geisa: gestion et etude des informations...

1
! " ! " ! " ! " N. Jacquinet-Husson, C. Boutammine, L. Crépeau, R. Armante, V. Capelle, C. Crevoisier, N.A. Scott, A. Chédin Laboratoire de Météorologie Dynamique (LMD), Ecole Polytechnique, Palaiseau, France ! # http://ether.ipsl.jussieu.fr Minor permanent constituents of EARTH’s atmosphere : O 3 ,CH 4 ,N 2 O,CO,N 2 Major Permanent constituents of EARTH’s atmosphere : O 2 ,H 2 O,CO 2 Trace molecules of EARTH’s atmosphere : NO, SO 2 ,NO 2 ,NH 3 , HNO 3 , OH,HF, HCl, HBr, HI, ClO, OCS, H 2 CO, PH 3 Molecules in atmospheres of JUPITER, SATURN, URANUS,TITAN etc.: C 6 H 6 , CH 3 D, C 2 H 2 , C 2 H 4 , GeH 4 , HCN, C 3 H 8 , C 3 H 4 (MSG-2 25/01/06) EARTH (CASSINI-HUYGENS 29/01/06) TITAN $%& ’( ) *$* ( +" , GEISA distribution by CNES/INSU/IPSL Ether Thematic Expertise Group for Atmospheric Chemistry http://ara.abct.lmd.polytechnique.fr GEISA: Gestion et Etude des Informations Spectroscopiques Atmosphériques; Management and Study of Atmospheric Spectroscopic Information - - - - Satellite data Desarchiving Channel sélection A priori Cloud detection Spatio-temporal collocation Radiative Transfer Direct Models Clear sky or scattering medium Data Archive 100 To In situ Radiosoundings GEISA SPECTROSCOPIC DATABASE #( .. /0 .( /. #( .. /0 .( /. #( .. /0 .( /. #( .. /0 .( /. + * + * + * + * ARSA Analyzed RadioSoundings Archive INFRARED Spectral range : 200 – 6500 cm -1 CFC-11, CFC-12, CFC-13, CFC-14, HCFC-22, HCFH-21, HFC-32, CFC-113, CFC-114, CFC-115, HCFC-123, HCFC-124, HFC-125, HFC-134, HFC-134a, HCFC-141b, HCFC-142b,HFC-143a, HFC-152a, HCFC-225ca, HCFC-225cb, N 2 O 5 , SF 6 , ClONO 2 , CCl 4 C 2 F 6 Perfluoroethane C 3 H 8 Propane C 2 H 6 Ethane C 2 H 2 Acetylene C 2 H 4 Ethene HFC-143, SF 5 CF 3 , C 4 F 8 , HNO 4 , HCH-365mfc C H , CH CN, C H NO (PAN) UV/VIS Spectral range : 7750 - 51,282 cm-1 NO 2 , O 3 SO 2 ,O 2 OClO, H2CO CS 2 OBrO BrO CHOCHO IO OIO H 2 CO C 6 H 6 Benzene C 8 H 10 Mxylene C 8 H 10 Oxylene C 8 H 10 Pxylene C 7 H 8 Toluene . * . * . * . *$ $ $* * * * 1 $ $ $ * * * *$ $ $* * * * 2 The development of GEISA was started in 1976 at LMD and is regularly updated. GEISA is a computer-accessible spectroscopic database, aiming at accurately describing the characteristics of absorption properties to meet the needs of communities involved in understanding the atmospheres of the Earth and other planets. Evolution of GEISA since 1975 (line parameters sub-database) Fig. Ref.: Jacquinet-Husson N, et al. The 2009 edition of the GEISA spectroscopic database. JQSRT (2011), doi:10.1016/j.jqsrt.2011.06.004 50 Molecules 111 Isotopes Molecules specific GEISA for planetary atmosphere studies Parameter ID Meaning, Units A Wavenumber (cm -1 ) of the line B Intensity of the line in (cm -1 /(molecule.cm -2 ) C Air broadening pressure halfwidth (HWHM)(*) (cm -1 atm -1 ) D Energy of the lower transition level (cm -1 ) E Transition quantum identifications for the lower and upper state of the transition F Temperature dependence coefficient n of the air broadening HWHM G Identification code for isotope as in GEISA I Identification code for molecule as in GEISA J Internal GEISA code for the data identification K Molecule number L Isotope number (1=most abundant. 