Recent advances in the spectroscopy of planetary and exoplanetary atmospheres what is out there
Download
1 / 34

Hitran 2010 Pierre Drossart LESIA, Observatoire de Paris - PowerPoint PPT Presentation


  • 110 Views
  • Uploaded on

RECENT ADVANCES IN THE SPECTROSCOPY OF PLANETARY AND EXOPLANETARY ATMOSPHERES : WHAT IS OUT THERE ?. Hitran 2010 Pierre Drossart LESIA, Observatoire de Paris. Spectra of Giant Planets. Day side (Reflected sunlight). Thermal emission. XO-1b Tinetti et al, 2010. G. Kuiper, ApJ, 1947.

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about ' Hitran 2010 Pierre Drossart LESIA, Observatoire de Paris' - lynley


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
Recent advances in the spectroscopy of planetary and exoplanetary atmospheres what is out there

RECENT ADVANCES IN THE SPECTROSCOPY OF PLANETARY AND EXOPLANETARY ATMOSPHERES : WHAT IS OUT THERE ?

Hitran 2010

Pierre Drossart

LESIA, Observatoire de Paris


Spectra of giant planets
Spectra of Giant Planets

Day side (Reflected sunlight)

Thermal emission

Hitran 2010 - Cambridge


XO-1b Tinetti et al, 2010

G. Kuiper, ApJ, 1947

Hitran 2010 - Cambridge


Line formation in Jupiter’s atmosphere (CH44 band)

Growth of line through vertical atmospheric integration

Hitran 2010 - Cambridge


Spectra of jupiter line formation in the thermal spectrum simulations at high low resolution
Spectra of Jupiter: Line formation in the thermal spectrumSimulations at high/low resolution

Radiative transfer in

Planetary atmospheres


Nicmos transmission spectroscopy
NICMOS: transmission spectroscopy

XO-1b, terminator

Hitran 2010 - Cambridge

Tinetti, et al., ApJ, 2010


Thermal structure retrieval
Thermal structure retrieval

o Machalek et al., 2009

+ Knutson et al., 2007

1500 K

1000 K

Hitran 2010 - Cambridge

Tinetti, et al., ApJ, 2010


Non lte emissions of ch 4 in giant planets
Non-LTE emissions of CH4 in giant planets

ISO observation of CH4 non-LTE emission on Jupiter

Drossart et al, ESA-SP 427, 1999

Hitran 2010 - Cambridge


Ch 4 non lte emission in exoplanets
CH4 non LTE emission in exoplanets ?

Swain et al, Nature, 2010

HD189733b

Hitran 2010 - Cambridge


Cassini
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)

Hitran 2010 - Cambridge


Saturn 80°S at 100 and 300 km

C2H2

Flasar et al., Sci. 2005

C4H2 et CH3C2H

C2H6

Radiance (W cm-2 sr-1 / cm-1)

C3H8

CO2

Hitran 2010 - Cambridge


Saturn at 80°S 100 and 300 km

CH4

CH3D

Flasar et al., Sci. 2005

Radiance (W cm-2 sr-1 / cm-1)

Hitran 2010 - Cambridge


First results from herschel in the solar system

First results from Herschel in the solar system

First publications in Astronomy & Astrophysics – May 2010


Instruments et observations
Instruments et observations

__

  • Observatory mode  access from proposals

    • “Key Programs” (– x 100 h, “legacy”), priority

    • normal programs (AO 20 may 2010)

___

__

___

_____

__

Hitran 2010 - Cambridge


Neptune spectrum from pacs
Neptune spectrum from PACS

Lellouch et al., A&A 2010

Hitran 2010 - Cambridge


Methane in the stratosphere of neptune
Methane in the stratosphere of Neptune

Lellouch et al. A & A 2010

Orton, Encrenaz et al. 2007


Venus atmosphere
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

Hitran 2010 - Cambridge


Venus nir day side spectrum
Venus NIR day side spectrum

Venus Express/VIRTIS spectra in the NIR (day side)

Most of the absorptions : CO2 !

