Detection of a tropospheric ozone anomaly using a newly developed ozone retrieval algorithm for an up-looking infrared interferometer

Author Posting. © American Geophysical Union, 2009. This article is posted here by permission of American Geophysical Union for personal use, not for redistribution. The definitive version was published in Journal of Geophysical Research 114 (2009): D06304, doi:10.1029/2008JD010270.On 2 June 2003, the Baltimore Bomem Atmospheric Emitted Radiance Interferometer (BBAERI) recorded an infrared spectral time series indicating the presence of a tropospheric ozone anomaly. The measurements were collected during an Atmospheric Infrared Sounder (AIRS) validation campaign called the 2003 AIRS BBAERI Ocean Validation Experiment (ABOVE03) conducted at the United States Coast Guard Chesapeake Light station located 14 miles due east of Virginia Beach, Virginia (36.91°N, 75.71°W). Ozone retrievals were performed with the Kurt Lightner Ozone BBAERI Retrieval (KLOBBER) algorithm, which retrieves tropospheric column ozone, surface to 300 mbar, from zenith-viewing atmospheric thermal emission spectra. KLOBBER is modeled after the AIRS retrieval algorithm consisting of a synthetic statistical regression followed by a physical retrieval. The physical retrieval is implemented using the k-Compressed Atmospheric Radiative Transfer Algorithm (kCARTA) to compute spectra. The time series of retrieved integrated ozone column on 2 June 2003 displays spikes of about 10 Dobson units, well above the error of the KLOBBER algorithm. Using instrumentation at Chesapeake Light, satellite imaging, trace gas retrievals from satellites, and Potential Vorticity (PV) computations, it was determined that these sudden increases in column ozone likely were caused by a combination of midtropospheric biomass burning products from forest fires in Siberia, Russia, and stratospheric intrusion by a tropopause fold occurring over central Canada and the midwestern United States.NASA for its support through grant NAG5- 1156-7 for AIRS Validation and grant NNG04GN42G for development of AIRS trace gas products, and through a subcontract with JPL on the AIRS Project prime contract NAS7-03001 for continuing optimization and validation of AIRS trace gas products.

HIGH RESOLUTION INFRARED SPECTRA OF THE 18O16O18O(C2ν^{18}O^{16}O^{18}O(C_{2}\nu) OZONE MOLECULE (1200 TO 500cm−1500 cm^{-1}. LINE POSITIONS

Author Institution: Groupe de Spectrom\'etrie Mol\'eculaire et Atmosph\'erique, UMR CNRS 6089 Universit\'e de Reims - Moulin de la Housse - BP 1039After the previous systematic analysis of $^{16}O{_{3}}^{1}, {^{18}}O{_{3}}{^{2}},{^{16}}O^{18}O^{16}O{^{3,4}}$ in medium infrared, we present here the results of the analysis of new $^{18}O^{16}O^{18}O$ observed bands. The spectra have been recorded with the FTS of $Reims^{5,6}$, with a resolution of $0.006cm^{-1}$, and products pathlength $\times$ pressure up to $32 m \times 3$ Torr. The data reduction to derive line positions uses a new multifit $program^{7}$. The analysis of spectra is performed using the same formalism as in references [1-4], using standard Watson's Hamiltonian for diagonal blocks and Coriolis and Fermi resonances for off diagonal blocks. 8 polyads have been analysed, among them 7 being analysed for the first time. They correspond to 10 observed bands (underlined) in interaction with ``dark'' bands. $\begin{array}{l}(\nu_{1}, \nu_{3}); (\nu_{2}+\nu_{3}, \nu_{1}+\nu_{2}); (\nu_{2}+2\nu_{3},\nu_{1}+\nu_{2}+\nu_{3}, 2\nu_{1}+\nu_{2}); (3\nu_{3}, \nu_{1}+2\nu_{3},2\nu_{1}+\nu_{3}); \\ (\nu_{2}+3\nu_{3}); (\nu_{1}+3\nu_{3}, 4\nu_{3}); (\nu_{1}+\nu_{2}+3\nu_{3},\nu_{2}+4\nu_{3}) and (5\nu_{3})\end{array}$ We give here the range of J and $K_{a}$ for observed transitions, statistics for energy levels, spectroscopic parameters and resonance coupling parameters. Acknowledgments: Authors thank S.A Tashkun for use of GIP programs, X. Thomas and P. Von der Heyden for recording spectra, L. R\'{e}galia and J. J. Plateaux for the use of multifit program. 1. S. M. Mikhailenko, A. Barbe, VI. G. Tyuterev and A. Chichery, Atmos. Oceanic Opt., 12, 9 (1999) 2. A. Chichery, A. Barbe, VI. G. Tyuterev, J. Molecular Spectrosc., 206, 1 - 26 (2001) 3. A. Chichery, A. Brabe, VI. G. Tyuterev, S.A. Tashkun, J. Molecular Spectrosc., 205, 347-349 (2001) 4. M. R. De Backer Barilly, A. Barbe, VI. G. Tyuterev, A. Chichery, Mol. Phys., accepted (2002). 5. J.J. Plateaux, A. Barbe, and A. Delahaigue, Spectrochim. Acta, A 51, 1153-1196 (1995). 6. L. R\'{e}galia, Thesis Universit\'{e} de Reims, (France) (1996). 7. J.J. Plateaux, L. R\'{e}galia, C. Boussin and A. Barbe, J.Q.S.R.T., 68, 507-520 (2001)

