EPSC Abstracts Vol. 6, EPSC-DPS20l1-PREVIEW, 2011 EPSC-DPS Joint Meeting 2011 @ Author(s) 2011 An Extended View of Mars Ozone K. E. Fast (I), T. Kostiuk (I), F. Lefevre (2), T. Hewagama (3), T. A. Livengood (4) and R. L. Smith (I) (1) NASA Goddard Space Flight Center, Greenbelt, Maryland, USA ([email protected]),(2)LATMOS,CNRS,Paris, France, (3) University of Maryland, College Park, Maryland, USA, (4) National Center for Earth and Space Science Education, Capito! Heights, Mal),Iand, USA Abstract observations of ozone on Mars possible from the ground, with suffi-cient spectral resolving power We present an ongoing effort to characterize (/,!llA> I 06) to distinguishing it from telluric features chemistry in Mars' atmosphere in multiple seasons [5,6]. The synergistic combination of space-based on timcscales longer than flight missions through and ground-based measurements is a powerful tool coordinated efforts by GSFC's HIPWAC for investigating long-term behavior and supports a spectrometer and Mars Express SPICAM, archival more complete interpretation of ozone chemistry. measurements, and tests/application of photochemical models. The trace species ozone (03) 2. Probing Chemistry and Climate is an effective probc of atmospheric chemistry because it is destroyed by chemically active odd IlIPWAC (!Ol<.l) ~"d SPICM,\ illac<S) 2coa. MY2ll; IRIl$ (h.~ohoo.l. \W3. 1.~Y2' hydrogen species (HO;,J that result from water vapor photolysis. Observed ozone abundance on Mars is a critical test for three-dimensional photochemistry coupled general circulation models (GCM) that make specific predictions for the spatial, diurnal, and seasonal behavior of ozone and related chemistry and climatological conditions. Coordinated measurements by HIPW AC and SPICAM quantitatively linked mission data (0 the 23-year GSFC ozone data record and also revealed unanticipated inter-decadal Figure I: Coordinated campaigns with GSFC's variability of same-season ozon~ abundances, a HIPW AC and Mars Express SPICAM tied mission possible indicator of changing cloud activity data previous heterodyne measurements and revealed (heterogeneous sink for HOx). A detailed study of unanticipated long-term variability at low latitudes in long-tenn conditions is critical to characterizing the the spring, possibly due to heterogencous chemistry predictability of Mars' seasonal chemical behavior, driven by cloud aetivity [4]. particularly in light of the implications of and the lack of explanation for reported methane behavior. Previous coordinated measurements by HIP\VAC and SPICAM [4] quantitatively linked mission data 1. Introduction to the 23-year IR heterodyne ozone data record through simultancous measurements and by verifying ESA's Mars Express SPICAM [I] is the first in column abundance retrievals from IR and UV stnunent to study ozone from Mars orbit since Mari spectroscopic techniques. Further measurements in ner 9 (1971-72), operating from 2004 to the present. December 2009 and Mareh 2010 made by HIPWAC Spectroscopy of ozone from the NASA Infrared in direct coordination vl/ith SPICAM operation arc an Telescope Facility with GSFC's InfraRed Hetero additional source of verification. The coordinated dyne Spectrometer (JRHS, decommissioned) and efforts arc the basis for studying long-term behavior, Heterodyne Instrument for Planetary Wind And by validating direct quantitative comparison between Composition (HIPWAC) dates from 1988 to the pre SPICAM measurements in this decade and IR sent [2,3,4], in seasons accessible during Mars appa heterodyne measurements made prior to the Mars ritions and covering the lailer half of a 32-ycar gap in Express mission and in previous decades. The work the spacecraft record. These infrared heterodyne revealed unanticipated inter-decadal variability from measurements (~9.5 Jlm) are the only direct ozone abundances measured by HIPWAC and SPICAM in 2008 and by IRHS in 1993 (Fig. I). heterodyne measurements are also used to test High