RECENT ADVANCES IN THE SPECTROSCOPY OF PLANETARY AND
- Slides: 34
RECENT ADVANCES IN THE SPECTROSCOPY OF PLANETARY AND EXOPLANETARY ATMOSPHERES : WHAT IS OUT THERE ? Hitran 2010 Pierre Drossart LESIA, Observatoire de Paris 16 -18 June 2010 Hitran 2010 - Cambridge
Spectra of Giant Planets Day side (Reflected sunlight) 16 -18 June 2010 Hitran 2010 - Cambridge Thermal emission
XO-1 b Tinetti et al, 2010 G. Kuiper, Ap. J, 1947 16 -18 June 2010 Hitran 2010 - Cambridge
Line formation in Jupiter’s atmosphere (CH 4 4 band) Growth of line through vertical atmospheric integration 16 -18 June 2010 Hitran 2010 - Cambridge
Radiative transfer in Planetary atmospheres Spectra of Jupiter: Line formation in thermal spectrum Simulations at high/low resolution
NICMOS: transmission spectroscopy XO-1 b, terminator 16 -18 et. June Tinetti, al. , 2010 Ap. J, 2010 Hitran 2010 - Cambridge
Thermal structure retrieval o Machalek et al. , 2009 + Knutson et al. , 2007 1500 K 1000 K 16 -18 June 2010 Tinetti, et al. , Ap. J, 2010 Hitran 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 16 -18 June 2010 Hitran 2010 - Cambridge
CH 4 non LTE emission in exoplanets ? Swain et al, Nature, 2010 HD 189733 b 16 -18 June 2010 Hitran 2010 - Cambridge
Cassini Saturn spectroscopic observations in the infrared CIRS has two combined interferometers, operating in the farinfrared (10 -600 cm 1) and mid-infrared (600 -1400 cm-1). VIMS is an imaging visible and near infrared spectrometer (0. 3 -5 micron) 16 -18 June 2010 Hitran 2010 - Cambridge
Saturn 80°S at 100 and 300 km C 4 H 2 et CH 3 C 2 H CO 2 16 -18 June 2010 C 2 H 6 C 3 H 8 Hitran 2010 - Cambridge Flasar et al. , Sci. 2005 Radiance (W cm-2 sr-1 / cm-1) C 2 H 2
Saturn at 80°S 100 and 300 km CH 3 D 16 -18 June 2010 Hitran 2010 - Cambridge Flasar et al. , Sci. 2005 Radiance (W cm-2 sr-1 / cm-1) CH 4
First results from Herschel in the solar system First publications in Astronomy & Astrophysics – May 2010 16 -18 June 2010 Hitran 2010 - Cambridge
Instruments et observations __ __ ___ _____ __ • Observatory mode access from proposals – “Key Programs” (– x 100 h, “legacy”), priority – normal programs (AO 20 may 2010) 16 -18 June 2010 Hitran 2010 - Cambridge
Lellouch et al. , A&A 2010 Neptune spectrum from PACS 16 -18 June 2010 Hitran 2010 - Cambridge
Methane in the stratosphere of Neptune Lellouch et al. A & A 2010 Orton, Encrenaz et al. 2007
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 16 -18 June 2010 Hitran 2010 - Cambridge
Venus NIR day side spectrum Venus Express/VIRTIS spectra in the NIR (day side) Most of the absorptions : CO 2 ! 16 -18 June 2010 Hitran 2010 - Cambridge
Depression in the polar region N. Ignatiev 16 -18 June 2010 Grey are VMC images Hitran 2010 - Cambridge Ignatiev et al. , JGRE 2009
Telluric planets : Venus thermal emission in the dark side • Deep atmosphere of Venus Thermal emission originating from the 0 -45 km altitude range in spectral windows • Accurate knowledge of CO 2 opacity is crucial VIRTIS-M spectrum Challenge for H 2 O spectroscopy CO 2 : CO 2 up to 90 bars, 450 KH 2 O H 2 O at the surface CO 2 1. 0 m Database : HITEMP, 1. 27 m 1. 18 m 1. 74 m CDSD-750 1. 10 m 16 -18 June 2010 • CO 2 H 2 O 2. 3 m Hitran 2010 - Cambridge – Weak allowed bands – Pressure-induced bands – Far wing line shape
Venus nightside windows 2. 3 m CO 2 16 -18 June 2010 Hitran 2010 - Cambridge • 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
Deep atmosphere of Venus by VIRTIS/Venus Express CO 16 -18 June 2010 H 2 O Hitran 2010 - Cambridge HDO OCS SO 2 Marq et al. , JGRE, 2008 CO 2
Venus day side observations at 4. 3 micron : CO 2 non – LTE emissions Gilli, Lopez-Valverde et al. , JGRE 2009 16 -18 June 2010 Hitran 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 16 -18 June 2010 Hitran 2010 - Cambridge
Hitran 2010 - Cambridge 25/20 Gérard et al. , Icarus, 2009 1. 27 micron emission of Venus Mean vertical brightness = 0. 5 MR O 2 intensity : night side emission of Venus at 1. 27 micron
16 -18 June 2010 PNAS, 2008 Piccioni et al. , Hitran 2010 - Cambridge
Mars exploration in the XXIth century The War of the Worlds : the Revenge Mars Odyssey (2002) Mars Reconnaissance Orbiter (2006) Mars Express (2003) Coming soon… Mars Science Laboratory (2011) Mars Exploration rovers (2003) 16 -18 June 2010 Mars Trace Gas Orbiter (2016) Hitran 2010 - Cambridge
The infrared spectrum of Martian atmosphere Solar reflected CO 2 Thermal H 2 O CO 2 Hydrated silicates Reflected sunlight -> mineralogy Thermal emission -> T(z), winds CO CO 2 ISO-SWS Lellouch et al. , 2000
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
First IR detection of H 2 O 2 on Mars H 2 O 2 and CO 2 lines at 1241. 6 cm-1 H 2 O 2 Encrenaz et al. Icarus 2004 CO 2
Mars Trace Gas Orbiter NASA / ESA 2016 • Science objectives – Detection of trace molecules CH 4, C 2 H 2, C 2 H 6, NO 2, N 2 O, H 2 S, SO 2, H 2 O, O 3, 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 16 -18 June 2010 Hitran 2010 - Cambridge
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 • 1 ppb in 6 s 50 km 2 cartography • 50 ppt in solar occultation mode for detection
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 16 -18 June 2010 Hitran 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 16 -18 June 2010 Hitran 2010 - Cambridge
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