Study of Planetary Atmospheres on the NASA IRTF Unique Capabili!Es

Study of Planetary Atmospheres on the NASA IRTF Unique Capabilies, Past Successes, and Future Direcons

Theodor Kosuk NASA Infrared Telescope Facility Future Direcons Workshop Biosphere 2, Tucson, 12-14 February 2018

Modern Astronomy Theorecal 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 resoluon and sensivity 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 resoluon different wavelengths Prototypes for future space flight instruments Complex instruments and capabilies 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 Priories for NASA Science Mission Directorate (SMD) Science Goals and Missions PLANETARY SCIENCE Ascertain the content, origin, and evoluon of the solar system and the potenal 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 evoluon 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. Idenfy and characterize objects in the solar system that pose threats to Earth, or offer resources for human exploraon. Atmospheres Science Goals •Atmospheric Evoluon Isotopic Composion and temporal and Spaal variability •Atmospheric Dynamics: Winds and circulaon Storms Longterm Thermal maps •Temporal Variability Diurnal Studies , e.g., Mars Global and Seasonal distribuon of temperature and atmospheric constuents •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-resoluon 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 resoluon grang spectrograph - Tommy Greathouse, SWRI BASS, medium resoluon 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 absorpon 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 constuents and isotopes in atmospheres – atmospheric

chemistry and evoluon, 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 Convecon 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 Maran 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 detecon of ethane and acetylene emission on Uranus. unexpected dip at the peak of the ethane emission. Yellow line: ethane emission with ethane ice absorpon. Blue: H2 connuum 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. Idenfy 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 Froners: Juno Titan – Dragonfly (APL), drone-like rotorcra to explore the prebioc 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 Invesgate Local Environment Dynamics. Composion, 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 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. dynamics and an aracve place to land (a) Doppler-shied CO2 absorpon feature large payloads. Breadth much greater than from troposphere, with mesospheric non-LTE depth creates a simple system to invesgate core emission, and a feature of 18OCO at lower mesoscale circulaon. High surface air pressure frequency. (b) Thermal profile and surface can benefit NASA goals for future crewed temperature from MGS-TES (blue) and exploraon and supports scienfic invesgaon modified profile and surface temperature (red) of trace species with enhanced path length. retrieved from HIPWAC spectrum, with cooler Yellow circles show examples for the surface, warmer boundary layer, and reduced spectroscopic field of view. surface pressure. (Livengood et al. 2018). Possible IRTF Enhancements

• Wide bandwidth IR (1-30 µm) Facility instruments Spectrometers and Imagers High spectral resoluon instruments: now only Visitor/PI instruments in mid-IR available. Facility instruments much more useful and can be used rounely and in remote observing. • Adapve Opcs: Makes Compeve with larger telescopes (with 6-m) • Larger (6-meter mirror) telescope: Beer spaal resoluon/imaging on small objects, e.g. Titan; compeve imager will be possible. • More flexibility to support Targets of Opportunity with mulple instruments e.g., SL-9 • Improve/Maintain Capability for Mul-Spectral Campaign Observaons • Maintain accessibility for New/PI instrumentaon and student “hands-on” experience Direct Measurements of Stratospheric Global Winds on Titan FOV Advantage with 6-Meter Telescope

Field of View on Titan with 3-m IRTF Prograde winds = 190 ±90 m/s (yellow circles) and 6 m IRTF (white circles) Kosuk et al. GRL 28, 2001 Possible IRTF Enhancements

• Wide bandwidth IR (1-30 µm) Facility instruments Spectrometers and Imagers High spectral resoluon instruments: now only Visitor/PI instruments in mid-IR available. Facility instruments much more useful and can be used rounely and in remote observing. • Adapve Opcs: Makes Compeve with larger telescopes (with 6-m) • Larger (6-meter mirror) telescope: Beer spaal resoluon/imaging on small objects, e.g. Titan; compeve imager will be possible. • More flexibility to support Targets of Opportunity with mulple instruments e.g., SL-9 • Improve/Maintain Capability for Mul-Spectral Campaign Observaons • Maintain accessibility for New/PI instrumentaon and student “hands-on” experience Hawaii February 6, 2008

January and February 2007 were the same