INFRARED HIGH RESOLUTION SPECTRA OF 16^{16}O3_3 : THE WEAK 3ν23\nu_2+3ν33\nu_3 AND 4ν24\nu_2+4ν34\nu_3 BANDS

Author Institution: Groupe de Spectrometrie Moleculaire et Atmospherique; U.M.R. CNRS 6089, Universite de REIMS, Moulin de la Housse, B.P. 1039; 51687 REIMS cedex 2, FRANCE; Laboratoire de Spectrometrie Physique, U.M.R. CNRS 5588, Universite Joseph Fourier; B.P. 87, 38402 Saint Martin d'Heres cedex, FRANCERecent progress in theory and improvement of sensitivity of experiments allow assigning new very weak bands of ozone, $^{16}$O$_3$. The $3\nu_2$+$3\nu_3$ near 5000 cm$^{-1}$ and the $4\nu_2$+$4\nu_3$ near 6500 cm$^{-1}$ are reported for the first time from the FTS and CRDS spectra respectively. The second band is particularly interesting, as transitions involving vibrational states with a $v_2$ = 4 bending excitation were never observed so far. Hamiltonian and dipole moment parameters, range of observed quantum numbers, statistics of the fits, comparison of band centres with predictions, as well as several agreements between observed and calculated spectra will be presented and discussed

CW-CRDS SPECTRA OF 16^{16}O3_3 FROM 5970 TO 6200 CM−1^{-1}: 2052 TRANSITIONS ASSIGNED AND ANALYSED

Author Institution: GSMA, B.P. 1039, 51687 Reims, France; LSP, B.P. 87, 38402 Grenoble, FranceThe high resolution CW-CRDS infrared spectra of ozone have been recorded in the 5970-6200 cm$^{-1}$ spectral range. The high sensitivity allow to observe very weak lines. In this region, only two A type bands centred at 6063 and 6124 cm$^{-1}$ were previously analysed}, \underline{780}, 223 (2006)}. Here, thanks to the record of new spectra, we largely extend the range of their observed quantum numbers, and, first of all, we observe three B type bands: $2\nu_1 +3\nu_2 +2\nu_3$ (138 transitions), $5\nu_1 +\nu_2$ (16 transitions), and $\nu_1+2\nu_2 + 4\nu_3$ (499 transitions). It is necessary to include 6 vibrational levels in the Hamiltonian model, accounting of many resonances to correctly (r.m.s=6x 10$^{-3}$ cm$^{-1}$ reproduce the observed positions. In addition, transition moment are fitted. Finally, more than 95\% of all experimentally observed lines are assigned and are satisfactorily reproduced, accounting of the difficulty of analyses of levels not far from the dissociation

