: Science Update to CAPS Bob Pappalardo, Europa Clipper Project Scientist Jet Propulsion Laboratory, California Institute of Technology March 29, 2017 0 © 2017 California Institute of Technology. Government sponsorship acknowledged. NASA-Selected Radiation Science Working Group Europa Instruments radiation environment

MASPEX Mass Spectrometer SUDA sniffing atmospheric Dust Analyzer ICEMAG composition surface & plume Magnetometer PIMS composition sensing ocean Faraday Cups Europa-UVS properties plasma environment UV Spectrograph surface & plume/atmosphere EIS composition Narrow-Angle Camera + Wide-Angle Camera E-THEMIS MISE mapping alien landscape Thermal Imager IR Spectrometer in 3D & color searching for hot spots surface chemical fingerprints

REASON Ice-Penetrating Radar plumbing the ice shell

Gravity Science Working Group confirming an ocean

Remote Sensing In Situ 1-1 Europa Instrument Overview: EIS

EIS-NAC Europa Imaging System Narrow Angle Camera Produces visible maps of the surface of Europa, to describe its topography (including possible lander landing sites), understand its , and to search for plumes. PI: Zibi Turtle Johns Hopkins Applied Physics Laboratory

EIS-WAC Europa Imaging System Wide Angle Camera Feb. 22, 2017 3 Pre-Decisional Information — For Planning and Discussion Purposes Only Europa Instrument Highlights: EIS

Europa Imaging System (EIS): Zibi Turtle, PI • Adding color capability to NAC – Scattered light analysis shows that addition of color stripe filters will not impede plume detection – Increases opportunities to gimbal-target coordination with other instruments, extrapolating to small scales and other regions – 10 m color resolution from 1000 km – Can join the “joint scan” planned for each flyby giving 200 - 400 m/pixel hemispheric color – Extrapolate composition information to smaller scales and other regions Thera & Thrace: Galileo 220 m/pixel

Feb. 22, 2017 combined with 1.4 km/pixel color3 4 Pre-Decisional Information — For Planning and Discussion Purposes Only Europa Instrument Overview: REASON & MISE

Radar for Europa Assessment and REASON Sounding: Ocean to Near-surface Uses VHF and HF bands to investigate Europa’s ice shell, subsurface ocean, plumes, tides, and potential landing sites

PI: Don Blankenship Produces maps of organic University of Texas compounds, salts, hot spots Institute for and ices to assess habitability of the ocean and investigate geologic history of the surface

Pegasus Airfield PI: Diana Blaney Jet Propulsion Laboratory

MISE Mapping Imaging Spectrometer for Europa

Feb. 22, 2017 6 Pre-Decisional Information — For Planning and Discussion Purposes Only Europa Instrument Highlights: REASON Radar for Europa Assessment and Sounding: Ocean to Near-surface (REASON): Don Blankenship, PI • REASON can use both topography from MARSIS Data, Using Clutter Model from Topography EIS stereo imaging and VHF interferometry to distinguish off-nadir- Subsurface Echo surface from subsurface reflectors Surface Clutter • Developed tools to quantify the suppression and interferometric Interferometry ineffective discrimination of surface clutter for distinguishing nadir – Assists spacecraft design and future analyses from off-nadir where <0 dB • Helps to clarify issues affecting REASON performance, esp. below 50 km

Feb. 22, 2017 5 Pre-Decisional Information — For Planning and Discussion Purposes Only Europa Instrument Highlights: MISE

Mapping Imaging Spectrometer Offner Architecture for Europa (MISE): Diana Blaney, PI • Thermal accommodation is critical to MISE – Cryocooler performance testing is currently underway • Changed from Offner to Dyson spectrometer design, permitting reduction Dyson Architecture from 2 to 1 cryocooler – Reduces instrument mass, energy, cost – More compact, so less to cool – Greater light gathering improves S/N – No change to spectral range or requirements

Feb. 22, 2017 6 Pre-Decisional Information — For Planning and Discussion Purposes Only Europa Instrument Overview: Europa-UVS & E-THEMIS

