Show simple item record

Files in this item

Thumbnail

Item metadata

dc.contributor.authorMisra, A.
dc.contributor.authorMeadows, V.
dc.contributor.authorClaire, M.
dc.contributor.authorCrisp, D.
dc.date.accessioned2014-05-16T12:01:02Z
dc.date.available2014-05-16T12:01:02Z
dc.date.issued2014-02-19
dc.identifier.citationMisra , A , Meadows , V , Claire , M & Crisp , D 2014 , ' Using dimers to measure biosignatures and atmospheric pressure for terrestrial exoplanets ' , Astrobiology , vol. 14 , no. 2 , pp. 67-86 . https://doi.org/10.1089/ast.2013.0990en
dc.identifier.issn1531-1074
dc.identifier.otherPURE: 118979352
dc.identifier.otherPURE UUID: 261470a7-5963-4520-8d5b-8b3219c33b30
dc.identifier.otherScopus: 84894531197
dc.identifier.otherORCID: /0000-0001-9518-089X/work/34103245
dc.identifier.otherWOS: 000331460600001
dc.identifier.urihttp://hdl.handle.net/10023/4816
dc.description.abstractWe present a new method to probe atmospheric pressure on Earth-like planets using (O-O) dimers in the near-infrared. We also show that dimer features could be the most readily detectable biosignatures for Earth-like atmospheres and may even be detectable in transit transmission with the James Webb Space Telescope (JWST). The absorption by dimers changes more rapidly with pressure and density than that of monomers and can therefore provide additional information about atmospheric pressures. By comparing the absorption strengths of rotational and vibrational features to the absorption strengths of dimer features, we show that in some cases it may be possible to estimate the pressure at the reflecting surface of a planet. This method is demonstrated by using the O A band and the 1.06 μm dimer feature, either in transmission or reflected spectra. It works best for planets around M dwarfs with atmospheric pressures between 0.1 and 10 bar and for O volume mixing ratios above 50% of Earth's present-day level. Furthermore, unlike observations of Rayleigh scattering, this method can be used at wavelengths longer than 0.6 μm and is therefore potentially applicable, although challenging, to near-term planet characterization missions such as JWST. We also performed detectability studies for JWST transit transmission spectroscopy and found that the 1.06 and 1.27 μm dimer features could be detectable (SNR>3) for an Earth analogue orbiting an M5V star at a distance of 5 pc. The detection of these features could provide a constraint on the atmospheric pressure of an exoplanet and serve as biosignatures for oxygenic photosynthesis. We calculated the required signal-to-noise ratios to detect and characterize O monomer and dimer features in direct imaging-reflected spectra and found that signal-to-noise ratios greater than 10 at a spectral resolving power of R=100 would be required.
dc.format.extent20
dc.language.isoeng
dc.relation.ispartofAstrobiologyen
dc.rightsThis is a copy of an article published in Astrobiology © 2014 copyright Mary Ann Liebert, Inc.; Astrobiology is available online at: http://online.liebertpub.com.en
dc.subjectQB Astronomyen
dc.subject.lccQBen
dc.titleUsing dimers to measure biosignatures and atmospheric pressure for terrestrial exoplanetsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Earth and Environmental Sciencesen
dc.contributor.institutionUniversity of St Andrews.St Andrews Isotope Geochemistryen
dc.identifier.doihttps://doi.org/10.1089/ast.2013.0990
dc.description.statusPeer revieweden


This item appears in the following Collection(s)

Show simple item record