Fourier transform and high sensitivity cw-cavity ringdown absorption spectroscopies of ozone in the in the 6030-6130 cm –1 region. First observation and analysis of the 3v1 + 3v3 and 2v2 + 5v3 bands

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FIRST OBSERVATION AND ANALYSIS OF THE 3ν13\nu_1+3ν33\nu_3 AND 2ν22\nu_2+5ν35\nu_3 BANDS OF OZONE

Author Institution: Groupe de Spectrometrie Moleculaire et Atmospherique,; U.M.R. CNRS 6089, Universite de REIMS, Moulin de la Housse, B.P. 1039,; 51687 REIMS cedex 2, FRANCE; Laboratoire de Spectrometrie Physique, U.M.R. CNRS 5588, Universite Joseph Fourier; B.P. 87, 38402 Saint Martin d'Heres cedex, FRANCEUsing FTS and CW-CRDS spectrometer, high resolution spectra of ozone have been recorded with high sensitivity (respectively 8x10$^{-8}$ and 3x10$^{-10}$ cm$^{-1}$) in the range 6030-6130 cm$^{-1}$. Two A-type bands ($\Delta Ka=0$) have been observed. 391 transitions for the $3\nu_1$+$3\nu_3$ band and 280 transitions for the $2\nu_2$+$5\nu_3$ band have been assigned. In order to correctly reproduce the observations, it has been necessary to include three dark perturbing states. Transition moment parameters have been derived and a complete listing is calculated. We present spectra, Hamiltonian parameters, transition moment parameters as well as agreement between calculated and observed spectra in various spectral ranges

OZONE : FIRST OBSERVATION OF THE 2ν12\nu_1+3ν23\nu_2+ν3\nu_3 BAND

Author Institution: Groupe de Spectrometrie Moleculaire et Atmospherique; U.M.R. CNRS 6089, Universite de REIMS, Moulin de la Housse, B.P. 1039; 51687 REIMS cedex 2, FRANCE; Groupe de Spectrometrie Moleculaire et Atmospherique; U.M.R. CNRS 6089, Universite de REIMS, Moulin de la Housse, B.P. 1039; 51687 REIMS cedex 2, FRANCEThis work continuous the systematic study of ozone in the infrared. Thanks to available predictions of band centres and rotational constants , \textbf{$316$}, 271-279, (2000).} and the improvement of signal/noise ratios of observed spectra, we are able to observe weaker and weaker bands. It is the case of the $2\nu_1$+$3\nu_2$+$\nu_3$ band, which lies in the 5160 cm$^{-1}$ spectral range. The spectrum has been recorded with the FTS of GSMA , (1996).}, with a path length of 36 metres and a pressure of 41.0 Torr. The transitions are derived with a precision better than $1\times 10^{-3}$ cm$^{-1}$ for wavenumbers and 10\% for the intensities. The analyse has been performed using effective Hamiltonian, and transition moment operators. 430 transitions have been assigned, with $J=34$, $Ka=11$. They are reproduced with an rms = $2\times 10^{-3}$ cm$^{-1}$, close to the experimental accuracy. Only one level $(24_3)$ has found to be slightly perturbed (Obs-Calc=-0.011 cm$^{-1}$). The perturber has easily been identified, as the $24_2$ level of the (302)state. It is particularly interesting that this level was known, derived from our analyse of the (302)-(001) band , \textbf{$102$}, 1707-1716, (2004).}, with a shift (Obs-Calc=+0.011 cm$^{-1}$), confirming the validity of both analyses. We present here the results, with spectroscopic parameters (including the resonance with the (302) state, effective transition moment operators, integrated band intensities, portion of created linelists available for databanks and examples of agreements between observed and calculated spectra