2= second…etc) M Einstein A-coefficient (s -1 ). N Self broadening pressure HWHM (cm -1 atm -1 ) (for water) O Air pressure shift of the line transition (cm -1 atm -1 ) in GEISA-09 Standardized parameter missing values 252 character Records; 31 Parameters; Reference temperature 296 K ARCHIVED SPECTROSCOPIC LINE PARAMETERS - Thermodynamics - Clouds - Greenhouse gases - Continental surfaces - Aerosols - etc… Radiative Transfer Inverse Models - Bayesian inference - Neural Networks - Clustering Model/observation bias computation Instruments monitoring Scientific Themes A priori infos nadir or limb Courtesy A. Chédin, Trattoria/CNES 2-3 April 2008 C 6 H 6 , CH 3 CN, C 2 H 3 NO 5 (PAN) (CH 3 ) 2 CO (Acetone) REFRACTIVE INDICES OF BASIC AEROSOL COMPONENTS: ** ** ** ** Water ice; ** ** ** **Acids; ** ** ** **Water droplets; ** ** ** **Water soluble components; ** ** ** **Thin films ; ** ** ** **Solid Substances ATMOSPHERIC AEROSOLS FROM LITMS (Rublev, 1994) SOFTWARE PACKAGE AND DATABASE OPAC (Hess et al., 1998) ** ** ** ** Optical Properties of Aerosols and Clouds GLOBAL AEROSOL DATA SET: GADS (Köpke et al., 1997) ( ! ( ! ( ! ( ! * " * * " * * " * * " *$ $ $* * * * ) Molecules of IASI (645 – 2760 cm -1 ) interest Molecules of CIRS (10 – 600 cm -1 ; 600 – 1500 cm -1 ) interest: C 4 H 2 , HC 3 N, C 2 H 6 , C 2 H 2 , C 2 H 4 , HCN, C 3 H 4 , C 6 H 6 , C 2 HD ! " ! " ! " ! " The performances of remote sensing applications of the second generation vertical sounding, high- resolution, sophisticated hyperspectral spectroscopic instruments, such as AIRS (http://www.airs.jpl.nasa.gov/ ) in the USA and IASI (http://earth-sciences.cnes.fr/IASI/ ) in Europe, highly depends on the accuracy of the spectroscopic parameters of the optically active atmospheric gases. Spectroscopy is at the root of modern planetology, enabling to determine the physical properties of planets remotely. The GEISA database has been extensively used in the modelling of Titan’s atmosphere and in the comparison with observations performed by Voyager ground-based telescopes (http://voyager.jpl.nasa.gov/ ). More recently the instruments on board the Cassini- Huygens mission http://www.esa.int/SPECIALS/Cassini- Huygens/index.html ), returned valuable information on Jupiter, Saturn and Titan. The measurements of the Iasi instrument NIR spectral region H 2 O intensity versus wavenumber transitions present in GEISA-03 (in red) transitions added in GEISA-09 (+ in blue) Illustration of additional spectroscopic data in GEISA-09 [email protected] #0 #0 #0 #0 Jacquinet-Husson N. et al. The 2003 edition of the GEISA/IASI spectroscopic database. JQSRT, 95, 429- 67, 2005. Jacquinet-Husson N. et al. The GEISA spectroscopic database: current and future archive for Earth & planetary atmosphere studies. JQSRT, 109, 1043 - 1059, 2008. Jacquinet-Husson N. et al. The 2009 edition of the GEISA spectroscopic database. JQSRT (2011), doi:10.1016/j.jqsrt.2011.06.004 R Temperature dependence coefficient n of the air pressure shift A’ Estimated accuracy (cm -1 ) on the line position B’ Estimated accuracy on the intensity of the line in (cm -1 /(molecule.cm -2 ) C’ Estimated accuracy on the air collision HWHM (cm -1 atm -1 ) F’ Estimated accuracy on the temperature dependence coefficient n of the air broadening HWHM O’ Estimated accuracy on the air pressure shift of the line transition (cm -1 atm -1 ) R’ Estimated accuracy on the temperature dependence coefficient n of the air pressure shift N’ Estimated accuracy on the self broadened HWHM (cm -1 atm -1 ) S Temperature dependence coefficient n of the self broadening HWHM S’ Estimated accuracy on the temperature dependence coefficient n of the self- broadening HWHM T Self pressure shift of the line transition (cm -1 atm -1 ) T’ Estimated accuracy on the self pressure shift of the line transition (cm -1 atm -1 ) U Temperature dependence coefficient n of the self pressure shift U’ Estimated accuracy on the temperature dependence coefficient n of the self pressure shift ===================================== (*) HWHM: line half-width at half-maximum Hydrocarbons: CH 4 : in the near-infrared region (from 0.8 to 5 micron) both from