Study of Planetary Atmospheres on the NASA IRTF Unique Capabili*es, Past Successes, and Future Direc*ons Theodor Kosuk NASA Infrared Telescope Facility Future Direc*ons Workshop Biosphere 2, Tucson, 12-14 February 2018 Modern Astronomy Theore*cal Studies Laboratory Studies Goals for observaons Data for planning and interpretation of Tools for remote and space flight measurements interpretaon of measurements Fundamental understanding Space Flight Missions Local and in situ studies Higher spaal resolu*on and sensi*vity Local Diurnal coverage No Earth atmospheric effects Ground Based Observatory Studies Data to plan missions Instrument Development Complementary studies: long term, simultaneous New techniques measurements, unique events Higher spectral, spaal resolu*on different wavelengths Prototypes for future space flight instruments Complex instruments and capabili*es Test of future space flight instruments Do fundamental research Synergy of Ground Based and Space-Based Measurements Voyager Cassini MGS - Thermal Huygens Emission Spectrometer: H2O, Temperature Mars Global SpitzerSpitzer Space Space Telescope Telescope Surveyor Voyager 1,2 - Cassini Huygens - InfraRed Spectrometer Composite Infrared Interferometer, IRIS: Spectrometer, CIRS: Composition, Composition, Temperature, WInds Temperature, Winds Mars Express Spitzer Space Mars Express - Telescope - SPICAM: IRAC, MIPS UV measurements of 10 m Keck Detect and measure O Exoplanets 3 8.2 m Subaru 3 m IRTF Decadal Survey Priori*es for NASA Science Mission Directorate (SMD) Science Goals and Missions PLANETARY SCIENCE Ascertain the content, origin, and evolu*on of the solar system and the poten*al for life elsewhere. a. Building New Worlds—advance the understanding of solar system beginnings 1. Explore and observe the objects in the solar system to understand how they formed and evolve. 2. Advance the understanding of how the chemical and physical processes in our solar system operate, interact and evolve. b. Planetary Habitats—search for the requirements for life 3. Explore and find locaons where life could have existed or could exist today. 4. Improve our understanding of the origin and evolu*on of life on Earth to guide our search for life elsewhere. c. Workings of Solar Systems—reveal planetary processes through *me 1. Explore and observe the objects in the solar system to understand how they formed and evolve. 2. Advance the understanding of how the chemical and physical processes in our solar system operate, interact and evolve. 5. Iden*fy and characterize objects in the solar system that pose threats to Earth, or offer resources for human exploraon. Atmospheres Science Goals •Atmospheric Evolu1on Isotopic Composi*on and temporal and Spaal variability •Atmospheric Dynamics: Winds and circulaon Storms Longterm Thermal maps •Temporal Variability Diurnal Studies , e.g., Mars Global and Seasonal distribu*on of temperature and atmospheric cons*tuents •Discovery of new species or phenomena that can be studies by orbiters/flybys : •Study environments that could help search for life •Determine environments conducive for Human landing and subsistence (Mars) IRTF Instruments IRTF Facility Instruments CSHELL – 1-5.5 µm Spectrometer/RETIRED SpeX, 0.7-5.3 µm medium-resolu*on spectrograph iSHELL, 1.1-5.3 µm cross-dispersed spectrograph and imager. MORIS, Andor 