Detection of carbon monoxide in the high-resolution day-side spectrum of the exoplanet HD 189733b

Kok, Remco de; Brogi, Matteo; Snellen, I. A. G.; Birkby, Jayne; Albrecht, S.; Mooij, Ernst de

doi:10.1051/0004-6361/201321381

Cited by 225 publications

(177 citation statements)

References 52 publications

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“…After basic calibrations, we optimally extracted a 1D spectrum for each position along the slit, and subsequently removed the stellar contribution for each position. The resulting spectra were crosscorrelated with planet model spectra (Extended Data Fig.1), which were produced in a similar way as for our previous work on hot Jupiters [10][11][12] .…”

Section: Methods Summarymentioning

confidence: 99%

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confidence: 99%

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Fast spin of the young extrasolar planet β Pictoris b

Snellen

Brandl

Kok

et al. 2014

Nature

410

416

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The spin-rotation of a planet arises from the accretion of angular momentum during its Near-infrared high-dispersion spectroscopy has been used to characterize the atmospheres of hot Jupiters in close-in orbits [10][11] . Such observations utilize changes in the radial component of the orbital velocity of the planet (resulting in changes in Doppler shift) to filter out the quasi-stationary telluric and stellar contributions in the spectra. Here we make use of the spatial separation and the difference in spectral signature between the planet and star, which allow the starlight to be filtered out. A similar technique 12 has been applied very successfully 13 at a medium spectral dispersion to characterize the exoplanet HR8799c. We observed the β Pictoris system 7,8 (K=3.5) using the Cryogenic highResolution InfraRed Echelle Spectrograph CRIRES 14 located at the Nasmyth focus of UT1 of the Very Large Telescope (VLT) of the European Southern Observatory (ESO) at Cerro Paranal in Chile on the night of 17 December 2013, with the slit oriented in such way that it encompassed the planet and star.An important step in the data analysis is the optimal removal of the stellar contribution along the slit, which for this A-star consists mostly of a telluric absorption spectrum. The resulting spectra were cross-correlated with theoretical spectral templates constructed in a similar way as in our previous work on hot Jupiters 10-11 , varying the planet's atmospheric temperature pressure (T/p) profile, the carbon monoxide abundance and that of water vapor and methane, which can also show features in the observed wavelength range. Note that there is a strong degeneracy between the atmospheric T/p profile and the abundance of the molecular species, meaning that different combinations of these parameters result in nearly identical template spectra.At the expected planet position a broad and blue-shifted signal is apparent (see Figure 1), which is strongest when the cross-correlation is performed with a spectral template from an atmospheric model with deep carbon monoxide lines and a small contribution from water. We estimate the signal to have a SNR of 6.4 by cross-correlating the residual spectrum with a broadened model template, and compare the peak of the cross-correlation profile with the standard deviation. If we use the crosscorrelation profile as seen in Figure 1 to estimate the SNR, we need to take into account the width of the signal and the dependence of adjacent pixels in the profile. This results in an SNR of 7.8, but this latter method we found to be less accurate, since it does not properly include contributions from correlated noise structures on scales of the broad signal. Cross-correlation with the optimal spectrum of water vapor alone provides a marginal signal at SNR~2, which means we cannot claim a firm detection of water in the planet atmosphere. No signal is retrieved for methane models (see Extended Data Fig. 1).We fit the planet profile using a grid of artificial cross-correlation functions, produced by crossc...

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Section: Methods Summarymentioning

confidence: 99%

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mentioning

confidence: 99%

Fast spin of the young extrasolar planet β Pictoris b

Snellen

Brandl

Kok

et al. 2014

Nature

410

416

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“…Conversely, those that transited (HD 209458 b and HD 189773 b; Snellen et al 2010;Birkby et al 2013;de Kok et al 2013) have not needed phase offsets, arguably due to their transits enabling far better defined ephemerides.…”

