THE GEISA 2008 EDITION : PRESENTATION AND EVALUATION FOR PLANETARY ATMOSPHERE STUDIESN. Jacquinet-Husson (1), V. Capelle (1), L. Crépeau (1), N.A. Scott (1), R. Armante (1), A. Chédin (1), A. Coustenis (2)

(1). Laboratoire de Météorologie Dynamique (LMD) Ecole Polytechnique, Palaiseau, France(2). Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Observatoire de Meudon, Meudon, France

EVOLUTION GEISA SINCE 1978

http://ara.lmd.polytechnique.fr

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

THE GEISA SYSTEM: Three SUB-DATABASES and ASSOCIATED MANAGEMENT SOFTWARES (For each sub-database)

ICSA-2007 Marseille 5-6 Juin 2007

GEISASpectroscopic

database

STRANSACLine-by-line

ForwardModel

4AAutomatizedAtmosphericAbsorption

Atlas

ECMWFRadiative

code

TIGR2300 selectedAtmospheric

Profiles (T,H2O,O3 …)PrecomputedBT, Trans.,

JACOBIANSRadiative flux

3RRapidRadiance

Recognition

Neural NetworkLearning

(forwardmode)

3IImproved

InitializationInversion

Neural Network Learning

(Inverse mode)

•Spectroscopy

•Forwardmodel

•Inverse model

•Educateddatabasededicatedto one particularapplication (TOVS, AIRS, IASI, Radiative budget …)

Faster3000/40000 times

Faster30/400 times

TheGEISA spectroscopic database in theARA/LMD tools

The ARA (Atmospheric Radiation Analysis) group at LMD has been engaged, during the past three decades, in the development of GEISA, a computer-accessiblespectroscopic database, designed to facilitate accurate and fast forward calculationsof atmospheric radiative transfer using a line-by-line and (atmospheric) layer-by-layerapproach.The performance of the second generation vertical sounding, high-resolution, sophisticated infrared spectroscopic instruments, such as AIRS (http://www.airs.jpl.nasa.gov/) in the USA and IASI (http://earth-ciences.cnes.fr/IASI/) in Europe, will highly depend on the accuracy in the spectroscopic parameters of the optically active atmospheric gases, since suchdata constitute an essential input in the forward models that are used to interpret the recorded spectral radiances.

GENERAL CONTEXT

GEISA DISTRIBUTION

GEISA implemented on the Ether (CNRS/CNES) Products and Services Centre (CPS)

http://ether.ipsl.jussieu.fr

53 co-authors- 24 Institutions

LINE TRANSITION PARAMETERS SUB-DATABASE

Mol. Spectral Range/ Band Id. ------------------------------------------------- GEISA-03 GEISA-08 update ===================================================H2O 0.007- 25232.004 cm-1 500- 8000 cm-1

CO2 436.123- 9648.007 cm-1 2200-7000 cm-1

4000-9000 cm-1

O3 0.026- 4060.783 cm-1 1613- 4845 cm-1

6000- 7000 cm-1 N2O 0.838- 5131.249 cm-1 525- 10175 cm-1

CO 3.414- 8464.882 cm-1 CH4 0.010- 9199.285 cm-1 750- 1350 cm-1 2850- 3150 cm-1

4800- 9200 cm-1

O2 0.000- 15927.806 cm-1 0.7 μm region NO 0.000- 9273.214 cm-1

SO2 0.017- 4092.948 cm-1 1011- 1410 cm-1NO2 0.498- 3074.366 cm-1 2780- 2940 cm-1NH3 0.058- 5294.502 cm-1 PH3 17.805- 2478.765 cm-1 770-3601 cm-1

HNO3 0.035- 1769.982 cm-1 Sub-millimeter Ʋ5-Ʋ9 2Ʋ9-Ʋ9 Ʋ5 ; 2Ʋ9 (Ʋ8+Ʋ9) ; (Ʋ6+Ʋ7)

OH 0.005- 35877.031 cm-1 HF 41.111- 11535.570 cm-1 HCl 20.240- 13457.841 cm-1

HBr 16.232- 9758.565 cm-1 HI 12.509- 8487.305 cm-1 ClO 0.015- 1207.639 cm-1 OCS 0.381- 4118.004 cm-1 H2CO 0.000- 2998.527 cm-1 1.573 µm

C2H6 725.603- 2977.926 cm-1 12 µm region CH3D 7.760- 3306.810 cm-1 3250-3700 cm-1 C2H2 604.774- 3374.223 cm-1 2.5 µm and 3.8 µm 1.5 µm region 0.83 µm region

Mol. Spectral Range/ Band Id. -------------------------------------------------- GEISA-03 GEISA-08 update ==================================================

C2H4 701.203- 3242.172 cm-1 1380- 1509 cm-1

GeH4 1937.371- 2224.570 cm-1 HCN 2.870- 18407.973 cm-1 14 µm (Ʋ2; 2Ʋ2-Ʋ2)