theory and laboratory measurements C 6 H 2 : the band at 642 cm -1 which is studied by the LISA group C 2 H 6 : a complete analysis of the 1400-1500 cm -1 band to be made, C 3 H 8 : needs in all bands beyond 800 cm -1 C 3 H 4 (propyne and allene) the data of the CDMS archive to be considered C 6 H 6 : a re-analysis of the Dang-Nhu data is required Nitriles: C 2 N 2 : presently no data on the combination band at 735 cm -1 (which interferes with C 2 H 2 and C 3 H 8 ) CH 3 CN (acetonitrile has been observed in the millimeter range, but also has bands in the mid and far IR) Other heavier nitriles such as propionitrile etc... For Titan’s atmosphere: - A global analysis to identify the hot bands and retrieve the intensities of the present molecular species is urgently needed - Furthermore, numerous isotopes now identified in Titan’s spectrum cannot be properly analyzed in the absence of adequate spectroscopic data. Updates in the available spectroscopic databases are essential to the study of the outer planets and their satellites with atmospheres. " " " - - - " " " 3" 3" 3" 3" 405 .( 0 405 .( 0 405 .( 0 405 .( 0 CNES, CNRS/INSU and EUMETSAT For their encouragements and supports The GEISA/IASI-09 database is an extraction (spectral range 599-3001 cm -1 ) of GEISA-09. It has been developed, is maintained and supported for many years with the purpose of assessing the IASI measurements capabilities, in the frame of the EUMETSAT/ Metop-A European Polar System (EPS). IASI is on Metop-A since October 19th 2006. For the Level 1 Cal/Val activities validation at CNES, GEISA/IASI has been chosen as the reference spectroscopic database, using the 4A line by line Radiative Transfer Model ([Scott & Chédin, J.Appl.Met (1981); 4A-OP co-developed by LMD (http://ara.abct.lmd.polytechnique.fr ) and NOVELTIS (http://www.noveltis..fr ) with support of CNES]. CONCLUSIONS FROM THE 2nd INTERNATIONAL IASI CONFERENCE, SEVRIER, France, 2010 Considering the still existing Spectroscopy issues, the following already ongoing specific actions have to be reinforced and maintained: Necessary validation: Assessment in GEISA/IASI of: - spectroscopic molecular species related to IASI trace gas retrievals, i.e: HCN, NH 3 , HCOOH, C 2 H 4 , CH 3 OH, H 2 CO, added to already implemented ones more related to operational meteorology, i.e.: H 2 O, CO 2 , O 3 , N 2 O,CO, CH 4 , O 2 , NO, SO 2 , NO 2 , HNO 3 , OCS, C 2 H 2 , N 2 .. - cross-sections already implemented: i.e.: CFC-11, CFC-12, CFC-14, CCl 4 , N 2 O 5 , HCFC-22. Consider complementary ones to be added (such as PAN). PAN implemented in GEISA-09 and GEISA/IASI-09. The still outstanding general spectroscopy-related conclusions for public databases - from ISSWG, CNES, Paris, France, (2008) - have to be remembered. Eventually, line coupling/mixing modelling (which should be used in conjunction with the molecular parameters of the data base from which they have been derived) and non-LTE (Local Thermodynamic Equilibrium) effects are areas to be investigated. 3" #, ( 3" #, ( 3" #, ( 3" #, ( 3 " " 3 " " 3 " " 3 " " The measurements of the Fourier transform spectrometer CIRS consisting of two interferometers scanning the far-infrared (10–600 cm -1 ) and mid-infrared (600–1500 cm -1 ) made possible enhanced Titan’s atmosphere modelling . The GEISA-09 updated or new line lists, such as those of: C 2 H 6 , HCN, C 3 H 4 , C 6 H 6 , C 2 HD, have been used in the composition of Titan’s atmosphere and isotopic ratios determination, such as the detection of C 2 HD and the determination of D/H ratio. See Coustenis et al.: Icarus 2007, 189 (35-62) Icarus 2008, 197 (539-548) Icarus 2010, 207 (461-476), etc … (Non exhaustive list of a few examples)

