The Multi-site All-Sky CAmeRA (MASCARA)

Talens, G. J. J.; Spronck, Jo W.; Lesage, A.-L.; Otten, G. P. P. L.; Stuik, Remko; Pollacco, D.; Snellen, I. A. G.

doi:10.1051/0004-6361/201630319

Cited by 69 publications

(73 citation statements)

References 28 publications

(23 reference statements)

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“…Note added in proof.. During the preparation of this paper, our team became aware of another paper by The Multi-site All-Sky CAmeRA (MASCARA) Collaboration (Talens et al 2017b) reporting the discovery of a planetary companion to the host star discussed here, HD 185603 (Talens et al 2017a). While we assume that this planetary companion is indeed , no information about the analysis Figure 14.…”

Section: Discussionmentioning

confidence: 99%

KELT-20b: A Giant Planet with a Period of P ∼ 3.5 days Transiting the V ∼ 7.6 Early A Star HD 185603

Lund

Rodriguez

Zhou

et al. 2017

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We report the discovery of KELT-20b, a hot Jupiter transiting a V 7.6 early A star, HD 185603, with an orbital period of P 3.47  days. Archival and follow-up photometry, Gaia parallax, radial velocities, Doppler tomography, and AO imaging were used to confirm the planetary nature of KELT-20b and characterize the system. From global modeling we infer that KELT-20 is a rapidly rotating ) . We place a 3s upper limit of M 3.5 J on the mass of the planet. Doppler tomographic 1 measurements indicate that the planetary orbit normal is well aligned with the projected spin axis of the star ( 3 . 4 2 . 1 l =    ). The inclination of the star is constrained to I 24 . 4 155 . 6 *  < <  , implying a three-dimensional spin-orbit alignment of 1 . 3 69 . 8 y  < <  . KELT-20b receives an insolation flux of 8 10 erg s cm 9 1 2´--, implying an equilibrium temperature of of ∼2250 K, assuming zero albedo and complete heat redistribution. Due to the high stellar T eff , KELT-20b also receives an ultraviolet (wavelength d 91.2  nm) insolation flux of 9.1 10 erg s cm 4 1 2´--, possibly indicating significant atmospheric ablation. Together with WASP-33, Kepler-13 A, HAT-P-57, KELT-17, and KELT-9, KELT-20 is the sixth A star host of a transiting giant planet, and the thirdbrightest host (in V ) of a transiting planet.

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Section: Discussionmentioning

confidence: 99%

KELT-20b: A Giant Planet with a Period of P ∼ 3.5 days Transiting the V ∼ 7.6 Early A Star HD 185603

Lund

Rodriguez

Zhou

et al. 2017

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“…Future and current planet hunting missions, such as the Transiting Exoplanet Survey Satellite (TESS ) and the ground-based Kilodegree Extremely Little Telescope ( KELT Pepper et al 2007) and the Multi-site All-Sky CAmeRA (MASCARA Talens et al 2017), have and will detect many hot planets transiting relatively bright stars. This will significantly increase the number of objects for which short-cadence, high-resolution optical transmission spectroscopy can be performed with 4-meter or 10-meter class telescopes.…”

Section: Discussionmentioning

confidence: 99%

A Decade of Hα Transits for HD 189733 b: Stellar Activity versus Absorption in the Extended Atmosphere

Cauley

Redfield

Jensen

2017

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HD 189733 b is one of the most well-studied exoplanets due to its large transit depth and host star brightness. The focus on this object has produced a number of high-cadence transit observations using high-resolution optical spectrographs. Here we present an analysis of seven full Hα transits of HD 189733 b using HARPS on the 3.6 meter La Silla telescope and HIRES on Keck I, taken over the course of nine years from 2006 to 2015. Hα transmission signals are analyzed as a function of the stellar activity level, as measured using the normalized core flux of the Ca II H and K lines. We find strong variations in the strength of the Hα transmission spectrum from epoch to epoch. However, there is no clear trend between the Ca II core emission and the strength of the in-transit Hα signal, although the transit showing the largest absorption value also occurs when the star is the most active. We present simulations of the in-transit contrast effect and find that the planet must consistently transit active latitudes with very strong facular and plage emission regions in order to reproduce the observed line strengths. We also investigate the measured velocity centroids with models of planetary rotation and show that the small line profile velocities could be due to large velocities in the upper atmosphere of the planet. Overall, we find it more likely that the measured Hα signals arise in the extended planetary atmosphere, although a better understanding of active region emission for active stars such as HD 189733 are needed.

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“…The design of bRing is based on the earlier on-sky validated design of MASCARA (Snellen et al 2012(Snellen et al , 2013Stuik et al 2014Stuik et al , 2016Talens et al 2017), which uses five cameras to take images of the whole visible sky above airmass 2 and to search for transiting exoplanets around bright stars (4 < m v < 8). The primary science goal of bRing is to monitor β Pictoris during the Hill sphere transit of β Pictoris b and to issue triggers for detailed observations if a transiting event is detected.…”

Section: Bringmentioning

confidence: 99%

“…The data reduction is similar to that of MASCARA as described in Talens et al (2017) is transferred to Leiden Observatory where systematic corrections are computed every two weeks using a modified version of the coarse decorrelation algorithm (Collier Cameron et al 2006;Talens et al 2017). …”

Section: Data Reductionmentioning

confidence: 99%

bRing: An observatory dedicated to monitoring the β Pictoris b Hill sphere transit

Stuik

Bailey

Dorval

et al. 2017

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Aims. We describe the design and first light observations from the β Pictoris b Ring ("bRing") project. The primary goal is to detect photometric variability from the young star β Pictoris due to circumplanetary material surrounding the directly imaged young extrasolar gas giant planet β Pictoris b. Methods. Over a nine month period centred on September 2017, the Hill sphere of the planet will cross in front of the star, providing a unique opportunity to directly probe the circumplanetary environment of a directly imaged planet through photometric and spectroscopic variations. We have built and installed the first of two bRing monitoring stations (one in South Africa and the other in Australia) that will measure the flux of β Pictoris, with a photometric precision of 0.5% over 5 min. Each station uses two wide field cameras to cover the declination of the star at all elevations. Detection of photometric fluctuations will trigger spectroscopic observations with large aperture telescopes in order to determine the gas and dust composition in a system at the end of the planet-forming era. Results. The first three months of operation demonstrate that bRing can obtain better than 0.5% photometry on β Pictoris in five minutes and is sensitive to nightly trends enabling the detection of any transiting material within the Hill sphere of the exoplanet.

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The Multi-site All-Sky CAmeRA (MASCARA)

Cited by 69 publications

References 28 publications

KELT-20b: A Giant Planet with a Period of P ∼ 3.5 days Transiting the V ∼ 7.6 Early A Star HD 185603

KELT-20b: A Giant Planet with a Period of P ∼ 3.5 days Transiting the V ∼ 7.6 Early A Star HD 185603

A Decade of Hα Transits for HD 189733 b: Stellar Activity versus Absorption in the Extended Atmosphere

bRing: An observatory dedicated to monitoring the β Pictoris b Hill sphere transit

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