Europa-UVS Europa Ultraviolet Spectrograph Characterizes thermal anomalies, active plumes, and surface properties Obtains ultraviolet images to support landing site assessment to explore Europa's and geology. composition and chemistry, search for plumes, and PI: Phil Christensen investigate connections with Europa’s environment

PI: Kurt Retherford Southwest Research Institute

E-THEMIS Europa Thermal Imaging System Feb. 22, 2017 Pre-Decisional Information — For Planning and Discussion Purposes Only Europa Instrument Highlights: Europa-UVS & E-THEMIS Europa Ultraviolet Spectrograph Solar Port KOZ (Europa-UVS): Kurt Retherford, PI • Working design to reduce angle to solar port, to permit smaller turns for solar occultations, while avoiding sun on SUDA KOZ Airglow/High-res • Designing open/close solar port door actuator Port FOV

Joint Scan Europa Thermal Imaging System E-THEMIS (E-THEMIS): Phil Christensen, PI FOV • Candidate detectors undergoing radiation and spectral response testing • Spacecraft scanning permits observing a range of local times of day on the surface Europa-UVS FOV Feb. 22, 2017 8 Pre-Decisional Information — For Planning and Discussion Purposes Only 10 D. Science InvestigEuropaation Instrument Overview: Background 1: Compositional Mapping

Europa is engulfed in a cloud of slow moving dust particles following 100 µm mSUDAicrometeoroid impacts & MASPEX ballistic orbits, ejected by continual bombardment of hypervelocity generate ~500 kg ejecta/second interplanetary meteoroids. A dust mass spectrometer such as SUDA SUDA @ 25 km measures the composition of the ejecta particles and traces each of the detects 40 ejecta/s detected grains back to the surface (upper figurSurfacee). Hence, SUD ADust will rela teAnalyzer the measuredSUDA composition to geological patterns and features on the Ejecta move on ballistic trajectories moon. 109 ejecta/km2s How many surface samples can be collected? The number of detectable ejectaD. dScienceuring a flybInyv oestigr a loationw altitude orbit can be esMeasurestimated by the dens theity composition of dust profile of Europa's well characterized ejecta cloud based on Galileo measurements (Krüger et al., 1999; Krivov et al., particles2003). The ejecta and size constrains geological Backgdrisotriundbuti o1n: Cappromopxiomasittelioy nafoll oMaws pap poingwer law with a slope of ~2.4 and ranges from ~100 nm up to the typical size of the impaactivitiesctor (about 100µ onm). and below the surface of

Europa is engulfed in a cloud of slowThe mo tovitangl madussst ejpaectedrticl esin afon lliompawingct on Eur100o µpam m faicrr oexceedmeteoroisd theimpa macts ss of the 860 km ballistic orbits, ejected by continuali mpabomctibngar dmeteoment roifd h(~17,yper000velo cx)ity (Kempfgen eet.rate a~5l, 02012)0Europa kg eje. cta As/sec oannd example, interplanetary meteoroids. A dust madsuris ngspectr eacho meterof the stwucho Euras opaSUD ClAipper 25 km flybys shown in the middle SUDA @ 25 km E9 measures the composition of the ejectafig urpaer tiSUDcles Aa ndwi lltra cocesllect ea 5000ch o sf athempl es originating from this area. detects 40 ejecta/s Thera Sniffs Europa’s detected grains back to the surface (upper figure). Hence, SUDA will relate Macula Ejecta move on the measured composition to geologiHocal wpa tternsis a coandmpo feasitituronaesl oman pthe g enerated? By PI:combi niSaschang many suchKempf m