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������������������� ����������������������������������������������������������������� ����������������������������������������������������������������� ����������������������������������������������������������������� ����������������������������������������������

����� ������!���"�������������������� ������!���"�������������������� ������!���"�������������������� ������!���"���������������N. Jacquinet-Husson, C. Boutammine, L. Crépeau, R. Armante, V. Capelle, C. Crevoisier, N.A. Scott, A. Chédin

Laboratoire de Météorologie Dynamique (LMD), Ecole Polytechnique, Palaiseau, France

���� !�#����������������������http://ether.ipsl.jussieu.fr

�Minor permanent constituents of EARTH’s atmosphere : O3,CH4,N2O,CO,N2 …

�Major Permanent constituents of EARTH’s atmosphere : O2,H2O,CO2 …

�Trace molecules of EARTH’s atmosphere :NO, SO2,NO2,NH3, HNO3, OH,HF, HCl, HBr, HI, ClO, OCS, H2CO, PH3

�Molecules in atmospheres of JUPITER, SATURN, URANUS,TITAN etc.:C6H6, CH3D, C2H2, C2H4, GeH4, HCN, C3H8, C3H4 …

(MSG-2 25/01/06)EARTH

(CASSINI-HUYGENS 29/01/06)TITAN

���������$%&��'���( ��)���*$����*��������������������( ���+�"��������, �����

GEISA distribution by CNES/INSU/IPSL EtherThematic Expertise Group for Atmospheric Chemistry

http://ara.abct.lmd.polytechnique.fr

GEISA: Gestion et Etude des Informations Spectroscopiques Atmosphériques; Management and Study of Atmospheric Spectroscopic Information

������������ �����-������������� �����-������������� �����-������������� �����-�

Satellite data

DesarchivingChannel sélection

A priori

Cloud detectionSpatio-temporal

collocation

Radiative Transfer Direct Models

Clear sky or scattering medium

Data Archive100 To

In situ Radiosoundings

GEISASPECTROSCOPIC

DATABASE

#��( �����..���������/����0�����.�( ����/�����.���#��( �����..���������/����0�����.�( ����/�����.���#��( �����..���������/����0�����.�( ����/�����.���#��( �����..���������/����0�����.�( ����/�����.���

�� ��+���������*��������������������������� ��+���������*��������������������������� ��+���������*��������������������������� ��+���������*�������������������������

