Assessment of the quality of OSIRIS mesospheric temperatures using satellite and ground-based measurements

Sheese, Patrick E.; Strong, Kimberly; Llewellyn, E. J.; Gattinger, R. L.; Russell, James M.; Boone, C. D.; Hervig, Mark E.; Sica, R. J.; Bandoro, Justin

doi:10.5194/amt-5-2993-2012

Cited by 17 publications

(16 citation statements)

References 33 publications

(39 reference statements)

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“…The temperature data also exhibit a cold bias of 10-15 K near 85 km (Sheese et al, 2011) (the upper boundary of the Rayleighscatter-derived temperatures) and a cold bias of 5-15 K near 48 km due to multiple scattering effects not taken into account in the retrieval. However, between 55 and 80 km, these temperatures are valid and are typically within 4-5 K of other satellite data (Sheese et al, 2012).…”

Section: Osiris Datamentioning

confidence: 52%

“…A comparison with these temperatures is therefore not included here. Instead, OSIRIS temperatures derived from the O 2 A-band emission spectra near 762 nm (see Sheese et al, 2010Sheese et al, , 2012, for details) are used. Temperature data are available between 45 and 110 km, but temperatures between 80 and 86 km are deemed unreliable, due to uncertainties in O 2 absorption in the A-band.…”

Section: Osiris Datamentioning

confidence: 99%

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Comparison of the CMAM30 data set with ACE-FTS and OSIRIS: polar regions

Pendlebury

Plummer²,

Scinocca³

et al. 2015

Atmos. Chem. Phys.

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Abstract. CMAM30 is a 30-year data set extending from 1979 to 2010 that is generated using a version of the Canadian Middle Atmosphere Model (CMAM) in which the winds and temperatures are relaxed to the Interim Reanalysis product from the European Centre for Medium-Range Weather Forecasts (ERA-Interim). The data set has dynamical fields that are very close to the reanalysis below 1 hPa and chemical tracers that are self-consistent with respect to the model winds and temperature. The chemical tracers are expected to be close to actual observations. The data set is here compared to two satellite records -the Atmospheric Chemistry Experiment Fourier transform spectrometer and the Odin Optical Spectrograph and Infrared Imaging System -for the purpose of validating the temperature, ozone, water vapour and methane fields. Data from the Aura microwave limb sounder are also used for validation of the chemical processing in the polar vortex. It is found that the CMAM30 temperature is warmer by up to 5 K in the stratosphere, with a low bias in the mesosphere of ∼ 5-15 K. Ozone is reasonable (±15 %), except near the tropopause globally and in the Southern Hemisphere winter polar vortex. Water vapour is consistently low by 10-20 %, with corresponding high methane of 10-20 %, except in the Southern Hemisphere polar vortex. Discrepancies in this region are shown to stem from the treatment of polar stratospheric cloud formation in the model.

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Section: Osiris Datamentioning

confidence: 52%

Section: Osiris Datamentioning

confidence: 99%

Comparison of the CMAM30 data set with ACE-FTS and OSIRIS: polar regions

Pendlebury

Plummer²,

Scinocca³

et al. 2015

Atmos. Chem. Phys.

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“…Shepherd et al (2001) determined temperature profiles from 65 to 90 km during the period March 1992 -January 1994 analysing WINDII/UARS data at 553nm. More recently Sheese et al (2012) retrieved temperature profiles using OSIRIS/Odin bright limb observations at 318.5 and 347.5 nm in the altitude range 45-85 10 km. In the frame of the ESA funded MesosphEO project, a new dataset of temperature profiles in the altitude range 35-85 km was created from the analysis of GOMOS/ENVISAT bright limb observations in the spectral band 420-480 nm.…”

Section: Mls (Microwave Limb Sounder On the Aura Satellite) And Sabermentioning

confidence: 99%

A new MesosphEO dataset of temperature profiles from 35 to 85 km using Rayleigh scattering at limb from GOMOS/ENVISAT daytime observations

