TEST The Tautenburg Exoplanet Search Telescope

Eigmüller, Philipp; Eislöffel, J.

doi:10.1017/s1743921308026598

Cited by 2 publications

(4 citation statements)

References 13 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The eclipsing binary presented in our work was detected in both surveys (Voss 2006;Eigmüller 2012) as planetary candidate. The object was published as an uncharacterized Algol type binary in Pasternacki et al (2011) with the identifier BEST F2_06375 after its planetary status was excluded.…”

Section: Photometric Observationssupporting

confidence: 58%

“…Photometric observations were taken during surveys for transiting planets with the Berlin Exoplanet Search Telescope (BEST; Rauer et al 2004) and the Tautenburg Exoplanet Search Telescope (TEST; Eigmüller & Eislöffel 2009). With both telescopes the same circumpolar field close to the galactic plane was observed for several years.…”

Section: Photometric Observationsmentioning

confidence: 99%

“…The pipeline used for the TEST data is described in Eigmüller & Eislöffel (2009). The methods used to analyze the BEST data set have been applied to various published BEST data sets (e.g., Fruth et al 2012Fruth et al , 2013Klagyivik et al 2013).…”

Section: Photometric Observationsmentioning

confidence: 99%

See 2 more Smart Citations

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

Eigmüller¹,

Eislöffel²,

Csizmadia³

et al. 2016

View full text Add to dashboard Cite

Only a few well characterized very low-mass M dwarfs are known today. Our understanding of M dwarfs is vital as these are the most common stars in our solar neighborhood. We aim to characterize the properties of a rare F+dM stellar system for a better understanding of the low-mass end of the Hertzsprung-Russel diagram. We used photometric light curves and radial velocity follow-up measurements to study the binary. Spectroscopic analysis was used in combination with isochrone fitting to characterize the primary star. The primary star is an early F-type main-sequence star with a mass of (1.493 ± 0.073) M e and a radius of (1.474 ± 0.040) R e . The companion is an M dwarf with a mass of (0.188 ± 0.014) M e and a radius of (0.234 ± 0.009) R e . The orbital period is (1.35121±0.00001) days. The secondary star is among the lowest-mass M dwarfs known to date. The binary has not reached a 1:1 spin-orbit synchronization. This indicates a young main-sequence binary with an age below ∼250 Myr. The mass-radius relation of both components are in agreement with this finding.

show abstract

Section: Photometric Observationssupporting

confidence: 58%

Section: Photometric Observationsmentioning

confidence: 99%

See 1 more Smart Citation

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

Eigmüller¹,

Eislöffel²,

Csizmadia³

et al. 2016

View full text Add to dashboard Cite

show abstract

“…Thanks to the increasing number of exoplanet search programs, such as the ground-based Optical Gravitational Lensing Experiment (OGLE) (Udalski et al 1992), the Hungarian Automated Telescope (HAT) (Bakos et al 2002(Bakos et al , 2004, the Super Wide Angle Search for Planets (SuperWASP) (Street et al 2003), the Berlin Exoplanet Search Telescope (BEST) (Rauer et al 2004), XO (McCullough et al 2005), the Transatlantic Exoplanet Survey (TrES) (Alonso et al 2007), and the Tautenburg Exoplanet Search Telescope (TEST) (Eigmüller & Eislöffel 2009) and the space-based missions "Convection, Rotation & Planetary Transits" (CoRoT) (Baglin et al 2002) and Kepler (Christensen-Dalsgaard et al 2007), the number of exoplanet transits has grown to 62 until September 1st 2009 2 and will grow drastically within the next years. These transiting planets have very short periods, typically <10 d, and very small semimajor axes of usually <0.1 AU, which is a selection effect based on geometry and Kepler's third law (Kepler et al 1619).…”

Section: Introductionmentioning

confidence: 99%

Transit detections of extrasolar planets around main-sequence stars

Heller

Mislis

Antoniadis³

2009

A&A

View full text Add to dashboard Cite

Context. The findings of more than 350 extrasolar planets, most of them nontransiting Hot Jupiters, have revealed correlations between the metallicity of the main-sequence (MS) host stars and planetary incidence. This connection can be used to calculate the planet formation probability around other stars, not yet known to have planetary companions. Numerous wide-field surveys have recently been initiated, aiming at the transit detection of extrasolar planets in front of their host stars. Depending on instrumental properties and the planetary distribution probability, the promising transit locations on the celestial plane will differ among these surveys. Aims. We want to locate the promising spots for transit surveys on the celestial plane and strive for absolute values of the expected number of transits in general. Our study will also clarify the impact of instrumental properties such as pixel size, field of view (FOV), and magnitude range on the detection probability. Methods. We used data of the Tycho catalog for ≈1 million objects to locate all the stars with 0 m m V 11.5 m on the celestial plane. We took several empirical relations between the parameters listed in the Tycho catalog, such as distance to Earth, m V , and (B − V), and those parameters needed to account for the probability of a star to host an observable, transiting exoplanet. The empirical relations between stellar metallicity and planet occurrence combined with geometrical considerations were used to yield transit probabilities for the MS stars in the Tycho catalog. Magnitude variations in the FOV were simulated to test whether this fluctuations would be detected by BEST, XO, SuperWASP and HATNet.Results. We present a sky map of the expected number of Hot Jupiter transit events on the basis of the Tycho catalog. Conditioned by the accumulation of stars towards the galactic plane, the zone of the highest number of transits follows the same trace, interrupted by spots of very low and high expectation values. The comparison between the considered transit surveys yields significantly differing maps of the expected transit detections. While BEST provides an unpromising map, those for XO, SuperWASP, and HATNet show FsOV with up to 10 and more expected detections. The sky-integrated magnitude distribution predicts 20 Hot Jupiter transits with orbital periods between 1.5 d and 50 d and m V < 8 m , of which two are currently known. In total, we expect 3412 Hot Jupiter transits to occur in front of MS stars within the given magnitude range. The most promising observing site on Earth is at latitude = −1.

show abstract

TEST The Tautenburg Exoplanet Search Telescope

Cited by 2 publications

References 13 publications

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

Transit detections of extrasolar planets around main-sequence stars

Contact Info

Product

Resources

About