ARSAAnalyzed RadioSoundings Archive

INFRAREDSpectral range : 200 – 6500 cm-1

CFC-11, CFC-12, CFC-13, CFC-14, HCFC-22, HCFH-21, HFC-32,CFC-113, CFC-114, CFC-115, HCFC-123, HCFC-124, HFC-125,HFC-134, HFC-134a, HCFC-141b,HCFC-142b,HFC-143a, HFC-152a,HCFC-225ca, HCFC-225cb,N2O5, SF6, ClONO2, CCl4C2F6 PerfluoroethaneC3H8 PropaneC2H6 EthaneC2H2 AcetyleneC2H4 EtheneHFC-143, SF5CF3, C4F8, HNO4, HCH-365mfcC H , CH CN, C H NO (PAN)

UV/VISSpectral range : 7750 - 51,282 cm-1

NO2, O3SO2,O2OClO, H2COCS2OBrOBrOCHOCHOIOOIOH2COC6H6 BenzeneC8H10 Mxylene C8H10 OxyleneC8H10 PxyleneC7H8 Toluene

.�����������������*.�����������������*.�����������������*.�����������������*$$$$����*�������*�������*�������*���1����������������$$$$����������*����������*����������*����������*$$$$����*��������*��������*��������*����2

The development of GEISA was started in 1976 at LMD and is regularly updated. GEISA is a computer-accessible spectroscopic database, aiming at accurately describing the characteristics of absorption properties to meet the needs of communities involved in understanding the atmospheres of the Earth and other planets.

Evolution of GEISA since 1975 (line parameters sub-database)

Fig. Ref.: Jacquinet-Husson N, et al. The 2009 edition of the GEISA spectroscopic database. JQSRT (2011), doi:10.1016/j.jqsrt.2011.06.004

50 Molecules111 Isotopes

Molecules specific GEISA for planetary atmosphere studies

Parameter ID Meaning, Units

A Wavenumber (cm-1) of the lineB Intensity of the line in (cm-1/(molecule.cm-2)C Air broadening pressure halfwidth (HWHM)(*) (cm-1atm-1)D Energy of the lower transition level (cm-1)E Transition quantum identifications for the lower and upper state of the transitionF Temperature dependence coefficient n of the air broadening HWHM G Identification code for isotope as in GEISAI Identification code for molecule as in GEISAJ Internal GEISA code for the data identificationK Molecule numberL Isotope number (1=most abundant. 2= second…etc)M Einstein A-coefficient (s-1).N Self broadening pressure HWHM (cm-1atm-1) (for water)O Air pressure shift of the line transition (cm-1atm-1)

in GEISA-09Standardized parameter

missing values

252 character Records; 31 Parameters; Reference temperature 296 K

ARCHIVED SPECTROSCOPIC LINE PARAMETERS

��������� �������������� �������������� �������������� �����

- Thermodynamics- Clouds- Greenhouse gases- Continental surfaces- Aerosols- etc…

Radiative Transfer Inverse Models

- Bayesian inference- Neural Networks- Clustering

Model/observation biascomputationInstruments monitoring

ScientificThemes

A prioriinfos

Clear sky or scattering mediumnadir or limb

Courtesy A. Chédin, Trattoria/CNES 2-3 April 2008

C6H6, CH3CN, C2H3NO5 (PAN)(CH3)2CO (Acetone)

� REFRACTIVE INDICES OF BASIC AEROSOL COMPONENTS:∗∗∗∗∗∗∗∗ Water ice; ∗∗∗∗∗∗∗∗Acids; ∗∗∗∗∗∗∗∗Water droplets; ∗∗∗∗∗∗∗∗Water soluble components; ∗∗∗∗∗∗∗∗Thin films ; ∗∗∗∗∗∗∗∗Solid Substances

� ATMOSPHERIC AEROSOLS FROM LITMS (Rublev, 1994)

