LSPM J1112+7626: Detection of a 41 Day M-Dwarf Eclipsing Binary From the Mearth Transit Survey

Irwin, Jonathan; Quinn, Samuel N.; Berta, Zachory K.; Latham, David W.; Torres, Guillermo; Burke, Christopher J.; Charbonneau, David; Dittmann, Jason; Esquerdo, Gilbert A.; Stefanik, R. P.; Oksanen, A.; Buchhave, Lars A.; Nutzman, P.; Berlind, P.; Calkins, M.; Falco, E.

doi:10.1088/0004-637x/742/2/123

Cited by 142 publications

(191 citation statements)

References 97 publications

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“…LL Aqr does not, in line with KIC 6131659 (P orb = 17.5 d, Bass et al 2012) and RW Lac (P orb = 10.4 d, Lacy et al 2005). LSPM J1112+7626 (P orb = 41.0 d, Irwin et al 2011) is an M-dwarf dEB which shows spot activity and inflated radii; its discord with the picture outlined above could easily be due to a young age.…”

Section: Discussionmentioning

confidence: 76%

The solar-type eclipsing binary system LL Aquarii

Southworth

2013

A&A

122

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The eclipsing binary LL Aqr consists of two late-type stars in an eccentric orbit with a period of 20.17 d. We use an extensive light curve from the SuperWASP survey augmented by published radial velocities and UBV light curves to measure the physical properties of the system. The primary star has a mass of 1.167 ± 0.009 M and a radius of 1.305 ± 0.007 R . The secondary star is an analogue of the Sun, with a mass and radius of 1.014 ± 0.006 M and 0.990 ± 0.008 R respectively. The system shows no signs of stellar activity: the upper limit on spot-induced rotational modulation is 3 mmag, it is slowly rotating, has not been detected at X-ray wavelengths, and the calcium H and K lines exhibit no emission. Theoretical stellar models provide a good match to its properties for a sub-solar metal abundance of Z = 0.008 and an age of 2.5 Gyr. Most low-mass eclipsing binary systems are found to have radii larger than expected from theoretical predictions, blamed on tidally-enhanced magnetic fields in these short-period systems. The properties of LL Aqr support this scenario: it exhibits negligible tidal effects, shows no signs of magnetic activity, and matches theoretical models well.

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Section: Discussionmentioning

confidence: 76%

The solar-type eclipsing binary system LL Aquarii

Southworth

2013

A&A

122

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“…Even in higher mass G-and K-dwarfs, strong magnetic activity in the stars results in disagreement with stellar models (Morales et al 2009). However, in wider separation M-dwarf DLEBs with magnetically inactive low-mass stars, the radii are still inflated (Irwin et al 2011;Doyle et al 2011), with no real convergence towards stellar models at longer periods (Birkby et al 2012). Obtaining K p for planets transiting M-dwarfs removes the uncertainty in stellar models and gives a direct and accurate characterisation of the star-planet system.…”

Section: Discussionmentioning

confidence: 99%

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

Kok

Brogi

Snellen

et al. 2013

A&A

213

170

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Context. After many attempts over more than a decade, high-resolution spectroscopy has recently delivered its first detections of molecular absorption in exoplanet atmospheres, both in transmission and thermal emission spectra. Targeting the combined signal from individual lines in molecular bands, these measurements use variations in the planet radial velocity to separate the planet signal from telluric and stellar contaminants. Aims. We apply high-resolution spectroscopy to probe molecular absorption in the day-side spectrum of the bright transiting hot Jupiter HD 189733b. Methods. We observed HD 189733b with the CRIRES high-resolution near-infrared spectograph on the Very Large Telescope during three nights, targeting possible absorption from carbon monoxide, water vapour, methane, and carbon dioxide, at 2.0 and 2.3 μm. Results. We detect a 5-σ absorption signal from CO at a contrast level of ∼4.5 × 10 −4 with respect to the stellar continuum, revealing the planet orbital radial velocity at 154 +4 −3 km s −1 . This allows us to solve for the planet and stellar mass in a similar way as for stellar eclipsing binaries, resulting in M s = 0.846 +0.068 −0.049 M and M p = 1.162 +0.058 −0.039 M Jup . No significant absorption is detected from H 2 O, CO 2 , or CH 4 and we determine upper limits on their line contrasts. Conclusions. The detection of CO in the day-side spectrum of HD 189733b can be made consistent with the haze layer proposed to explain the optical to near-infrared transmission spectrum if the layer is optically thin at the normal incidence angles probed by our observations, or if the CO abundance is high enough for the CO absorption to originate from above the haze. Our non-detection of CO 2 at 2.0 μm is not inconsistent with the deep CO 2 absorption from low-resolution NICMOS secondary eclipse data in the same wavelength range. If genuine, the absorption would be so strong that it blanks out any planet light completely in this wavelength range, leaving no high-resolution signal to be measured.

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“…Interestingly, the quantity (c/3 + d/5), which sets the integral of I(µ) over the stellar surface, defines the line along which c and d are most strongly correlated in the MCMC samples (see also Irwin et al 2011). For quadratic limb-darkening, the commonly quoted 2u 1 + u 2 combination (Holman et al 2006) has the same physical meaning.…”

Section: Combined White Light Curvementioning

confidence: 99%

THE FLAT TRANSMISSION SPECTRUM OF THE SUPER-EARTH GJ1214b FROM WIDE FIELD CAMERA 3 ON THEHUBBLE SPACE TELESCOPE

Berta

Charbonneau

Désert

et al. 2012

ApJ

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361

476

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Capitalizing on the observational advantage offered by its tiny M dwarf host, we present HST/WFC3 grism measurements of the transmission spectrum of the super-Earth exoplanet GJ1214b. These are the first published WFC3 observations of a transiting exoplanet atmosphere. After correcting for a ramp-like instrumental systematic, we achieve nearly photon-limited precision in these observations, finding the transmission spectrum of GJ1214b to be flat between 1.1 and 1.7 µm. Inconsistent with a cloud-free solar composition atmosphere at 8.2σ, the measured achromatic transit depth most likely implies a large mean molecular weight for GJ1214b's outer envelope. A dense atmosphere rules out bulk compositions for GJ1214b that explain its large radius by the presence of a very low density gas layer surrounding the planet. High-altitude clouds can alternatively explain the flat transmission spectrum, but they would need to be optically thick up to 10 mbar or consist of particles with a range of sizes approaching 1 µm in diameter.

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LSPM J1112+7626: Detection of a 41 Day M-Dwarf Eclipsing Binary From the Mearth Transit Survey

Cited by 142 publications

References 97 publications

The solar-type eclipsing binary system LL Aquarii

The solar-type eclipsing binary system LL Aquarii

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

THE FLAT TRANSMISSION SPECTRUM OF THE SUPER-EARTH GJ1214b FROM WIDE FIELD CAMERA 3 ON THEHUBBLE SPACE TELESCOPE

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