190 Poster session, J27Databases of Infrared Spectra of Ethylene, Methane and Water for theVAMDC european e-infrastructureLudovic Daumont 1 , Gad Rekik 2 , D. Bonhommeau 3 , M. Rotger 4 , Vl. G. Tyuterev 5 ,V. Boudon 6 , C. Wenger 7 , M.-L. Dubernet 81 GSMA, France, ludovic.daumont@univ-reims.fr; 2 GSMA, France,gad.rekik@etudiant.univ-reims.fr; 3 GSMA, France, david.bonhommeau@univ-reims.fr;4 GSMA, France, maud.rotger@univ-reims.fr; 5 GSMA, France, vladimir.tiouterev@univreims.fr;6 LICB, France, vincent.boudon@u-bourgogne.fr; 7 LICB, France,christian.wenger@u-bourgogne.fr; 8 LPMAA, France, ml.dubernet@upmc.fr;Daumont L.Rekik G.Bonhommeau D.Rotger M.Tyuterev Vl.G.Boudon V.Wenger C.Dubernet M.-L.Ethylene is a volatile organic compound (VOC) that is present in the Earth troposphereas a pollutant, produced by road traffic and biomass fires [1]. It is also present in theatmosphere of giant planets [2], of Titan [3] and possibly of exoplanets like GJ436b [4].However, present data bases (HITRAN, GEISA …) contain too few C 2 H 4 lines, whosespectrum is poorly simulated. We presently work on the analysis of the bending tetradin the 10 microns region as well as on the (ν 9 /ν 11 ) C–H stretch dyad in the 3 micronsregion.Methane is a key species in many atmospheric environments. On Earth, it is one of themost important greenhouse gases and it is present in significant quantities in theatmospheres of giant planets, Titan, exoplanets, brown dwarves… We are presentlyworking on the global analysis of the CH 4 absorption spectrum in the 0 to 6200 cm -1region. This is especially motivated by the need of extensive methane line lists for theinterpretation of data from the Cassini-Huygens mission [5,6].Water vapor has a key role in the physics and chemistry of the Earth atmosphere. Thenumerous studies dealing with its rovibrational spectrum are being processed by anIUPAC task group [7]. The long path experimental database originating from studiesperformed at GSMA from 26000 cm -1 down-to 4200 cm -1 is included in the VAMDC e-Infrastructure [8] in order to provide access to the original experimental values. Thedatabase structure is implemented to provide access to the standard line positions,intensities self-broadening and broadening by air or nitrogen or any other species.References :[1] Rinsland C. P. et al., J. Quant. Spectrosc. Radiat. Transfer, 96, 31 (2005)[2] Bézard B. et al., Bull Am. Astron. Soc., 33, 1079 (2001)[3] Coustenis A. et al., Icarus, 189, 35 (2007)[4] Stevenson K.B. et al., Nature, 464, 1161 (2010)[5] De Bergh C. et al., Planetary and Space Science, 61, 85–98 (2012)[6] Sromovsky et al., Icarus, 218, 1–23 (2012)[7] Tennyson J., et al. J. Quant. Spectrosc. Radiat. Transfer, submitted.[8] Dubernet M.L. et al., J. Quant. Spectrosc. Radiat. Transfer, 111, 2265 (2010)
Poster session, J28 191New analysis of the triplet (b 3 Σ - – a 3 Π) system of the AlHW. Szajna 1 , R. Hakalla 2 , M. Zachwieja 3 ,I. Piotrowska 4 , M. Ostrowska-Kopeć 5 , P. Kolek 6 , R. Kępa 71,2,3,4,5,6,7 Atomic and Molecular <strong>Ph</strong>ysics Laboratory, Institute of <strong>Ph</strong>ysics,University of Rzeszów, 35-310 Rzeszów, POLAND1 szajna@univ.rzeszow.pl, 2 hakalla@univ.rzeszow.pl, 3 zachwiej@univ.rzeszow.pl,4 ipiotrowska@if.univ.rzeszow.pl, 5 mostrow@univ.rzeszow.pl,6 kolek@if.univ.rzeszow.pl, 7 krepa@univ.rzeszow.pl,Szajna W.Hakalla R.Zachwieja M.Piotrowska I.Ostrowska-Kopec M.Kolek P.Kepa R.The emission spectrum of the b 3 Σ - – a 3 Π system of the AlH molecule was reinvestigatedin the spectral region of about 26 000 cm -1 by using a high accuracy dispersive opticalspectroscopy. The AlH molecules were formed and excited in an aluminium hollowcathodelamp with two anodes, filled with a mixture of Ne buffer gas and a trace ofNH 3 . The emission from the discharge was observed with a plane grating spectrographand recorded by a photomultiplier tube. The full rotational structure of the 0-0 and 1-1bands was precisely measured end rotationally analyzed and many new constants of theb 3 Σ - and a 3 Π states have been derived from the analysis. Also, pointed out by Zhu et al. 1differences in the λ constants values for the υ = 0 and υ = 1 of the b 3 Σ - state have beenexplained. Although the b - a system has previously been seen in emission 2,3,4,5 , ourwork represents the first modern and complete analysis of this transition of the AlHmolecule.Fig. 1: An overview of the b 3 Σ - – a 3 Π system of AlH in the spectral region of 26 000 cm -1 .References[1] Y. Zhu, R. Shehadeh, E. Grant, J. Chem. <strong>Ph</strong>ys., 97, 883, 1992.[2] W. Holst, Z. <strong>Ph</strong>ys., 86, 338, 1933.[3] C. N. Challacombe, G. M. Almy, <strong>Ph</strong>ys. Rev., 51, 930, 1937.[4] M. Rafi, M. Aslam Baig, Il Nuo. Cim., 43, 271, 1978.[5] C. Tao, X. Tan, P. Dagdigian, M. Alexander, J. Chem. <strong>Ph</strong>ys., 118, 10477, 2003.
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Book of abstractsof the 22 th Inter
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CommitteesLocal Organizing committe
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Table of contentProgram of sessions
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8 Program of sessionsInvited Lectur
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10 Program of sessionsD6 Tasinato N
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26 Program of sessionsIoannes Marcu
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48 Poster session, D1Spectroscopic
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54 Poster session, D7IR spectroscop
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136 Poster session, H23Spectroscopy
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138 Poster session, H25New investig
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240 Author indexKhelkhal M. — D29
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248 Author indexZamotaeva V.A. —
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250 EmailsAbdelghany A.Abdelghany A
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252 EmailsGuarnieri A.ag@tf.uni-kie
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254 EmailsMichaut X.Xavier.Michaut@
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256 EmailsTyuterev Vl.G.vladimir.ti
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FT-IR spectrometerIFS 125HROutstand
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32nd International Symposium on Fre
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Some more information
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Addresses:Conference Site: National