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dc.creatorHargreaves, R. J.en_US
dc.creatorMichaux, L.en_US
dc.creatorLi, G.en_US
dc.creatorBeale, C.en_US
dc.creatorIrfan, M.en_US
dc.creatorBernath, P. F.en_US
dc.date.accessioned2012-07-09T19:14:06Z
dc.date.available2012-07-09T19:14:06Z
dc.date.issued2012en_US
dc.identifier2012-RF-07en_US
dc.identifier.urihttp://hdl.handle.net/1811/52267
dc.descriptionAuthor Institution: Department of Chemistry, University of York, Heslington, York, YO10 5DD, UK; Harvard-Smithsonian Center for Astrophysics, Atomic and Molecular Physics Division, MS 50, 60 Garden St., Cambridge, MA, 02138,USA; Department of Chemistry & Biochemistry, Old Dominion University, 4541 Hampton Boulevard, Norfolk, VA, 23529-0126, USA; School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK; Department of Chemistry & Biochemistry, Old Dominion University, 4541 Hampton Boulevard, Norfolk, VA, 23529-0126, USA; and University of York, Dept. of Chemistry, Heslington, York, YO10 5DD, UKen_US
dc.description.abstractSpectra of cool stars, brown dwarfs and extrasolar planets (exoplanets) contain a dense forest of lines from hot molecules. Examples include CH$_{4}$ and NH$_{3}$ in brown dwarfs and CH$_{4}$ in 'hot Jupiter' exoplanets. These observations present challenges to astronomers, who typically use databases such as HITRAN intended for room-temperature applications, to model the spectral energy distributions. We have used a novel technique to combine 'hot' emission spectra recorded for a range of sample temperatures (300 -- 1400$^irc}$C) in order to deduce empirical lower state energies of the emitted lines. We have applied this method to NH$_{3}$ in the 740 -- 2100 cm$^{-1}$ range \textbf{735} (2011) 111.} which includes the $\nu_{2}$ and the $\nu_{4}$ fundamental modes and in the 1650 -- 4000 cm$^{-1}$ range, (2012) in press.} which includes the $\nu_{1}$ and $\nu_{3}$ fundamental modes. We have estimated empirical lower state energies and our values have been incorporated into the line lists along with line positions and calibrated line intensities. This method is currently being extended to CH$_{4}$. Our results can be used directly for the simulation of astronomical spectra.en_US
dc.language.isoenen_US
dc.publisherOhio State Universityen_US
dc.titleUSING HOT EMISSION SPECTRA IN GENERATING LINE LISTS OF MOLECULES (NH$_{3}$, CH$_{4}$) FOR ASTROPHYSICAL APPLICATIONSen_US
dc.typeArticleen_US
dc.typeImageen_US
dc.typePresentationen_US


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