ballistic trajectories k measurements a compositional map of the surface can be generated. For moon. 0 atmosphere and 8 E6 each particle detection, a two dimensional pr10o9LASP, baejecta/kmbility d2sis tri butiUniversityon is 9 of How many surface samples can be coldlectederived? Thefor itsnumber origin oof nd etectathe surfable ce. As an example, the middle figure Thrace Macula exosphere to determine ejectaD. duriScienceng a flybIny ovrestig a lowation altitude orbishot wcasn abe M esonte-timaCatedrl ob ys theimul daenstionity o f SUDA measurColoradoements during Eur Boulderopa profile of Europa's well characterizedCl ipperejecta 25 cl kmoud flyb bayss ed6 andon 9 Gaovlileoer the dark lobated features Thrace Macula their chemical measurements (Krüger et al., 1999; Kriandvo vThera et al ., M2003)acula. . TheEach ej ectacolo rsedize dot indicates the origin of an ejecta Backdgisrtrioundbutio 1n : aCppromoxipmaostelitioy nafolllo Maws pa ppoingdwetecteder law wbiyth SUD a slAope ra ondf o~2.ml4y alndaunched from inside (red) and outside 420 km composition ranges from ~100 nm up to the typical s(iyzeel lofw the) the impa feactoturre .( Theabout lo 100µwer figm)ur. e shows the resulting probability map The total mass ejected in an impact on Eurfor othepa faorir gexceedin of thes the detected mass o fpa therti cles from the dark features on Europa Europa is engulfed in a cloud of slow moving dust particles following 100 µm micrometeoroid impacts 860 km Probability for origin inside contour lines: ballistic orbits, ejected by continuaimpal boctimngba rmeteodmentr ooidf (h~17,yper000vel ox)cit y( Kempf(rgede n et.edrao teats l~5, i02012)n0 kmig edj.e dcl taeAs /sple coaot)nd exaif idmplentiefied, by their unique composition. SUDA interplanetary meteoroids. A dust maduriss ngs pectreacho ometerf the twsucho Eur aso paSUD CliApper c25an kmuna mflybbigysu osuhoslyw idn enint ifythe a mind ddchlea racterize the composition of the ThrE9ace SUDA @ 25 km PI: Hunter Waite measures the composition of the ejectafigur pae rSUDticlesA awndill cotrallcesect ea5000ch osaf mplthees oMarigicnaulati ngan dfr Tohmer thia Mas acrueala. terrains. detects 40 ejecta/s Thera detected grains back to the surface (upper figure). Hence, SUDA will relate Macula Ejecta move on Southwest the measured composition to geologHoicawl paistterns a co ampond fseaitituronaesl maon p thegenera Whatedt? isBy the co spambitianil rnges omalutinoyn osfuch a co mposm itional map? Without knowledge

ballistic trajectories k measurements a compositional map of othef the surfa duscet impacan ctbe s peedgenera, theted s. paFotira l resol ution is roughly given by the SC moon. 0 8 E6 each particle detection, a two dimensaltiiotudnael oprvoerba thebility a readis triof butiinterones t.is The res9 olution of SUDA maps is even Research Institute 109 ejecta/km2s derived for its origin on the surface. hiAsgher an, becaexampluse eSUD, theA midetermiddle fignesur ethe velocity componentThra ocef dust particles How many surface samples can be collected? The number of detectable Macula ejecta during a flyby or a low altitude osrbihotw cas na beM oesnte-timaCatedrlo b ysi mtheul adtienson ityof SUDaloAng meathes urinsementstrument d uriaxings Eurby omeapa suring its time-of-flight between the profile of Europa's well characterizedCli pperejecta 25 kmcloud flyb bays s6ed a ndo n9 oGaverlileo the dentraark loncebated gri dfea aturt thees Thraapercetur Me aaculnda acceleration grid at the target with an 55% measurements (Krüger et al., 1999; Karindvo Therav et a l.M, 2003)acula. . TheEach ejcoectalor edsize d ot aiccurandicatescy othef abo outri g1%in . o Thif asn imprejectaoves the resolution in the direction of the 75% distribution approximately follows a podetectedwer law bwyi thSUD a sAlo pera ndof o~2.mly4 laandunched S/ Cfr voelmo ciinsty ivdectoe (rred b)y aa ndfacto oruts ofi d2.e 420 km 95% Mass Spectrometer for ranges from ~100 nm up to the typical (syielzelo owf )the the impa featurctoer. The(abo utlo w100µer figm)ur. e shows the resulting probability map The total mass ejected in an impact onf oEurr theopa o farirg iexceedn of thes thedetected mass o paf therticl es from the dark 860featur kmes on Europa Probability for origin inside contour lines: MASPEX Planetary Exploration (red dots in middle plot) if identified by their unique composition. SUDA impacting meteoroid (~17,000 x) (Kempf et. al, 2012). As an example, Feb. 22, 2017 can unambiguously identify and characterize the composition of the Thrace 9 during each of the two Europa Clipper 25 km flybys shown in the middle molecules and ionsfrom theE9Jovian magnetosphere, and dust impacts. Theseprocesses arerespon- figure SUDA will collect 5000 samples Maorigciunalati angnd fr Toherma thi Mas caureala .terrains. Pre-Decisional Information — For Planning and Discussion Purposes Only sibleforTherathe formation of strong oxidants (O2,H2O2) inirradiated ices, accumulation of molecules Macula What is the spatial resolution of a compositional map? Without knowledge How is a compositional map generated? By combining many such and elementsm from Io(SO2, Na, K, Cl) together with chondritic and cometary materials containing

