Total Column Ozone Climatology From My34 To My36
From Measurements By The Nomad-Uvis Spectrometer.
J.P. Mason, M.R. Patel, J.A. Holmes, P. Streeter, J. Alday, M. Brown, G. Sellers, C. Marriner, S.R Lewis,
School Of Physical Sciences, The Open University, Milton Keynes Uk (Jon.Mason@Open.Ac.Uk), M.J. Wolff,
Space Science Institute, Boulder, Co, U.S.A, Y. Willame, C. Depiesse, B. Ristic, I. Thomas, F. Daerden, A.C.
Vandaele, Royal Belgian Institute For Space Aeronomy Bira-Iasb Belgium, J.-J. Lopez-Moreno, Instituto De
Astrofìsica De Andalucía/Csic, Granada, Spain, G. Bellucci, Istituto Di Astrofisica E Planetologia Spaziali,
Inaf, Rome, Italy.

Introduction: Near Continuous Radiance Measurements Of The Martian Atmosphere In The 200650 Nm Wavelength Range By The Ultraviolet And
Visible Spectrometer (Uvis) (Patel Et Al., 2017) As
Part Of The Nomad Instrument On The Exomars
Trace Gas Orbiter (Tgo) (Vandaele, Et Al., 2018)
Provides A Powerful Tool For Investigating The Ozone
Climatology, The Water Cycle (From The Wellestablished Photochemical Anti-Correlation Between
Water Vapour And Ozone), And By Extension Photochemical Reactions In The Martian Atmosphere.
Previous Observations Have Shown That, Spatially,
Ozone Is Observed In Three Main Regions (1) At High
Northern Latitudes (50° - 90° N) Through The Northern
Autumn, Winter And Spring Seasons, (2) At Equivalent