Section: Improving Ephemerides For Non-transiting Planetsmentioning

confidence: 99%

Discovery of Water at High Spectral Resolution in the Atmosphere of 51 Peg b

Birkby¹,

Kok²,

Brogi³

et al. 2017

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189

244

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We report the detection of water absorption features in the day side spectrum of the first-known hot Jupiter, 51 Peg b, confirming the star-planet system to be a double-lined spectroscopic binary. We use high-resolution ( » R 100,000), m 3.2 m spectra taken with CRIRES/VLT to trace the radial-velocity shift of the water features in the planet's day side atmosphere during 4 hr of its 4.23 day orbit after superior conjunction. We detect the signature of molecular absorption by water at a significance of J , placing it at the transition boundary between Jovian and Neptunian worlds. We determine upper and lower limits on the orbital inclination of the system of  < <  i 70 8 2.2. We also provide an updated orbital solution for 51 Peg b, using an extensive set of 639 stellar radial velocities measured between 1994 and 2013, finding no significant evidence of an eccentric orbit. We find no evidence of significant absorption or emission from other major carbon-bearing molecules of the planet, including methane and carbon dioxide. The atmosphere is non-inverted in the temperature-pressure region probed by these observations. The deepest absorption lines reach an observed relative contrast of´-0.9 10 3 with respect to the host star continuum flux at an angular separation of 3 milliarcseconds. This work is consistent with a previous tentative report of K-band molecular absorption for 51 Peg b by Brogi et al.

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“…With the CRyogenic InfraRed Echelle Spectrograph (CRIRES) at the VLT, Snellen et al (2010) provided a proof of concept of this technique and detected carbon monoxide in the atmosphere of the transiting exoplanet HD 209458 b consistent with previous detections using Hubble Space Telescope data (Swain et al 2009). By detecting the RV variation of a planet's atmospheric lines in about six hours of observations on single nights, further work has detected the dayside and nightside thermal spectra of various transiting and non-transiting hot Jupiters, reporting detections of water and carbon monoxide, as well as the presence of winds and measurements of the length of day (Snellen et al 2010;Brogi et al 2012Brogi et al , 2013Brogi et al , 2014Brogi et al , 2016Rodler et al 2012;Birkby et al 2013;de Kok et al 2013;Snellen et al 2014;Schwarz et al 2015). With HARPS, Martins et al (2015) recently observed the reflected light spectrum of 51 Peg b in a similar manner, combining 12.5 hr of data taken over seven nights when the full dayside of the planet was observable.…”

Section: Introductionmentioning

confidence: 99%

EVIDENCE FOR THE DIRECT DETECTION OF THE THERMAL SPECTRUM OF THE NON-TRANSITING HOT GAS GIANT HD 88133 b

Piskorz

Benneke

Crockett

et al. 2016

ApJ

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We target the thermal emission spectrum of the non-transiting gas giant HD 88133 b with high-resolution nearinfrared spectroscopy, by treating the planet and its host star as a spectroscopic binary. For sufficiently deep summed flux observations of the star and planet across multiple epochs, it is possible to resolve the signal of the hot gas giant's atmosphere compared to the brighter stellar spectrum, at a level consistent with the aggregate shot noise of the full data set. To do this, we first perform a principal component analysis to remove the contribution of the Earth's atmosphere to the observed spectra. Then, we use a cross-correlation analysis to tease out the spectra of the host star and HD 88133 b to determine its orbit and identify key sources of atmospheric opacity. In total, six epochs of Keck NIRSPEC L-band observations and three epochs of Keck NIRSPEC K-band observations of the HD 88133 system were obtained. Based on an analysis of the maximum likelihood curves calculated from the multi-epoch cross-correlation of the full data set with two atmospheric models, we report the direct detection of the emission spectrum of the non-transiting exoplanet HD 88133 b and measure a radial projection of the Keplerian orbital velocity of 40±15 km s , and an atmosphere opacity structure at high dispersion dominated by water vapor. This, combined with 11 years of radial velocity measurements of the system, provides the most up-to-date ephemeris for HD 88133.

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Detection of carbon monoxide in the high-resolution day-side spectrum of the exoplanet HD 189733b

Cited by 225 publications

References 52 publications

Fast spin of the young extrasolar planet β Pictoris b

Fast spin of the young extrasolar planet β Pictoris b

Discovery of Water at High Spectral Resolution in the Atmosphere of 51 Peg b

EVIDENCE FOR THE DIRECT DETECTION OF THE THERMAL SPECTRUM OF THE NON-TRANSITING HOT GAS GIANT HD 88133 b

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