512 x 512 pixel CCD camera mounted at the side-facing window of SpeX Collaborave PI/Facility Instrument (w/Boston University) MIRSI, 8-26 µm camera and grism spectrometer with 320x240 Si:As array with 0.27 arcsec/pixel Visitor Instruments TEXES, 8-26 µm high resolu*on grang spectrograph - Tommy Greathouse, SWRI BASS, medium resolu*on 3-14 µm spectrometer 116 element, non-scanning prism system - Ray Russell, Aerospace Corp HIPWAC, 7-13 µm heterodyne spectrograph R>1,000,000 - Tim Livengood, NASA/GSFC Examples of Objects of Opportunity and Unique Discoveries • Infrared Aurorae and Polar Warming on jupiter and Saturn – + Hydrocarbon, H3 . Mul*-seasonal Variability • Neptune ethane ice absorp*on and C2H6 on Uranus for the first *me • Natural CO2 Lasers/NLTE on Mars and Venus: Probes of Mesosphere/ Thermosphere, Circulaon and Temperatures • Mesospheric/Thermospheric Winds on Venus and Mars • Mesospheric/ Thermosperic Temperatures on Mars and Venus • Minor cons*tuents and isotopes in atmospheres – atmospheric chemistry and evolu*on, e.g., C2H4 on jupiter/Saturn; C2H6 on Neptune; Ozone and Isotopes of CO2 on Mars. H2O2 on Mars Methane on Mars Campaigns: jupiter SL9 Impacts , H2O, NH3, Impact site dynamics jupiter impacts Saturn/jupiter/ Neptune Storms 1. Explore and observe the objects in the solar system to understand how they formed and evolve. 2. Advance the understanding of how the chemical and physical processes in our solar system operate, interact and evolve. Depth of a Strong Jovian Jet From a Planetary-Scale Disturbance Sanchez-Lavega (Universidad del Pais Vasco, Spain), G.S. Orton (JPL), et al. Nature 451, 2008 5 April 2007 – Two high plumes Trailing “wake” from each is dark, bright at 5 μm Remove upper-level clouds RGB, Zac Pujic 15 NASA IRTF SpeX 10 1.58 μm 5 15 10 2.17 μm 5 15 10 4.78 μm Centric Latude °N 5 220 210 200 190 180 170 160 150 140 130 Longitude°W (System III) Mid-IR Spectral Images of jupiter with MIRSI Moist Convec*on and the 2010-2011 Revival of jupiter’s South Equatorial Belt Fletcher et al. Icarus 2017 DIURNAL VARIABILITY OF 16O12C18O ON MARS Comparison to Mission Results IRTF/HIPWAC 0.1 Best fit MGS-TES (initial) (a)Mars spectrum measured with HIPWAC. (b) a 952.8808 cm–1 b Thermal profile and surface temperature from 70 –1 /sr) 952.8629 cm Non-LTE -1 MGS-TES (blue) and modified profile and /cm surface temperature (red) retrieved from 2 60 HIPWAC spectrum, with cooler surface, 1.0 warmer boundary layer, and reduced surface 18 pressure. (Livengood et al. 2018). 50 OCO 271K CO 237K 240K 2 7.6 mbar 5.6 mbar Radiance Radiance (erg/s/cm 40 200 400 600 800 1000 1200 1400 150 186 223 259 295 Δν (MHz from LO) T (K) 290K Curiosit Phoenix 0.053 cm-1 Spectroscopy y Viking Mars isotopic abundance retrieved from HIPWAC spectra. Compared to results from Genesis (solar missions. Note apparent temperature wind) dependence (Livengood et al. 2018). Strong Water Isotopic Anomalies in the Mar*an Atmosphere: Probing Current and Ancient Reservoirs Villanueva et al. Science 348, 2015 CSHELL/IRTF, CRIRES/VLT, NIRSPEC/Keck Isotopic enrichment as evidence for global loss of water on Mars. Jupiter’s Mid-Infrared Aurora 1979 – 2016 NASA IRTF IRHS/HIPWAC – Kostiuk et al. 2016 Example of Long Term (Seasonal/Solar Cycle) Variability On#Hot#Spot# Off#Hot#Spot# Observa(ons+of+Jupiter’s+Mid5Infrared+Aurora+197952010+60°N,##178°# 60°N,##104°# Example+of+Long+Term+Variability+ C2H6 Emission On 30+ )+ V1,+ Cassini+ and Off Polar Hot Flyby+ ppm V2+ + Spot 2004 6 Flyby+ H 2 20+ Jupiter’s+Mid+–IR+Aurora+and+ISES+ IRHS%Observa-ons%of%Jupiter’s%Mid9Infrared%Aurora%200092010%Solar+Cycle+Sunspot+Number+ ISES%Solar%Cycle%Sunspot%Number%Progression% +Intensity+(C Observed%data%through%Aug.