Hauchecorne¹,

Blanot

Wing³

et al. 2018

Preprint

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Abstract. Given that the scattering of sunlight by the Earth's atmosphere above 30–35 km is primarily due to molecular Rayleigh scattering, the intensity of scattered photons can be assumed to be directly proportional to the atmospheric density. From the measured relative density profile it is possible to retrieve an absolute temperature profile by assuming local hydrostatic equilibrium, the perfect gas law, and an a priori temperature from a climatological model at the top of the atmosphere. This technique is applied to Rayleigh lidar observations for over 35 years. The GOMOS star occultation spectrometer included spectral channels to observe daytime limb scattered sunlight close to the star direction. GOMOS Rayleigh scattering profiles in the spectral range 420–480 nm have been used to retrieve temperature profiles in the altitude range 35–85 km with a 2-km vertical resolution. A database of more than 309,000 temperature profiles has been created. A global climatology was built and compared to GOMOS external model. In the upper stratosphere, where the external model is based on ECMWF analysis, the agreement is better than 2 K. In the mesosphere, where the external model follows MSIS climatology, 5 to 10 K differences are observed. Comparison with nighttime collocated Rayleigh lidar profiles above south of France shows some differences with a vertical structure that may be at least partially explained by the contribution of thermal diurnal tide. The temperature evolution obtained at Equator indicates the occurrence of mesospheric inversion layers in the temperature profile with global longitudinal extension, descending in about one month from 80 to 70 km. The climatology shows a semi-annual variation in the upper stratosphere, a stratopause altitude varying between 47 and 54 km and an annual variation in the mesosphere. The technique to derive temperature profiles from Rayleigh scattering at limb can be applied to any other limb-scatter sounder providing observation in the spectral range 350–500 nm. This is also a good candidate for a future small satellite constellation due to the simplicity of the principle.

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“…OSIRIS retrieved temperature profiles were compared to SABER, SOFIE, ACE-FTS v2.2, and ACE-FTS v3.0 (Sheese et al, 2012). Comparison with ACE-FTS found that ACE-FTS was 9 K warmer at 48 km but less than 3 K warmer between 60 and 80 km.…”

Section: Ace-fts Data Setsmentioning

confidence: 99%

New temperature and pressure retrieval algorithm for high-resolution infrared solar occultation spectroscopy: analysis and validation against ACE-FTS and COSMIC

et al. 2016

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Abstract. Motivated by the initial selection of a high-resolution solar occultation Fourier transform spectrometer (FTS) to fly to Mars on the ExoMars Trace Gas Orbiter, we have been developing algorithms for retrieving volume mixing ratio vertical profiles of trace gases, the primary component of which is a new algorithm and software for retrieving vertical profiles of temperature and pressure from the spectra. In contrast to Earth-observing instruments, which can rely on accurate meteorological models, a priori information, and spacecraft position, Mars retrievals require a method with minimal reliance on such data. The temperature and pressure retrieval algorithms developed for this work were evaluated using Earth-observing spectra from the Atmospheric Chemistry Experiment (ACE) FTS, a solar occultation instrument in orbit since 2003, and the basis for the instrument selected for a Mars mission. ACE-FTS makes multiple measurements during an occultation, separated in altitude by 1.5–5 km, and we analyse 10 CO2 vibration–rotation bands at each altitude, each with a different usable altitude range. We describe the algorithms and present results of their application and their comparison to the ACE-FTS data products. The Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) provides vertical profiles of temperature up to 40 km with high vertical resolution. Using six satellites and GPS radio occultation, COSMIC's data product has excellent temporal and spatial coverage, allowing us to find coincident measurements with ACE with very tight criteria: less than 1.5 h and 150 km. We present an intercomparison of temperature profiles retrieved from ACE-FTS using our algorithm, that of the ACE Science Team (v3.5), and from COSMIC. When our retrievals are compared to ACE-FTS v3.5, we find mean differences between −5 and +2 K and that our retrieved profiles have no seasonal or zonal biases but do have a warm bias in the stratosphere and a cold bias in the mesosphere. When compared to COSMIC, we do not observe a warm/cool bias and mean differences are between −4 and +1 K. COSMIC comparisons are restricted to below 40 km, where our retrievals have the best agreement with ACE-FTS v3.5. When comparing ACE-FTS v3.5 to COSMIC we observe a cold bias in COSMIC of 0.5 K, and mean differences are between −0.9 and +0.6 K.

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Assessment of the quality of OSIRIS mesospheric temperatures using satellite and ground-based measurements

Cited by 17 publications

References 33 publications

Comparison of the CMAM30 data set with ACE-FTS and OSIRIS: polar regions

Comparison of the CMAM30 data set with ACE-FTS and OSIRIS: polar regions

A new MesosphEO dataset of temperature profiles from 35 to 85 km using Rayleigh scattering at limb from GOMOS/ENVISAT daytime observations

New temperature and pressure retrieval algorithm for high-resolution infrared solar occultation spectroscopy: analysis and validation against ACE-FTS and COSMIC

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