k measurements a compositional map oof fthe the sdurfaustce impa canct be speed genera, theted spa. Ftioar l resoluti on is roughly given by the SC both 0 inorganic and organic components (Carlson et al., 2009). Endogenic processes are responsi- 8 E6 each particle detection, a two dimensaltitudionae l oprvero bathebil ityar ead isotrif ibutinteroesn t. isThe ble resfor9 olutitheon deliof SUDveryA maof psnon-ice is even materials which are best manifested in disrupted surface features: derived for its origin on the surface. hi gAsher a, nbeca exausmple SUDe, theA dmietermiddle nesfigur thee velocity componentThra ocef d ust particles Macula shows a Monte-Carlo simulation of SUDalongA meathe siurnsementstrument d uriaxings bEury meaopa sridges,uring its chaotictime-of-fliterrains,ght betweenpits, theand domes. Galileo and telescopic IR data suggests the presence of Clipper 25 km flybys 6 and 9 over the entradark nceloba tedgrid f eaattur thees aThraperturce eM andcul aa ccelhydratederation sulfgrid ateat thespecies: target wMgith anand Na sulfates together with sulfuric55% acid hydrates (McCord et al., and Thera Macula. Each colored dota ccuraindicacytes o f theabo utori 1%gin. Thiof sa nimpr ejectaoves the resolution in the direction of the 75% 1998; Carlson et al., 2009; Shirley et al., 2010; Brown and 95Hand% , 2013). CO2 isreported in col- detected by SUDA randomly launchedS/C vfreloomci tyins viectode (rr edby) a afandcto oruts of i2.de ored non-ice materials420 km (Hansen and McCord, 2008). The detection of Na and K in the exosphere (yellow) the feature. The lower figure shows the resulting probability map for the origin of the detected particles from the dark features on Europa Probability for origin inside contour lines: (red dots in middle plot) if identified by their unique composition. SUDA can unambiguously identify and charmoleculesacterize the andcompionsosition fromof thethe ThrJoacevian magnetosphere, and dust impacts. Theseprocesses arerespon- Macula and Thera Macula terrains. siblefor theformation of strong oxidants (O ,H O ) inirradiated ices, accumulation of molecules 2 2 2 2 What is the spatial resolution of a coandmpoelementssitional map?from WithoIout(SO know2,ledNa,ge K, Cl) together with chondritic and cometary materials containing of the dust impact speed, the spatiabothl resolinorutiong ianics rougandhly giorveng anicby thecompone SC nts (Carlson et al., 2009). Endogenic processes are responsi- altitude over the area of interest. Theble rforesoltheutiondeli of SUDveryA ofmapsnon-ice is even materials which are best manifested in disrupted surface features: higher, because SUDA determines the velocity component of dust particles along the instrument axis by mearidges,suring itschaotic time-of-terrains,flight betwpits,een theand domes. Galileo and telescopic IR data suggests the presence of entrance grid at the aperture and ahccelydratederationsulf gridate at thespecies: target wMgith aandn Na sulfates together with sulfuric55% acid hydrates (McCord et al., accuracy of about 1%. This improves the resolution in the direction of the 75% 1998; Carlson et al., 2009; Shirley et al., 2010; Brown and Hand95% , 2013). CO2 is reported in col- S/C velocity vector by a factor of 2. ored non-ice materials (Hansen and McCord, 2008). The detection of Na and K in the exosphere molecules and ionsfrom theJovian magnetosphere, and dust impacts. Theseprocesses arerespon- siblefor theformation of strong oxidants (O ,H O ) inirradiated ices, accumulation of molecules 2 2 2 2 and elements from Io(SO2, Na, K, Cl) together with chondritic and cometary materials containing both inorganic and organic components (Carlson et al., 2009). Endogenic processes are responsi- ble for the delivery of non-ice materials which are best manifested in disrupted surface features: ridges, chaotic terrains, pits, and domes. Galileo and telescopic IR data suggests the presence of hydrated sulfate species: Mg and Na sulfates together with sulfuric acid hydrates (McCord et al., 1998; Carlson et al., 2009; Shirley et al., 2010; Brown and Hand, 2013). CO2 is reported in col- ored non-ice materials (Hansen and McCord, 2008). The detection of Na and K in the exosphere

