Astrophysics The Earth as an extrasolar transiting planet II. HARPS and UVES detection of water vapour, biogenic O 2 , and O 3Reportar como inadecuado

Astrophysics The Earth as an extrasolar transiting planet II. HARPS and UVES detection of water vapour, biogenic O 2 , and O 3 - Descarga este documento en PDF. Documentación en PDF para descargar gratis. Disponible también para leer online.

1 OSU PYTHEAS - Institut Pythéas 2 ObsGE - Observatoire Astronomique de l-Université de Genève 3 IAP - Institut d-Astrophysique de Paris 4 CfA - Harvard-Smithsonian Center for Astrophysics 5 Unidad de Astronomia 6 University of Chile Santiago 7 NIWA - National Institute of Water and Atmospheric Research Wellington 8 Deutsches Zentrum für Luft und Raumfahrt 9 IMCCE - Institut de Mécanique Céleste et de Calcul des Ephémérides 10 LAM - Laboratoire d-Astrophysique de Marseille 11 CFHT Corporation 12 astrononomy department, universidad de chile

Abstract : Context. The atmospheric composition of transiting exoplanets can be characterized during transit by spectroscopy. Detections of several chemical species have previously been reported in the atmosphere of gaseous giant exoplanets. For the transit of an Earth twin, models predict that biogenic oxygen O 2 and ozone O 3 atmospheric gases should be detectable, as well as water vapour H 2 O, a molecule linked to habitability as we know it on Earth. Aims. The aim is to measure the Earth radius versus wavelength λ – or the atmosphere thickness hλ – at the highest spectral resolution available to fully characterize the signature of Earth seen as a transiting exoplanet. Methods. We present observations of the Moon eclipse of December 21, 2010. Seen from the Moon, the Earth eclipses the Sun and opens access to the Earth atmosphere transmission spectrum. We used two different ESO spectrographs HARPS and UVES to take penumbra and umbra high-resolution spectra from ≈3100 to 10 400 Å. A change of the quantity of water vapour above the telescope compromised the quality of the UVES data. We corrected for this effect in the data processing. We analyzed the data by three different methods. The first method is based on the analysis of pairs of penumbra spectra. The second makes use of a single penumbra spectrum, and the third of all penumbra and umbra spectra. Results. Profiles hλ are obtained with the three methods for both instruments. The first method gives the best result, in agreement with a model. The second method seems to be more sensitive to the Doppler shift of solar spectral lines with respect to the telluric lines. The third method makes use of umbra spectra, which bias the result by increasing the overall negative slope of hλ. It can be corrected for this a posteriori from results with the first method. The three methods clearly show the spectral signature of the Rayleigh scattering in the Earth atmosphere and the bands of H 2 O, O 2 , and O 3. Sodium is detected. Assuming no atmospheric perturbations, we show that the E-ELT is theoretically able to detect the O 2 A-band in 8 h of integration for an Earth twin at 10 pc. Conclusions. Biogenic O 2 , O 3 , and water vapour are detected in Earth observed as a transiting planet, and, in principle, would be within reach of the E-ELT for an Earth twin at 10 pc. Key words. Earth – Moon – atmospheric effects – planets and satellites: atmospheres – planets and satellites: terrestrial planets – astrobiology

Autor: L Arnold - D Ehrenreich - A Vidal-Madjar - X Dumusque - C Nitschelm - Richard Querel - P Hedelt - J Berthier - C Lovis - C Moutou



Documentos relacionados