CN in the frequency range of 230 to 232 GHz, each with >4σ confidence. Radiative transfer modeling suggests that most of the C2H3CN emission originates at altitudes of ≳200 km, in agreement with recent photochemical models. The vertical column densities implied by our best-fitting models lie in the range of 3.7 × 1013 to 1.4 × 1014 cm-2. The corresponding production rate of vinyl cyanide and its saturation mole fraction imply the availability of sufficient dissolved material to form ~107 cell membranes/cm3 in Titan's sea Ligeia Mare.
Publication status:
Published
Peer review status:
Peer reviewed

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Publisher copy:
10.1126/sciadv.1700022

Authors



Publisher:
American Association for the Advancement of Science
Journal:
Science Advances More from this journal
Volume:
3
Issue:
7
Article number:
e1700022
Publication date:
2017-07-28
Acceptance date:
2017-06-27
DOI:
ISSN:
2375-2548
Pmid:
28782019


Language:
English
Keywords:
Pubs id:
pubs:713203
UUID:
uuid:d99d6ca3-2887-464d-a984-0e5ff04700f3
Local pid:
pubs:713203
Source identifiers:
713203
Deposit date:
2017-11-06

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