The Odin satellite

Frisk, U.; Hagström, Magnus; Ala‐Laurinaho, Juha; Andersson, Stefan; Berges, J.; Chabaud, J. P.; Dahlgren, Magnus; Emrich, Anders; Floren, G.; Florin, Gunnar; Fredrixon, Mathias; Gaier, T.; Haas, Rüdiger; Hirvonen, T.; Hjalmarson, Å.; Jakobsson, Björn; Jukkala, P.; Kildal, Per-Simon; Kollberg, E.; Lassing, J.; Lecacheux, A.; Lehikoinen, P.; Lehto, A.; Mallat, Juha; Marty, C.; Michet, D.; Narbonne, J.; Nexon, M.; Olberg, M.; Olofsson, H.; Olofsson, G.; Origné, A.; Petersson, Martin; Piirone, P.; Pouliquen, Dominque; Ristorcelli, I.; Rosolen, C.; Rouaix, G.; Räisänen, Antti V.; Serra, G.; Sjöberg, Fredrik; Stenmark, Lars; Torchinsky, S.; Tuovinen, J.; Ullberg, C.; Vinterhav, E.; Wadefalk, Niklas; Zirath, Herbert; Zimmermann, Peter; Zimmermann, Rüdiger

doi:10.1051/0004-6361:20030335

Cited by 184 publications

(104 citation statements)

References 12 publications

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“…Odin is a combination of astronomy and aeronomy missions with equal time disposition. OSIRIS is dedicated to aeronomy studies [Murtagh et al, 2002] and a second instrument, the Submillimeter and Millimeter Radiometer (SMR) [Frisk et al, 2003] carries out both aeronomy and astronomy studies. The instruments are coaligned and scan the limb of the atmosphere over a tangent height range 7 km to 70 km in approximately 85 seconds during normal stratospheric operations through controlled nodding of the satellite.…”

Section: Osiris Instrumentmentioning

confidence: 99%

Validation of Odin/OSIRIS stratospheric NO₂ profiles

Brohede¹,

Haley²,

McLinden³

et al. 2007

J. Geophys. Res.

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[1] This paper presents the validation study of stratospheric NO 2 profiles retrieved from Odin/OSIRIS measurements of limb-scattered sunlight (version 2.4). The Optical Spectrograph and Infrared Imager System (OSIRIS) NO 2 data set is compared to coincident solar occultation measurements by the Halogen Occultation Experiment (HALOE), Stratospheric Aerosol and Gas Experiment (SAGE) II, SAGE III, and Polar Ozone and Aerosol Measurement (POAM) III during the 2002-2004 period. Comparisons with seven Systeme d'Analyse par Observation Zenithal (SAOZ) balloon measurements are also presented. All comparisons show good agreement, with differences, both random and systematic, of less than 20% between 25 km and 35 km. Inconsistencies with SAGE III below 25 km are found to be caused primarily by diurnal effects from varying NO 2 concentrations along the SAGE III line-of-sight. On the basis of the differences, the OSIRIS random uncertainty is estimated to be 16% between 15 km and 25 km, 6% between 25 km and 35 km, and 9% between 35 km and 40 km. The estimated systematic uncertainty is about 22% between 15 and 25 km, 11-21% between 25 km and 35 km, and 11-31% between 35 km and 40 km. The uncertainties for AM (sunrise) profiles are generally largest and systematic deviations are found to be larger at equatorial latitudes. The results of this validation study show that the OSIRIS NO 2 profiles are well behaved, with reasonable uncertainty estimates between 15 km and 40 km. This unique NO 2 data set, with more than hemispheric coverage and high vertical resolution will be of particular interest for studies of nitrogen chemistry in the middle atmosphere, which is closely linked to ozone depletion.

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Section: Osiris Instrumentmentioning

confidence: 99%

Validation of Odin/OSIRIS stratospheric NO₂ profiles

Brohede¹,

Haley²,

McLinden³

et al. 2007

J. Geophys. Res.

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“…The spectrum of the H 2 O (1 10 − 1 01 ) line at 557 GHz (λ = 538.29 µm) was observed by the Odin satellite towards W Hya using the autocorrelation spectrometer (Nordh et al 2003;Frisk et al 2003). The resulting spectrum is a combination of two separate observing sessions, in December 2002 and July 2003, of a total of 185 orbits.…”

Section: Observationsmentioning

confidence: 99%

W Hya through the eye of Odin

Justtanont¹,

Bergman²,

Larsson³

et al. 2005

A&A

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Abstract. We present Odin observations of the AGB star W Hya in the ground-state transition of ortho-H 2 O, 1 10 − 1 01 , at 557 GHz. The line is clearly of circumstellar origin. Radiative transfer modelling of the water lines observed by Odin and ISO results in a mass-loss rate of (2.5 ± 0.5) × 10 −7 M yr −1 , and a circumstellar H 2 O abundance of (2.0 ± 1.0) × 10 −3 . The inferred mass-loss rate is consistent with that obtained from modelling the circumstellar CO radio line emission, and also with that obtained from the dust emission modelling combined with a dynamical model for the outflow. The very high water abundance, higher than the cosmic oxygen abundance, can be explained by invoking an injection of excess water from evaporating icy bodies in the system. The required extra mass of water is quite small, on the order of ∼0.1 M ⊕ .

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“…Measurements of water production rates allow us to determine the relative abundances of cometary volatiles, whose production rates are measured at the same time. The Odin satellite (Nordh et al 2003;Frisk et al 2003) was launched on 20 February 2001 on a Sun-synchronous polar orbit. Odin houses a radiometer with a 1.1-m primary mirror and five receivers at 119 GHz, 486-504 GHz, and 541-580 GHz, which are frequencies that are in large part unobservable from the ground.…”

Section: Introductionmentioning

confidence: 99%

Periodic variation in the water production of comet C/2001 Q4 (NEAT) observed with the Odin satellite

Biver¹,

Bockelée‐Morvan²,

Colom³

et al. 2009

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Context. Comet C/2001 Q4 (NEAT) was extensively studied with the 1.1-m submillimetre telescope of the Odin satellite. The H 2 O line at 557 GHz was regularly observed from 6 March to 16 May 2004 and nearly continuously monitored during 3 periods between 26 April and 2 May 2004. Aims. This last set of data shows periodic variations in the line intensity, and we looked for characterising the long-and short-term behaviour of this comet. Methods. We used the variance ratio method and χ 2 minimization to find the period of variation in the water production rate and simulations to infer its amplitude at the nucleus surface. Results. A 40% periodic variation in the water production rate is measured with a period of 0.816 ± 0.004 day (19.58 ± 0.1 h). The comet also exhibits a seasonal effect with a mean peak of outgassing around 2.7 × 10 29 molec. s −1 taking place about 18 days before perihelion.

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The Odin satellite

Cited by 184 publications

References 12 publications

Validation of Odin/OSIRIS stratospheric NO₂ profiles

Validation of Odin/OSIRIS stratospheric NO₂ profiles

W Hya through the eye of Odin

Periodic variation in the water production of comet C/2001 Q4 (NEAT) observed with the Odin satellite

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The Odin satellite

Cited by 184 publications

References 12 publications

Validation of Odin/OSIRIS stratospheric NO2 profiles

Validation of Odin/OSIRIS stratospheric NO2 profiles

W Hya through the eye of Odin

Periodic variation in the water production of comet C/2001 Q4 (NEAT) observed with the Odin satellite

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Validation of Odin/OSIRIS stratospheric NO₂ profiles

Validation of Odin/OSIRIS stratospheric NO₂ profiles