C3H8 700.015- 799.930 cm-1 C2N2 203.955- 2181.690 cm-1 203.872 - 266.320 cm-1

C4H2 190.588- 654.425 cm-1 199.1 - 244.0 cm-1 605.5 - 651.4 cm-1

HC3N 474.293- 690.860 cm-1 16 µm (Ʋ5) 20µm (Ʋ6)HOCl 0.024- 3799.249 cm-1 3- 309 cm-1N2 1992.628- 2625.497 cm-1 4.3 μm CH3Cl 674.143- 3161.830 cm-1 650- 2650 cm-1H2O2 0.043- 1499.487 cm-1 0.043- 1730 cm-1H2S 2.985- 4098.234 cm-1 HCOOH 1060.962- 1161.251 cm-1 10- 100 cm-1 940- 1244 cm-1 COF2 725.006- 2001.348 cm-1 SF6 940.425- 952.238 cm-1 Ʋ3, Ʋ4, Ʋ4+Ʋ6-Ʋ6C3H4 290.274- 359.995 cm-1 290- 360 cm-1

592- 673 cm-1

HO2 0.173- 3675.819 cm-1 ClONO2 763.641- 790.805 cm-1 500- 1330 cm-1=====================================================

New Molecular Species (non exhaustive list)=====================================================

CH3Br 16 µm

CH3OH 0.02 - 33 cm-1 10 µm region

NO+ 1635- 2530 cm-1HNC 0.22- 12594 cm-1C6H6 642 –705 cm-1 C2HD 451 - 580 cm-1 600 - 760 cm-1

Major Permanent constituents of EARTH’s atmosphere : O2,H2O,CO2 … Molecules in atmospheres of JUPITER, SATURN, URANUS,TITAN etc.: C2H6, CH3D, C2H2, C2H4, GeH4, HCN, C3H8, C3H4 …

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

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

30 Parameters 255 Character recordsReference Temperature 296 K

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 identification

(For inter-compatibility with HITRAN-04 format)

K 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)P Accuracy indices for frequency, intensity and halfwidthQ Indices for lookup of references for frequency, intensity and halfwidth

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 shift

(Especially dedicated to Water Molecule)N’ 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

ARCHIVED SPECTROSCOPICLINE PARAMETERS

AEROSOL SUB-DATABASE

Data on microphysical and optical properties of basic aerosol components.

4 sub-databases included: 

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) 

FROM CONCLUSIONS OF VALIDATION WITH THE 4A-00/LMD MODEL FOR IASI RADIATIVE TRANSFER MODELLING

The water vapour spectroscopic parameters: still need to be validatedThe water vapour continuum: more tuning to be done when more validation data (especially with high water vapor content) become availableThe freons bands at 850 and 920 cm-1: refine the temperature dependenceO3 in the 9.6 μm region: the spectroscopic parameters still need to be validatedSome CO2 – Q,P and R branches: further improvement/tuning of the line mixing

NEEDS IN SPACE STUDIES OF OUTER PLANETS AND TITAN (Courtesy of Athena Coustenis and Bruno Bézard)

Hydrocarbons:CH4 in the near-infrared region (from 0.8 to 5 μm) both from theory and laboratory measurementsC6H2: (at 642 cm-1) this band is being studied by Jolly and BénilanC2H6: need of the spectroscopic parameters for the 1400-1500 cm-1 band (observed on Jupiter & Titan)

Also: for molecules heavier than C2H6 (like C6H2, HC5N, there’s still few data)C3H8: needs in all bands except at 748 cm-1 , in particular the one at 1150 cm-1

C3H4 (allene) C6H6 benzeneC4H2 : for the band at 628 cm-1 it would require a global analysis (like the one for HC3N and C4N2) to identify all the hot bands (some work is being done by Bénilan and Jolly, based on a re-analysis of data by Arié)

REMAINING SPECTROSCOPY RELATED PROBLEMS

Non exhaustive list

CROSS-SECTION SUB-DATABASE

INFRARED cross-sections sub-database

CFC-11, CFC-12, CFC-13, CFC-14, HCFC-22, 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, CCl4

C2F6 PerfluoroethaneC3H8 PropaneC2H6 ethaneC2H2 acetyleneC2H4 etheneSF5CF3 trifluoromethyl sulfur pentafluoride CHF2CH2F (HFC-143), SF5CF3, C4F8, HNO4, HCH-365mfc

GEISA-03 UV/VIS cross-sections sub-databaseSpectral range 230 – 1333 nm

11 molecular species ; 180 T,P sets

Next update : June 2008

Courtesy of J. Orphal

No update

ACKNOWLEDGMENTS

to

CNES, CNRS/INSU and EUMETSAT

for their Encouragements and Supports