latitude measurements arc generally consistent photochemical model predictions [e.g., 10,11] so that but differences in the low latitude retrievals arc they can be used to interpret past mcasurcmcnts and significant. Column abundances measured by IRHS determine the importance of chemical and in 1993 (MY21) are consistently -2-4 times higher climatological processes indicated by the observed than those retrieved by the functionally equivalent behavior, such as heterogeneous chemistry catalyzed HIPWAC and by SPICAM in 2008 (MY29), eight by cloud particles. Martian years lator during the same northern mid spring season. This increased OZOl1e may be an Mars 11 Dec2009 40'N indicator of increased cloud activity at low latitudes serving as a sink for ozone-destroying species, as indicated by photochemical modeling of heterogeneous chemical processes [4,10,11]. Archival IR heterodyne measurements compared to Hubble Space Telescope (HST) UV measurements [7,8] showed generally consistent retrievals for con temporaneous observations as well as for those at similar seasons (LS) within a few years of each other [3]. However, during LS~60'-90' (late northern Figure 2: Ozone (03) absorption features at 9.7 Ilm spring) both HST and IRHS yielded approximately measured by HIPWAC (histogram) in Dec. 2009 at two to five times more ozone in the 1990's than was the NASA Infrared Telescope Facility in observed by SPICAM at similar seasons, but one coordination with Mars Express SPICAM. decade later. This was attributed to possible interan~ Temperature is simultaneously constraincd by the nual variability by Perrier et al. [9], who did not re~ CO2 absorption profile in radiative transfer modeling port such variability during the two consecutive (solid curve). Martian springs measured by SPICAM at the time. These snapshots arc significant, as photochcmical Acknowledgements models have generally been checked against combined ground~based and spacecraft mcasure~ This work was supported by NASA's Planetary mcnts made over all Martian years that have avail~ Astronomy Program. K. E. Fast, T. Kostiuk and T. A. able data [e.g., 10,11,12]. Although ozone exhibits Livengood were Visiting Astronomers at the Infrared large spatial, diurnal, and seasonal variability, year~ Telescope Facility, which is operalcd by the to~year and inter~decadal variability are 110t well University of Hawaii under Cooperative Agreement studied and can probe climatology. A detailed study No. NNX~08AE38A with the National Aeronautics of long~term behavior is critical to refining photo~ and Space Administration, Science Mission chemical models and to characterizing the predict~ Directorate, Planetary Astronomy Program. ability of Mars' seasonal behavior and the variability of its dimate. References 3, Recent Work [1] Bert<lux, J.~L., ot a!., Planet. Space Sci. 48,1303-1320. [2) Espenak, F. ct al. (1991), Icarus, 92, 252·262. [3] Fast, We introduce HIPWAC measurements of ozonc K. E.. et al. (2006), learns, 181,410-431. [4] Fast, K. Eo. ct made during the last Mars apparition, in December al. (2009), Icarus, 203, 20~27. [5J Kostiuk, T. and Mumma 2009 (e.g., Fig. 2) and in March 2010. These M.1. (1983) Appl. Opt., 17,2644-2654. [6] Kostiuk, T. (1994), Infrared Phys. Teehnol., 35, 243-266. [7) Clancy, R. observations were made in direct coordination with T. ct al. (1999), Icarus 138,49-63. [8] Clancy, R. T. ct al. Mars Express SPICAM and are sources of additional (1996), Journal Geophys. Res. 10 I, 12,777-12,783. [9) verification of consistent total ozone column Perrier, S. et al. (2006), J. Gcophys. Res., III, E09S06. [10] abundance retrievals from the two techniques. This Lefevre, F. et al. (2004), J. Geophys. Res., 109, £07004. strengthens the basis for quantitative study of long~ [II] Lefevre, F. et al. (2008), Nature, 454, 971-975. [12] term ozone variability in multiple seasons all Fast, K. E.. et al. (2006), Icarus, 183,396-402. timescalcs longer than current missions. Recent