1. RECENT ADVANCES IN THE SPECTROSCOPY OF PLANETARY AND EXOPLANETARY ATMOSPHERES : WHAT IS OUT THERE ? Hitran 2010 Pierre Drossart LESIA, Observatoire de Paris

2. 16-18 June 2010Hitran 2010 - Cambridge Spectra of Giant Planets Day side (Reflected sunlight) Thermal emission

3. 16-18 June 2010Hitran 2010 - Cambridge XO-1b Tinetti et al, 2010 G. Kuiper, ApJ, 1947

4. 16-18 June 2010Hitran 2010 - Cambridge Line formation in Jupiter’s atmosphere (CH 4 4 band) Growth of line through vertical atmospheric integration

5. Radiative transfer in Planetary atmospheres Spectra of Jupiter: Line formation in the thermal spectrum Simulations at high/low resolution

6. 16-18 June 2010Hitran 2010 - Cambridge NICMOS: transmission spectroscopy Tinetti, et al., ApJ, 2010 XO-1b, terminator

7. 16-18 June 2010Hitran 2010 - Cambridge Thermal structure retrieval o Machalek et al., 2009 + Knutson et al., 2007 1500 K 1000 K Tinetti, et al., ApJ, 2010

8. 16-18 June 2010Hitran 2010 - Cambridge Non-LTE emissions of CH 4 in giant planets Drossart et al, ESA-SP 427, 1999 ISO observation of CH 4 non-LTE emission on Jupiter

9. 16-18 June 2010Hitran 2010 - Cambridge CH 4 non LTE emission in exoplanets ? Swain et al, Nature, 2010 HD189733b

10. 16-18 June 2010Hitran 2010 - Cambridge Cassini Saturn spectroscopic observations in the infrared CIRS has two combined interferometers, operating in the far- infrared (10-600 cm- 1) and mid-infrared (600-1400 cm-1). VIMS is an imaging visible and near infrared spectrometer (0.3-5 micron)

11. 16-18 June 2010Hitran 2010 - Cambridge Saturn 80°S at 100 and 300 km C2H2C2H2 C2H6C2H6 C 4 H 2 et CH 3 C 2 H C3H8C3H8 Radiance (W cm -2 sr -1 / cm -1 ) CO 2 Flasar et al., Sci. 2005

12. 16-18 June 2010Hitran 2010 - Cambridge Saturn at 80°S 100 and 300 km CH 4 CH 3 D Radiance (W cm -2 sr -1 / cm -1 ) Flasar et al., Sci. 2005

13. First results from Herschel in the solar system First publications in Astronomy & Astrophysics – May 2010

14. 16-18 June 2010Hitran 2010 - Cambridge Observatory mode  access from proposals –“Key Programs” (– x 100 h, “legacy”), priority –normal programs (AO 20 may 2010) Instruments et observations __ ___ _____

15. 16-18 June 2010Hitran 2010 - Cambridge Neptune spectrum from PACS Lellouch et al., A&A 2010

16. Methane in the stratosphere of Neptune Orton, Encrenaz et al. 2007 Lellouch et al. A & A 2010

17. 16-18 June 2010Hitran 2010 - Cambridge Venus atmosphere Venus Express observations A new start in Venus atmosphere observations after a long gap since Venera 15 and Vega russian missions Next mission Akatsuki (Jaxa) Launched on May 20

18. 16-18 June 2010Hitran 2010 - Cambridge Venus NIR day side spectrum Venus Express/VIRTIS spectra in the NIR (day side) Most of the absorptions : CO 2 !

