WATER, METHANE, AND CARBON DIOXIDE PRESENT IN THE DAYSIDE SPECTRUM OF THE EXOPLANET HD 209458b

Swain, Mark R.; Tinetti, Giovanna; Vasisht, Gautam; Deroo, P.; Griffith, C. A.; Bouwman, J.; Chen, Pin; Yung, Yuk L.; Burrows, Adam; Brown, Linda R.; Matthews, J. M.; Rowe, Jason F.; Kuschnig, R.; Angerhausen, Daniel

doi:10.1088/0004-637x/704/2/1616

Cited by 259 publications

(242 citation statements)

References 25 publications

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“…For XO-1b in Tinetti et al (2010), both components are determined simultaneously through a joint minimization over the entire time-domain (including in-eclipse). This calibration approach has been described in detail in SVT08 and updated in Swain et al (2009Swain et al ( , 2009b. The minimization process minimizes the residual obtained by removing the eclipse light curve and the instrument model from the data:…”

Section: Observations and Methodsmentioning

confidence: 99%

“…From this initial result, molecular spectroscopy of exoplanet atmospheres has grown rapidly, using Spitzer (Grillmair et al 2008), Hubble (Swain et al 2009a(Swain et al , 2009b, and ground-based measurements Thatte et al 2010;Snellen et al 2010). The alkali element sodium has also been detected in exoplanet atmospheres using Hubble, (Charbonneau et al 2002) and ground-based measurements have also been made (Redfield et al 2008;Snellen et al 2008).…”

Section: Introductionmentioning

confidence: 99%

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NICMOS spectroscopy of HD 189733b

2010

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Abstract. Spectral features corresponding to methane and water opacity were reported based on transmission spectroscopy of HD 189733b with Hubble/NICMOS. Recently, these data, and a similar data set for XO-1b, have been reexamined in Gibson et al. (2010), who claim they cannot reliably reproduce prior results. We examine the methods used by the Gibson team and identify two specific issues that could act to increase the formal uncertainties and to create instability in the minimization process. This would also be consistent with the GPA10 finding that they could not identify a way to select among the several instrument models they constructed. In the case of XO-1b, the Gibson team significantly changed the way in which the instrument model is defined (both with respect to the three approaches they used for HD 189733b, and the approach used by previous authors); this change, which omits the effect of the spectrum position on the detector, makes direct intercomparison of results difficult. In the experience of our group, the position of the spectrum on the detector is an important element of the instrument model because of the significant residual structure in the NICMOS spectral flat field. The approach of changing instrument models significantly complicates understanding the data reduction process and interpreting the results. Our team favors establishing a consistent method of handling NICMOS instrument systematic errors and applying it uniformly to data sets.

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Section: Observations and Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

NICMOS spectroscopy of HD 189733b

2010

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“…Agol et al 2010;Beaulieu et al 2008Beaulieu et al , 2010Beaulieu et al , 2011Brown 2001;Burke et al 2010;Charbonneau et al 2005Charbonneau et al , 2008Deming et al 2013;Désert et al 2011;Grillmair et al 2008;Knutson et al 2007;Machalek et al 2009;Pont et al 2008;Sing et al 2011a;Stevenson et al 2010;Swain et al 2008Swain et al , 2009b. Parametric models approximate systematic noise via the use of auxiliary information of the instrument, the so-called optical state vectors, which often include the positional drifts of the star on the detector, the focus and the detector temperature changes, the positional angles of the telescope on the sky etc.…”

Section: Primary Transit Observationsmentioning

confidence: 99%

“…The data were recorded with Spitzer IRAC/IRS/MIPS Grillmair et al 2008;Deming et al 2006) and Hubble NICMOS (Swain et al 2009a(Swain et al , 2009b. The spectral simulations and data interpretations, were performed by different teams, using radiative-transfer models and spectral retrieval methods.…”

Section: Fig 7amentioning

confidence: 99%

Spectroscopy of planetary atmospheres in our Galaxy

Tinetti

Encrenaz

Coustenis

2013

Astron Astrophys Rev

126

111

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About 20 years after the discovery of the first extrasolar planet, the number of planets known has grown by three orders of magnitude, and continues to increase at neck breaking pace. For most of these planets we have little information, except for the fact that they exist and possess an address in our Galaxy. For about one third of them, we know how much they weigh, their size and their orbital parameters. For less than 20, we start to have some clues about their atmospheric temperature and composition. How do we make progress from here?We are still far from the completion of a hypothetical Hertzsprung-Russell diagram for planets comparable to what we have for stars, and today we do not even know whether such classification will ever be possible or even meaningful for planetary objects. But one thing is clear: planetary parameters such as mass, radius and temperature alone do not explain the diversity revealed by current observations. The chemical composition of these planets is needed to trace back their formation history and evolution, as happened for the planets in our Solar System. As in situ measurements are and will remain off-limits for exoplanets, to study their chemical composition we will have to rely on remote sensing spectroscopic observations of their gaseous envelopes.

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“…Impressive progress has been made with Spitzer (Swain et al 2009)and HST (Charbonneau et al 2002), in obtaining the first spectral diagnostics of exoplanets. Two techniques can be used to probe transiting extrasolar planet atmospheres with JWST.…”

Section: Spectroscopymentioning

confidence: 99%

The James Webb Space Telescope and its capabilities for exoplanet science

Clampin

2010

Proc. IAU

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Abstract. The James Webb Space Telescope is a large aperture (6.5 meter), cryogenic space telescope with a suite of near and mid-infrared instruments covering the wavelength range of 0.6 ?m to 28 ?m. JWSTs primary science goal is to detect and characterize the first galaxies. It will also study the assembly of galaxies, star formation, and the formation of evolution of planetary systems. JWSTs instrument complement offers numerous capabilities to study the formation and evolution of exoplanets via direct imaging, high contrast coronagraphic imaging and photometric and spectroscopic observations of transiting exoplanets.

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WATER, METHANE, AND CARBON DIOXIDE PRESENT IN THE DAYSIDE SPECTRUM OF THE EXOPLANET HD 209458b

Cited by 259 publications

References 25 publications

NICMOS spectroscopy of HD 189733b

NICMOS spectroscopy of HD 189733b

Spectroscopy of planetary atmospheres in our Galaxy

The James Webb Space Telescope and its capabilities for exoplanet science

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