Hitran 2010 - Cambridge


Depression in the polar region
Depression in the polar region

Grey are VMC images

N. Ignatiev

Hitran 2010 - Cambridge

Ignatiev et al., JGRE 2009


Telluric planets venus thermal emission in the dark side
Telluric planets : Venus thermal emission in the dark side

  • Thermal emission originating from the 0-45 km altitude range in spectral windows

  • Accurate knowledge of CO2 opacity is crucial

    • Weak allowed bands

    • Pressure-induced bands

    • Far wing line shape

  • Deep atmosphere of Venus

    Challenge for spectroscopy : CO2 up to 90 bars, 450 K at the surface

    Database : HITEMP, CDSD-750

VIRTIS-Mspectrum

H2O

CO2

H2O

H2O

CO2

CO2

CO2

H2O

1.0 m

1.27 m

1.18 m

1.74 m

2.3 m

1.10 m

Hitran 2010 - Cambridge


Venus nightside windows2.3 m

  • CFHT/FTS observations (Res = 0.15 cm-1) [Taylor et al. 1997]

  • Altitude range: 26-45 km

  • Absorbers: CO2, H2O, HDO, CO, OCS, SO2, HF

CO2

Hitran 2010 - Cambridge


Deep atmosphere of venus by virtis venus express
Deep atmosphere of Venus by VIRTIS/Venus Express

CO2

CO H2O HDO OCS SO2

Marq et al., JGRE, 2008

Hitran 2010 - Cambridge


Venus day side observations at 4.3 micron :

CO2non – LTE emissions

Gilli, Lopez-Valverde et al., JGRE 2009

Hitran 2010 - Cambridge


Gravity waves observed in co 2 non lte emission of venus
Gravity waves observed in CO2 non-LTE emission of Venus

Day side up/night side down

Center on South pole

Polar vortex in red

Garcia et al., JGRE, 2009

Hitran 2010 - Cambridge


O 2 intensity night side emission of venus at 1 27 micron
O2 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

11/09/2014

Hitran 2010 - Cambridge

25/20


Piccioni et al., PNAS, 2008

Hitran 2010 - Cambridge


Mars exploration in the xxi th century
Mars exploration in the XXIth century

The War of the Worlds : the Revenge

Mars Reconnaissance Orbiter (2006)

Coming soon…

Mars Science Laboratory (2011)

Mars Trace Gas Orbiter (2016)

Mars Odyssey

(2002)

Mars Express (2003)

Mars Exploration rovers (2003)

Hitran 2010 - Cambridge


The infrared spectrum of Martian atmosphere

Solar reflected Thermal

CO2 H2O

CO CO2

Hydrated

silicates

CO2 CO2

Reflected sunlight -> mineralogy

Thermal emission -> T(z), winds

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

H2O2, 10-7

synthetic

TEXES data


First IR detection of H2O2 on Mars

H2O2 and CO2 lines at 1241.6 cm-1

H2O2

H2O2

CO2

Encrenaz et al. Icarus 2004


Mars trace gas orbiter nasa esa 2016
Mars Trace Gas OrbiterNASA / ESA 2016

  • Science objectives

    • Detection of trace molecules CH4, C2H2, C2H6, 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

Hitran 2010 - Cambridge


Some trace gases to search for with tgo nadir and limb observations
Some trace gases to search for with TGOnadir and limb observations

  • The spectral domain has been optimized for several simultaneous gas detection

  • Sensitivity to methane

    • 1ppb in 6 s  50 km2 cartography

    • 50 ppt in solar occultation mode for detection


Conclusions about exo planetary atmospheres spectroscopy
Conclusions about (exo)planetary atmospheres spectroscopy

What is out there ?

At first order : CO2 , CH4 , H2O , 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 : H2O2, OH, H2CO

    Giant planets : NH3, PH3, H2S

Hitran 2010 - Cambridge


Acknowledgements to
Acknowledgements to

  • Bruno Bézard

  • Régis Courtin

  • Emmanuel Lellouch

  • Dominique Bockelee

  • Giovanna Tinetti

  • Athena Coustenis

  • Thérèse Encrenaz

  • Giuseppe Piccioni

  • Miguel Lopez-Valverde

  • Raphaël Garcia

Hitran 2010 - Cambridge


ad