19. 16-18 June 2010Hitran 2010 - Cambridge N. Ignatiev Grey are VMC images Depression in the polar region Ignatiev et al., JGRE 2009

20. 16-18 June 2010Hitran 2010 - Cambridge Telluric planets : Venus thermal emission in the dark side Deep atmosphere of Venus Challenge for spectroscopy : CO 2 up to 90 bars, 450 K at the surface Database : HITEMP, CDSD-750 CO 2 H2OH2O H2OH2O 1.74  m 2.3  m 1.27  m 1.18  m 1.10  m 1.0  m VIRTIS-M spectrum H2OH2O H2OH2O Thermal emission originating from the 0-45 km altitude range in spectral windows Accurate knowledge of CO 2 opacity is crucial –Weak allowed bands –Pressure-induced bands –Far wing line shape

21. 16-18 June 2010Hitran 2010 - Cambridge Venus nightside windows 2.3  m CFHT/FTS observations (Res = 0.15 cm -1 ) [Taylor et al. 1997] Altitude range: 26-45 km Absorbers: CO 2, H 2 O, HDO, CO, OCS, SO 2, HF CO 2

22. 16-18 June 2010Hitran 2010 - Cambridge Deep atmosphere of Venus by VIRTIS/Venus Express CO 2 CO H 2 O HDO OCS SO 2 Marq et al., JGRE, 2008

23. 16-18 June 2010Hitran 2010 - Cambridge Venus day side observations at 4.3 micron : CO 2 non – LTE emissions Gilli, Lopez-Valverde et al., JGRE 2009

24. 16-18 June 2010Hitran 2010 - Cambridge Gravity waves observed in CO 2 non- LTE emission of Venus Day side up/night side down Center on South pole Polar vortex in red Garcia et al., JGRE, 2009

25. 16-18 June 2010Hitran 2010 - Cambridge O 2 intensity : night side emission of Venus at 1.27 micron Mean vertical brightness = 0.5 MR 1.27 micron emission of Venus Gérard et al., Icarus, 2009 24/06/201525/20

26. 16-18 June 2010Hitran 2010 - Cambridge Piccioni et al., PNAS, 2008

27. 16-18 June 2010Hitran 2010 - Cambridge Mars exploration in the XXI th century Mars Odyssey (2002) Mars Express (2003) Mars Exploration rovers (2003) Mars Reconnaissance Orbiter (2006) Coming soon… Mars Science Laboratory (2011) Mars Trace Gas Orbiter (2016) The War of the Worlds : the Revenge

28. The infrared spectrum of Martian atmosphere Solar reflectedThermal CO 2 H 2 O CO 2 COCO 2 ISO-SWS Lellouch et al., 2000 Hydrated silicates Reflected sunlight -> mineralogy Thermal emission -> T(z), winds

29. The 1237-1243 cm -1 spectrum of Mars (TEXES, IRTF) All lines identified down to depths of 0.3% S/N > 1000 in the continuum H 2 O 2, 10 -7 synthetic TEXES data

30. First IR detection of H 2 O 2 on Mars H 2 O 2 and CO 2 lines at 1241.6 cm -1 H2O2H2O2 H2O2H2O2 CO 2 Encrenaz et al. Icarus 2004

31. 16-18 June 2010Hitran 2010 - Cambridge Mars Trace Gas Orbiter NASA / ESA 2016 Science objectives –Detection of trace molecules CH 4, C 2 H 2, C 2 H 6, NO2, N2O, H2S, SO2, H2O, O3, isotopologues Determine the type of activiy : geological, or biological from the molecular ratio Characterize spatial and temporal variations Find the correlations between trace species to constrain the chemistry –Localize the sources Trace the origin of gases Determine uncertainty of a landing mission for EXOMARS

32. Some trace gases to search for with TGO nadir and limb observations The spectral domain has been optimized for several simultaneous gas detection Sensitivity to methane 1ppb in 6 s  50 km 2 cartography 50 ppt in solar occultation mode for detection

33. 16-18 June 2010Hitran 2010 - Cambridge Conclusions about (exo)planetary atmospheres spectroscopy What is out there ? At first order : CO 2, CH 4, H 2 O, CO … but we still do not fully understand the spectroscopy of these molecules! Isotopes, line shapes, CIA, line mixing, relaxation coefficients, etc. Trace constituents Telluric planets : H 2 O 2, OH, H 2 CO Giant planets : NH 3, PH 3, H 2 S

34. 16-18 June 2010Hitran 2010 - Cambridge Acknowledgements to Bruno Bézard Régis Courtin Emmanuel Lellouch Dominique Bockelee Giovanna Tinetti Athena Coustenis Thérèse Encrenaz Giuseppe Piccioni Miguel Lopez-Valverde Raphaël Garcia