� SOFTWARE PACKAGE AND DATABASE OPAC (Hess et al., 1998)∗∗∗∗∗∗∗∗ Optical Properties of Aerosols and Clouds

� GLOBAL AEROSOL DATA SET: GADS (Köpke et al., 1997)

( ������!���� ����������� ������������( ������!���� ����������� ������������( ������!���� ����������� ������������( ������!���� ����������� ������������

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Molecules of IASI (645 – 2760 cm-1) interest

Molecules of CIRS (10 – 600 cm-1; 600 – 1500 cm-1) interest:

C4H2, HC3N, C2H6, C2H2, C2H4, HCN, C3H4, C6H6, C2HD

������������������ ������!���"������������������������������ ������!���"������������������������������ ������!���"������������������������������ ������!���"������������

�The performances of remote sensing applications of the second generation vertical sounding, high-resolution, sophisticated hyperspectral spectroscopicinstruments, such as AIRS (http://www.airs.jpl.nasa.gov/)in the USA and IASI (http://earth-sciences.cnes.fr/IASI/)in Europe, highly depends on the accuracy of the spectroscopic parameters of the optically active atmospheric gases.

�Spectroscopy is at the root of modern planetology, enabling to determine the physical properties of planets remotely.�The GEISA database has been extensively used in the modelling of Titan’s atmosphere and in the comparison with observations performed by Voyager ground-based telescopes (http://voyager.jpl.nasa.gov/).

�More recently the instruments on board the Cassini-Huygens mission http://www.esa.int/SPECIALS/Cassini-Huygens/index.html), returned valuable information on Jupiter, Saturn and Titan.

The measurements of the

Iasi instrument

NIR spectral region H2O intensity versus wavenumbertransitions present in GEISA-03 (�in red)transitions added in GEISA-09 (+ in blue)

Illustration of additional spectroscopic data in GEISA-09

[email protected]

��#���0�����#���0�����#���0�����#���0���

Jacquinet-Husson N. et al. The 2003 edition of the GEISA/IASI spectroscopic database. JQSRT, 95, 429-67, 2005.Jacquinet-Husson N. et al. The GEISA spectroscopic database: current and future archive for Earth & planetary atmosphere studies. JQSRT, 109, 1043 - 1059, 2008.Jacquinet-Husson N. et al. The 2009 edition of the GEISA spectroscopic database. JQSRT (2011), doi:10.1016/j.jqsrt.2011.06.004

O Air pressure shift of the line transition (cm atm )R Temperature dependence coefficient n of the air pressure shiftA’ Estimated accuracy (cm-1) on the line positionB’ Estimated accuracy on the intensity of the line in (cm-1/(molecule.cm-2)C’ Estimated accuracy on the air collision HWHM (cm-1atm-1)F’ Estimated accuracy on the temperature dependence coefficient n of the air broadening

HWHMO’ Estimated accuracy on the air pressure shift of the line transition (cm-1atm-1)R’ Estimated accuracy on the temperature dependence coefficient n of the air pressure

shiftN’ Estimated accuracy on the self broadened HWHM (cm-1atm-1)S Temperature dependence coefficient n of the self broadening HWHMS’ Estimated accuracy on the temperature dependence coefficient n of the self- broadening

HWHMT Self pressure shift of the line transition (cm-1atm-1)T’ Estimated accuracy on the self pressure shift of the line transition (cm-1atm-1) U Temperature dependence coefficient n of the self pressure shift U’ Estimated accuracy on the temperature dependence coefficient n of the self pressure shift

=====================================(*) HWHM: line half-width at half-maximum

�Hydrocarbons:CH4: in the near-infrared region (from 0.8 to 5 micron) both from theory

and laboratory measurementsC6H2: the band at 642 cm-1 which is studied by the LISA groupC2H6: a complete analysis of the 1400-1500 cm-1 band to be made, C3H8:

needs in all bands beyond 800 cm-1

C3H4 (propyne and allene) the data of the CDMS archive to be considered C6H6: a re-analysis of the Dang-Nhu data is required

� Nitriles:C2N2: presently no data on the combination band at 735 cm-1 (which

interferes with C2H2 and C3H8)CH3CN (acetonitrile has been observed in the millimeter range, but also

has bands in the mid and far IR)Other heavier nitriles such as propionitrile etc...

