The Search for an Atmospheric Signature of the Transiting Exoplanet HD 149026b1

Bozorgnia, Nassim; Fortney, Jonathan J.; McCarthy, C.; Fischer, Debra A.; Marcy, Geoffrey W.

doi:10.1086/508237

Cited by 29 publications

(5 citation statements)

References 25 publications

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“…However, the very shallow transit (depth 0.3 per cent) means that its light‐curve parameters remain ill defined despite the reasonably good quality of the available photometry. Wolf et al (2007) have studied the Rossiter–McLaughlin effect in the system and Bozorgnia et al (2006) have searched for the presence of lithium and potassium in the planetary atmosphere. Harrington et al (2007) observed a secondary eclipse of HD 149026 with Spitzer and found a high brightness temperature at 8 μm of 2300 ± 200 K for the planet.…”

Section: Results For Each Systemmentioning

confidence: 99%

Homogeneous studies of transiting extrasolar planets – I. Light-curve analyses

Southworth

2008

Monthly Notices of the Royal Astronomical Society

364

424

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I present a homogeneous analysis of the transit light curves of 14 well-observed transiting extrasolar planets. The light curves are modelled using JKTEBOP, random errors are measured using Monte Carlo simulations and the effects of correlated noise are included using a residualpermutation algorithm. The importance of stellar limb darkening on the light-curve solutions and parameter uncertainties is investigated using five different limb darkening laws and including different numbers of coefficients as fitted parameters. The linear limb darkening law cannot adequately fit the Hubble Space Telescope (HST) photometry of HD 209458, but the other four laws give very similar results to each other for all transit light curves. In most cases fixing the limb darkening coefficients at theoretically predicted values does not bias the results, but does cause the error estimates to be too small. The available theoretical limb darkening coefficients clearly disagree with empirical values measured from the HST light curves of HD 209458; limb darkening must be included as fitted parameters when analysing high-quality light curves.In most cases the results of my analysis agree with the values found by other authors, but the uncertainties I find can be significantly larger (by factors of up to 3). Despite these greater uncertainty estimates, the analyses of sets of independent light curves for both HD 189733 and HD 209458 lead to results which do not agree with each other. This discrepancy is worst for the ratio of the radii (6.7σ for HD 189733 and 3.7σ for HD 209458), which depends primarily on the depth of the transit. It is therefore not due to the analysis method but is present in the light curves. These underlying systematic errors cannot be detected from the reduced data alone unless at least three independent light curves are available for an individual planetary system.The surface gravities of transiting extrasolar planets are known to be correlated with their orbital periods. New surface gravity values, calculated from the light-curve results and the stellar spectroscopic orbits, show that this correlation is still present. New high-precision light curves are needed for HD 149026, OGLE-TR-10, OGLE-TR-56, OGLE-TR-132 and GJ 436, and new radial velocity curves for the XO-1, WASP-1, WASP-2 and the OGLE (Optical Gravitational Lensing Experiment) planetary systems.

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Section: Results For Each Systemmentioning

confidence: 99%

Homogeneous studies of transiting extrasolar planets – I. Light-curve analyses

Southworth

2008

Monthly Notices of the Royal Astronomical Society

364

424

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“…At visible wavelengths, where the emitted light from the planet is negligible, the technique of transmission spectroscopy has been employed from space-based platforms to study atoms, molecules, and clouds in the atmospheres of HD 209458b (Charbonneau et al 2002;Vidal-Madjar et al 2003;Barman 2007) and HD 189733b (Tinetti et al 2007;Pont et al 2008;Swain et al 2008a). Ground-based studies had yielded only upper limits, albeit valuable ones (Moutou et al 2001(Moutou et al , 2003Winn et al 2004;Deming et al 2005a;Narita et al 2005;Arribas et al 2006;Bozorgnia et al 2006) until the recent breakthrough detection by Redfield et al (2008) of atomic sodium in the atmosphere of HD 189733b. Searches for reflected starlight have delivered increasingly stringent constraints on the wavelength-dependent geometric albedo and phase function (Charbonneau et al 1999;Collier Cameron et al 2002;Leigh et al 2003a,b;Rowe et al 2006Rowe et al , 2008.…”

Section: Introductionmentioning

confidence: 99%

The Broadband Infrared Emission Spectrum of the Exoplanet HD 189733b

Charbonneau

Knutson

Barman

et al. 2008

Astrophysical Journal

290

353

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We present Spitzer Space Telescope time series photometry of the exoplanet system HD 189733 spanning two times of secondary eclipse, when the planet passes out of view behind the parent star. We estimate the relative eclipse depth in 5 distinct bands and find the planet-to-star flux ratio to be 0.256 +/- 0.014% (3.6 microns), 0.214 +/- 0.020% (4.5 microns), 0.310 +/- 0.034% (5.8 microns), 0.391 +/- 0.022% (8.0 microns), and 0.598 +/- 0.038% (24 microns). For consistency, we re-analyze a previously published time series to deduce a contrast ratio in an additional band, 0.519 +/- 0.020% (16 microns). Our data are strongly inconsistent with a Planck spectrum, and we clearly detect emission near 4 microns as predicted by published theoretical models in which this feature arises from a corresponding opacity window. Unlike recent results for the exoplanet HD 209458b, we find that the emergent spectrum from HD 189733b is best matched by models that do not include an atmospheric temperature inversion. Taken together, these two studies provide initial observational support for the idea that hot Jupiter atmospheres diverge into two classes, in which a thermal inversion layer is present for the more strongly irradiated objects.Comment: 20 pages, 3 figures, accepted to the Astrophysical Journal, minor revision

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“…So far, Na i detection via ground‐based high‐resolution spectroscopy has only been achieved on three transiting planets, HD 209458b (Snellen et al ; Langland‐Shula et al ; Jensen et al ), HD 189733b (Redfield et al ) and WASP‐17b (Wood et al ), along with numerous unsuccessful attempts (e.g. Narita et al ; Bozorgnia et al ). Recent detections around the K i resonance line by narrow‐band photometry have also been achieved with XO‐2b (Sing et al ) and HD 80606b (Colón et al ).…”

Section: Introductionmentioning

confidence: 99%

Detection of sodium absorption in WASP-17b with Magellan

Zhou

Bayliss

2012

Monthly Notices of the Royal Astronomical Society

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We present the detection of sodium absorption in the atmosphere of the extrasolar planet WASP-17b, an inflated 'hot-Jupiter' in a tight orbit around an F6 dwarf. In-transit observations of WASP-17 made with the MIKE spectrograph on the 6.5-m Magellan Telescope were analysed for excess planetary atmospheric absorption in the sodium I 'D' doublet spectral region. Using the interstellar sodium absorption lines as reference, we detect an excess 0.58 \pm 0.13 per cent transit signal, with 4.5{\sigma} confidence, at 1.5 {\AA} bandwidth around the stellar sodium absorption feature. This result is consistent with the previous VLT detection of sodium in WASP-17b, confirming that the planet has a highly inflated atmosphere.Comment: 6 pages, 4 figures and 2 tables, accepted by MNRA

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The Search for an Atmospheric Signature of the Transiting Exoplanet HD 149026b1

Cited by 29 publications

References 25 publications

Homogeneous studies of transiting extrasolar planets – I. Light-curve analyses

Homogeneous studies of transiting extrasolar planets – I. Light-curve analyses

The Broadband Infrared Emission Spectrum of the Exoplanet HD 189733b

Detection of sodium absorption in WASP-17b with Magellan

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