2 Europa Instrument Highlights: SUDA & MASPEX Incoming Ejecta Particle SUrface Dust Analyzer (SUDA): Sascha Kempf, PI • SUDA is oriented directly into dust ram at closest approach, when particle number density is highest • Sun must be out of FOV while making dust measurements • Improving TRL on Ir-coated detector through prototype testing • Investigating innovative ways to lower instrument mass TOFMS MAss Spectrometer for Planetary EXploration Cryotrap Calibration Gas Detector (MASPEX): Hunter Waite, PI Radiator Gas Inlet Reflectron • VAT valve to reduce leak rate, facilitating cryosample analysis System • Performing lifetime testing on ion pump • Fabricating parts for detector • Contamination control is key – spacecraft cleanliness, FOV/KOZ incursions, thruster products

Feb. 22, 2017 10 Pre-Decisional Information — For Planning and Discussion Purposes Only Europa Instrument Overview: PIMS & ICEMAG

PIMS Plasma Instrument for Magnetic Sounding

Measures the plasma surrounding Europa to characterize its subsurface ocean, its ice shell, and plumes

PI: Joe Westlake Johns Hopkins Applied Infers location, thickness and Physics Laboratory conductivity of Europa’s ocean using electromagnetic sounding

PI: Carol Raymond Jet Propulsion Laboratory

Interior Characterization of Europa ICEMAG using Magnetometry Feb. 22, 2017 13 Pre-Decisional Information — For Planning and Discussion Purposes Only Europa Instrument Highlights: PIMS &ICEMAG Plasma Instrument for Magnetic Sounding (PIMS): Joe Westlake, PI • 2 sensors, each with 2 Faraday cups (90° FOV each) • Moved electronics to within cups, improving grounding • Modeling demonstrates mag cleanliness can be relaxed • Developing tools to assess potential science impacts of spacecraft charging, which can affect ion or electron measurements Interior Characterization of Europa using Magnetometry (ICEMAG): Carol Raymond, PI • Optimized location on the boom of the FG and SVH sensors • Working with spacecraft team on sensor attitude knowledge 2 x Scalar/Vector Helium (SVH): and magnetic cleanliness requirements alternating scalar and vector Feb. 22, 2017 2 x Flux Gate (FG): vector 12 Pre-Decisional Information — For Planning and Discussion Purposes Only Magnetometer Boom Deployment

Deployment Stowed Boom • Single hinge design sweep • Simple deployment • Fewer unknowns reduces magnetometer pointing uncertainty

Deployed Boom

Feb. 22, 2017 13 Pre-Decisional Information — For Planning and Discussion Purposes Only Spacecraft Deployment Sequence

Feb. 22, 2017 1416 Pre-Decisional Information — For Planning and Discussion Purposes Only Europa Flyby Animation

Pre-Decisional Information — For Planning and Discussion Purposes Only