1. IGRINS Science Workshop 2010 1 High Spectral Resolution Mid- Infrared Spectroscopy as a Probe of the Physical State of Planetary Atmospheres August 26, 2010

2. IGRINS Science Workshop 2010 2 Advantages of High Spectral Resolution Increased sensitivity to unresolved spectral features (changes linearly with resolving power) Increases spectral separation of observed emission or absorption features allowing for unique identifications of a multitude of molecular features when molecular rotation-vibration bands overlap. Increases the amount of open spectral space to observation by reducing blending and increasing separation of telluric absorption features. The line shape of resolved spectral features can be use to retrieve information on velocity of the gas (compact H 2 regions, galaxies, etc), information on vertical variation of temperature or abundance of molecules in a planetary atmosphere, or the ability to separate distinct clouds of gas along a given line of sight.

3. IGRINS Science Workshop 2010 3 TEXES: Texas Echelon Cross Echelle Spectrograph Operates between 5 and 25  m A ground based prototype for EXES, an instrument to be flown on SOFIA

4. IGRINS Science Workshop 2010 4 36 inches long 0.3 inch groove spacing 0.03 inch groove height 0.3” Echelon Grating

5. IGRINS Science Workshop 2010 5 T.K. Greathouse J.I. Moses J.H. Lacy M.J. Richter NASA/JPL/Space Science Institute Probing Stratospheric Chemistry, Energetics, and Dynamics. A Detailed Study of Giant Planet Stratospheres

6. IGRINS Science Workshop 2010 6 Pressure (bar) Temperature (Kelvin) Troposphere Stratosphere Thermosphere Tropopause Mesosphere Mesopause Stratopause General Atmospheric Structure

7. IGRINS Science Workshop 2010 7 Process Dependencies Stratospheric Temperatures  Chemistry  Latitude?  Season?  Insolation  Latitude  Season  Solar Flux  Molecular Abundances  Latitude?  Season?  Dynamic Mixing?  Heating  Aerosols  Chemistry  Insolation  Advection?  Cooling  Molecular Abundances  Chemistry  Advection?

8. IGRINS Science Workshop 2010 8 Moses et al. 2000, Icarus. Question: What molecules exist in the stratosphere?

9. IGRINS Science Workshop 2010 9 Using Doppler Shifts for Unambiguous Detection of C 3 H 8 First Detection of Propane on Saturn -20  10  Latitude -80  10  Latitude

10. IGRINS Science Workshop 2010 10 ISO Schulz et al. 1999 First Detections of C 2 H 4 in Neptune

11. IGRINS Science Workshop 2010 11 A Second Detection AKARI data Fletcher et al. 2010

12. IGRINS Science Workshop 2010 12 The First Spectrally Resolved Detection of C 2 H 4 on Neptune

13. IGRINS Science Workshop 2010 13 Spectral Line Separation The Unambiguous Detection of C 3 H 8 Propane on Titan Roe et al. 2003 Propane Measure weak lines Measure features in crowded spectral regions

14. IGRINS Science Workshop 2010 14 Seasonal Studies

15. IGRINS Science Workshop 2010 15 Temperature Retrievals Using thermal emission spectra to retrieve temperatures requires knowledge of mixing ratio of observed molecule. Methane serves this purpose. Homogeneously mixed vertically and horizontally we can use this useful molecule as a thermometer.

16. Courtesy Glenn Orton southern winter southern spring southern summer

17. IGRINS Science Workshop 2010 17 CH 4 emission from –80° latitude

18. IGRINS Science Workshop 2010 18 Temperatures from 2002-2009

19. IGRINS Science Workshop 2010 19

22. IGRINS Science Workshop 2010 22

23. IGRINS Science Workshop 2010 23 C

24. IGRINS Science Workshop 2010 24 Ethane Spectrum with Missing Features

25. IGRINS Science Workshop 2010 25 A Few Project Ideas for IGRINS Auroral studies on Jupiter –IGRINS gives access the simultaneous acquisition of H 2 and H 3 + emission features. Cloud elevation studies on Saturn and Jupiter. Occultation observations –Very good probe of CH 4 vertical density distribution. Comet Observations Kuiper belt objects probably best left to GMTNIRS

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