NEAR-IR DIRECT DETECTION OF WATER VAPOR IN TAU BOÖTIS b

Lockwood, Alexandra; Johnson, John Asher; Bender, Chad F.; Carr, John S.; Barman, Travis; Richert, Alexander J. W.; Blake, Geoffrey A.

doi:10.1088/2041-8205/783/2/l29

Cited by 113 publications

(175 citation statements)

References 43 publications

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“…This is also a rough upper bound for the spectroscopic contrast a spec . Since the cross-correlation analyses described in Section 4.3 are not very sensitive to contrast ratios, varying the value of a spec does not change our conclusions on the RV of the planet, and thus the system inclination (Lockwood et al 2014). However, the specific value of a s does affect our conclusions on the composition and structure of the planet's atmosphere.…”

Section: Model Planetary Spectrummentioning

confidence: 89%

“…Lockwood et al (2014) showed that the CCF is proportional to the log of the likelihood. At each epoch, we can easily retrieve and confirm the stellar velocity, as shown by the single strong peak in panel A of Figure 5.…”

Section: Two-dimensional Cross-correlationmentioning

confidence: 99%

“…The specific departure from Lockwood et al (2014) is the use of PCA to correct for telluric features in the data (Section 3.3). Our analysis of five nights of L-band data recovers a projected Keplerian orbital velocity of 121±8 km s −1 , a mass of …”

Section: Tests Of the Orbital Solutionmentioning

confidence: 99%

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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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Section: Model Planetary Spectrummentioning

confidence: 89%

Section: Two-dimensional Cross-correlationmentioning

confidence: 99%

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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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“…One way to mitigate these issues is by using ground-based highdispersion spectroscopy. For example, detections of sodium and potassium have been presented in the optical (Redfield et al 2008;Snellen et al 2008;Sing et al 2011a;Wood et al 2011;Jensen et al 2011;Zhou & Bayliss 2012;Wyttenbach et al 2015), and detections of carbon monoxide and water in the infrared (Brogi et al 2012(Brogi et al , 2014Rodler et al 2012;de Kok et al 2013;Birkby et al 2013;Lockwood et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Using the chromatic Rossiter-McLaughlin effect to probe the broadband signature in the optical transmission spectrum of HD 189733b

Gloria

Snellen

Albrecht

2015

A&A

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Context. Transmission spectroscopy is a powerful technique for probing exoplanetary atmospheres. A successful ground-based observational method uses a differential technique that uses high-dispersion spectroscopy, but it only preserves narrow features in transmission spectra. Broadband features, such as the remarkable Rayleigh-scattering slope from possible hazes in the atmosphere of HD 189733b as observed by the Hubble Space Telescope, cannot be probed in this way. Aims. Here we use the chromatic Rossiter-McLaughlin (RM) effect to measure the Rayleigh-scattering slope in the transmission spectrum of HD 189733b with the aim to show that it can be effectively used to measure broadband transmission features. The amplitude of the RM effects depends on the effective size of the planet, and in the case of an atmospheric contribution therefore depends on the observed wavelength. Methods. We analysed archival HARPS data of three transits of HD 189733b, covering a wavelength range of 400 to 700 nm. The radial velocity (RV) time-series were determined for white light and for six wavelength bins each 50 nm wide, using the crosscorrelation profiles as provided by the HARPS data reduction pipeline. The RM effect was first fitted to the white-light RV time series using the publicly available code AROME. The residuals to this best fit were subsequently subtracted from the RV time series of each wavelength bin, after which they were also fitted using the same code, leaving only the effective planet radius to vary. Results. We measured the slope in the transmission spectrum of HD 189733b at a 2.5σ significance. Assuming it is due to Rayleigh scattering and not caused by stellar activity, it would correspond to an atmospheric temperature, as set by the scale height, of T = 2300 ± 900 K, well in line with previously obtained results. Conclusions. Ground-based high-dispersion spectral observations can be used to probe broad-band features in the transmission spectra of extrasolar planets, such as the optical Rayleigh-scattering slope of HD 189733b, by using the chromatic Rossiter-McLaughlin effect. The precision achieved with HARPS per transit is about an order of magnitude lower than that with STIS on the Hubble Space Telescope. This method will be particularly interesting in conjunction with the new echelle spectrograph ESPRESSO, which currently is under construction for ESO's Very Large Telescope, which will provide a gain in signal-to-noise ratio of about a factor 4 compared to HARPS. This will be of great value because of the limited and uncertain future of the Hubble Space Telescope and because the future James Webb Space Telescope will not cover this wavelength regime.

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“…Kolbl et al (2015) observed planet-hosting stars from the Kepler survey with optical Keck HIRES spectroscopy in order to search for binary companions with relative radial velocities greater than 10 km s −1 such that the secondary absorption lines are Doppler shifted. A similar technique is used to probe absorption lines in the atmospheres of hot Jupiters, which exhibit rapidly varying velocity offsets (Snellen et al 2010;de Mooij et al 2012;Birkby et al 2013;Lockwood et al 2014). For cases where the hidden companion has a significantly different effective temperature than the target star, Kolbl et al (2015) were also able to detect companions with smaller radial velocity offsets.…”

Section: Introductionmentioning

confidence: 99%

Friends of Hot Jupiters. Iii. An Infrared Spectroscopic Search for Low-Mass Stellar Companions

Piskorz

Knutson

Ngo

et al. 2015

ApJ

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Surveys of nearby field stars indicate that stellar binaries are common, yet little is known about the effects that these companions may have on planet formation and evolution. The Friends of Hot Jupiters project uses three complementary techniques to search for stellar companions to known planet-hosting stars: radial velocity monitoring, adaptive optics imaging, and near-infrared spectroscopy. In this paper, we examine high-resolution K band infrared spectra of fifty stars hosting gas giant planets on short-period orbits. We use spectral fitting to search for blended lines due to the presence of cool stellar companions in the spectra of our target stars, where we are sensitive to companions with temperatures between 3500 and 5000 K and projected separations less than 100 AU in most systems. We identify eight systems with candidate low-mass companions, including one companion that was independently detected in our AO imaging survey. For systems with radial velocity accelerations, a spectroscopic non-detection rules out scenarios involving a stellar companion in a high inclination orbit. We use these data to place an upper limit on the stellar binary fraction at small projected separations, and show that the observed population of candidate companions is consistent with that of field stars and also with the population of wide-separation companions detected in our previous AO survey. We find no evidence that spectroscopic stellar companions are preferentially located in systems with short-period gas giant planets on eccentric and/or misaligned orbits.

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NEAR-IR DIRECT DETECTION OF WATER VAPOR IN TAU BOÖTIS b

Cited by 113 publications

References 43 publications

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

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

Using the chromatic Rossiter-McLaughlin effect to probe the broadband signature in the optical transmission spectrum of HD 189733b

Friends of Hot Jupiters. Iii. An Infrared Spectroscopic Search for Low-Mass Stellar Companions

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