%2014%Progression+ 10.7+cm+Radio+Flux+ )+ Cassini%Flyby% 10+ Observed+data+Jan.+2000+through+ )% Cassini+ Juno%at%Jupiter%Juno+at+ 15% Auroral ppm + ppm Flyby+ 6 Aug.+2014+Jupiter+ % 6 1980+ 2005+ H H 2 Cycle%23% Cycle%24% 2 Jupiter’s+Mid+–IR+Aurora+and+Solar+ 10% Radio+Observa(ons+197852007+ 5% %Intensity%(per%C Sunspot%Number% +Intensity+(C Both+Ground5based+and+Space5 Auroral 0% based+Data+on+Jupiter’s+Mid+–IR+ Auroral Aurora+is+Available+197952014+ Jan.+2000+ 2005+ +2010+ 2015+ Mid-Infrared Ethane Emission on Neptune and Uranus Heidi B. Hammel, M. Sitko (Space Science Inst.) D. Lynch, R. Russell (The Aerospace Corp.), L.S. Bernstein (Spectral Science), T. Hewagama (Goddard) Obtained new spectra using the BASS spectrometer on the IRTF. Spectra obtained from 3-13 microns with a single exposure. One can see significant changes in the ethane emission at 12.2 microns as well as changes in the methane emission at 7.8 microns. Note the BASS detec*on of ethane and acetylene emission on Uranus. unexpected dip at the peak of the ethane emission. Yellow line: ethane emission with ethane ice absorp*on. Blue: H2 con*nuum emission. Red: Acetylene emission. Grey: model spectrum. 1. Explore and observe the objects in the solar system to understand how they formed and evolve. 2. Advance the understanding of how the chemical and physical processes in our solar system operate, interact and evolve 3. Explore and find locaons where life could have existed or could exist today. 5. Iden*fy and characterize objects in the solar system that pose threats to Earth, or offer resources for human exploraon. Strong Release of Methane on Mars in Northern Summer 2003 Mumma et al. Science 323, 2009 CSHELL with TEXES Future Missions? Discovery: Venus, Mars New Fron1ers: Juno Titan – Dragonfly (APL), drone-like rotorcra to explore the prebio*c chemistry and habitability of dozens of sites Enceladus – Enceladus Life Signatures and Habitability (ELSAH), NASA/Ames/GSFC Venus – Venus In situ Composion Invesgaons (VICI), NASA/GSFC Saturn probe Mars Flagship: Mars Rover 2020 and Europa Clipper ICE Giants: Uranus/Neptune /probe Small Missions: SIMPLEx (Small Innovave Missions for Planetary Exploraon) e.g., Venus: CUVE, SAEVe; Mars: Aeolus, MISEN, MAT; Outer Planets: SNAP ESO, JAXA……Venus, Mars, jupiter: Icy Moon Explorer (jUICE) Comparison of HIPWAC ( solid) and Mars Mars CO2 and Ozone IRTF/HIPWAC 2008 Express SPICAM (tracks) measurements of Ozone on Mars 2006-2008 and variaon from 1993 IRHS (hatched) results Fast et al. Icarus 203, 2009 Inves*gate Local Environment Dynamics. Composi*on, and Temperature of Possible Mars Lander Site? 0.1 Best fit MGS-TES (initial) a 952.8808 cm–1 b 70 –1 /sr) 952.8629 cm Non-LTE -1 /cm 2 60 1.0 18 50 OCO 271K CO 237K 240K 2 7.6 mbar 5.6 mbar Radiance (erg/s/cm 40 200 400 600 800 1000 1200 1400 150 186 223 259 295 Δν (MHz from LO) T (K) 290K Hellas Basin is a laboratory for atmospheric Mars spectrum measured with HIPWAC.