� For Titan’s atmosphere:- A global analysis to identify the hot bands and retrieve the intensities of

the present molecular species is urgently needed- Furthermore, numerous isotopes now identified in Titan’s spectrum

cannot be properly analyzed in the absence of adequate spectroscopic data. Updates in the available spectroscopic databases are essential to the study of the outer planets and their satellites with atmospheres.

��������""""������������----����""""���� �������������������� �������������������������������������������������������������������� ���������������������������� ��������������������

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CNES, CNRS/INSU and EUMETSAT

For their encouragements and supports

�The GEISA/IASI-09 database is an extraction(spectral range 599-3001 cm-1) of GEISA-09. It has been developed, is maintained and supported for many years with the purpose of assessing the IASImeasurements capabilities, in the frame of theEUMETSAT/ Metop-A European Polar System (EPS). IASI is on Metop-A since October 19th 2006.�For the Level 1 Cal/Val activities validation at CNES, GEISA/IASI has been chosen as the reference spectroscopic database, using the 4A line by line Radiative Transfer Model ([Scott & Chédin, J.Appl.Met (1981); 4A-OP co-developed by LMD (http://ara.abct.lmd.polytechnique.fr) and NOVELTIS (http://www.noveltis..fr) with support of CNES].

CONCLUSIONS FROM THE 2nd INTERNATIONAL IASI CONFERENCE, SEVRIER, France, 2010

Considering the still existing Spectroscopy issues, the following already ongoing specific actions have to be reinforced and maintained:� Necessary validation: Assessment in GEISA/IASI of:

- spectroscopic molecular species related to IASI trace gas retrievals, i.e: HCN, NH3, HCOOH, C2H4, CH3OH, H2CO, added to already implemented ones more related to operational meteorology, i.e.: H2O, CO2, O3, N2O,CO, CH4, O2, NO, SO2, NO2, HNO3, OCS, C2H2, N2..

- cross-sections already implemented: i.e.: CFC-11, CFC-12, CFC-14, CCl4, N2O5, HCFC-22. Consider complementary ones to be added (such as PAN). PAN implemented in GEISA-09 and GEISA/IASI-09.� The still outstanding general spectroscopy-related conclusions for public databases - from ISSWG, CNES, Paris, France, (2008) - have to be remembered. Eventually, line coupling/mixing modelling (which should be used in conjunction with the molecular parameters of the data base from which they have been derived) and non-LTE (Local Thermodynamic Equilibrium) effects are areas to be investigated.

������ �����������������3����"����������������#��, ����( ��� ������������������ �����������������3����"����������������#��, ����( ��� ������������������ �����������������3����"����������������#��, ����( ��� ������������������ �����������������3����"����������������#��, ����( ��� ������������

��3������������������ �����"���������������������������"������������������3������������������ �����"���������������������������"������������������3������������������ �����"���������������������������"������������������3������������������ �����"���������������������������"����������������

The measurements of the Fourier transform spectrometer CIRS consisting of two interferometers scanning the far-infrared (10–600 cm−1) and mid-infrared (600–1500 cm−1) made possible enhanced Titan’s atmosphere modelling .

�The GEISA-09 updated or new line lists, such as those of: C2H6, HCN, C3H4, C6H6, C2HD, have been used in the composition of Titan’s atmosphere and isotopic ratios determination, such as the detection of C2HD and the determination of D/H ratio. See Coustenis et al.: Icarus 2007, 189 (35-62)

Icarus 2008, 197 (539-548)Icarus 2010, 207 (461-476), etc …

(Non exhaustive list of a few examples)