Binarity of transit host stars

Daemgen, S.; Hormuth, F.; Brandner, W.; Bergfors, C.; Janson, Markus; Hippler, S.; Henning, Th.

doi:10.1051/0004-6361/200810988

Cited by 122 publications

(205 citation statements)

References 34 publications

Supporting

Mentioning

182

Contrasting

Order By: Relevance

“…They gave a projected separation between the TrES-2 host star and the companion candidate of (1.089 ± 0.008) . Our values for the projected separation of the dip relative to the center of the transit (see Table 5) is five orders of magnitude lower than the projected separation of the companion candidate Daemgen et al (2009) found. Thus, this companion candidate can not be the origin of the second dip in our light curves.…”

Section: Companioncontrasting

confidence: 71%

See 1 more Smart Citation

Planetary transit observations at the University Observatory Jena: TrES‐2

Raetz¹,

Mugrauer²,

Schmidt³

et al. 2009

Astron Nachr

View full text Add to dashboard Cite

We report on observations of several transit events of the transiting planet TrES-2 obtained with the Cassegrain-TeleskopKamera at the University Observatory Jena. Between March 2007 and November 2008 ten different transits and almost a complete orbital period were observed. Overall, in 40 nights of observation 4291 exposures (in total 71.52 h of observation) of the TrES-2 parent star were taken. With the transit timings for TrES-2 from the 34 events published by the TrESnetwork, the Transit Light Curve project and the Exoplanet Transit Database plus our own ten transits, we find that the orbital period is P = (2.470614 ± 0.000001) d, a slight change by ∼ 0.6 s compared to the previously published period. We present new ephemeris for this transiting planet. Furthermore, we found a second dip after the transit which could either be due to a blended variable star or occultation of a second star or even an additional object in the system. Our observations will be useful for future investigations of timing variations caused by additional perturbing planets and/or stellar spots and/or moons.

show abstract

Section: Companioncontrasting

confidence: 71%

“…First hint for the validity of this hypotheses gave Daemgen et al (2009). Using high-resolution "Lucky Imaging" with AstraLux at the 2.2 m Calar Alto telescope they found a companion candidate (physical association needs to be confirmed by second epoch observations) close to the TrES-2 host star.…”

Section: Companionmentioning

confidence: 99%

Planetary transit observations at the University Observatory Jena: TrES‐2

Raetz¹,

Mugrauer²,

Schmidt³

et al. 2009

Astron Nachr

View full text Add to dashboard Cite

show abstract

“…In most cases, the optimized value is close to the van Hamme value. The abnormally high value found for KOI 1.01 may be a result of it having a (visual) binary companion (Daemgen et al, 2009), thereby affecting the assigned (near solar) temperature. Table 5 allows assessment of the quality of the lightcurve fittings.…”

Section: Resultsmentioning

confidence: 95%

Analysis of selected Kepler Mission planetary light curves

Rhodes

Budding

2014

Astrophys Space Sci

View full text Add to dashboard Cite

We have modified the graphical user interfaced close binary system analysis program CurveFit to the form WinKepler and applied it to 16 representative planetary candidate light curves found in the NASA Exoplanet Archive (NEA) at the Caltech website http://exoplanetarchive.ipac.caltech.edu, with an aim to compare different analytical approaches. WinKepler has parameter options for a realistic physical model, including gravity-brightening and structural parameters derived from the relevant Radau equation. We tested our best-fitting parameter-sets for formal determinacy and adequacy.A primary aim is to compare our parameters with those listed in the NEA. Although there are trends of agreement, small differences in the main parameter values are found in some cases, and there may be some relative bias towards a 90 • value for the NEA inclinations. These are assessed against realistic error estimates.Photometric variability from causes other than planetary transits affects at least 6 of the data-sets studied; with small pulsational behaviour found in 3 of those. For the false positive KOI 4.01, we found that the eclipses could be modelled by a faint background clas- Our empirical checks of limb-darkening, in the cases of KOI 1.01 and 12.01, revealed that the assigned stellar temperatures are probably incorrect. For KOI 13.01, our empirical mass-ratio differs by about 7% from that of Mislis and Hodgkin (Mon. Not. R. Astron. Soc. 422:1512Soc. 422: ,2012, who neglected structural effects and higher order terms in the tidal distortion. Such detailed parameter evaluation, additional to the usual main geometric ones, provides an additional objective for this work.

show abstract

“…In order to derive approximate spectral types for the binary or multiple systems discovered in the AstraLux M dwarf survey and exclude background contaminants, each target was observed in SDSS i ′ -and z ′ -band and individual spectral types were derived from i ′ − z ′ colours and the integrated JHK spectral types, with estimated errors of ±1 spectral subtype (see Daemgen et al 2009;Bergfors et al 2010). Obtaining near-infrared spectral types allows us to Table 2.…”

Section: Comparison Of Near-infrared Spectral Types To Astralux Opticmentioning

confidence: 99%

Characterization of close visual binaries from the AstraLux Large M Dwarf Survey

Bergfors¹,

Brandner²,

Bonnefoy³

et al. 2015

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

We present VLT/SINFONI J, H + K spectra of seven close visual pairs in M dwarf binary/triple systems, discovered or observed by the AstraLux M dwarf survey. We determine the spectral types to within ±1.0 subclasses from comparison to template spectra and the strength of K-band water absorption, and derive effective temperatures. The results are compared to optical spectral types of the unresolved binary/multiple systems, and we confirm that our photometric method to derive spectral types in the AstraLux M dwarf survey is accurate. We look for signs of youth such as chromospheric activity and low surface gravity, and find an age in the range 0.25 − 1 Gyr for the GJ 852 system. Strong Li absorption is detected in optical spectra of the triple system J024902 obtained with FEROS at the ESO-MPG 2.2 m telescope. The equivalent width of the absorption suggests an age consistent with the β Pic moving group. However, further observations are needed to establish group membership. Ongoing orbital monitoring will provide dynamical masses and thus calibration of evolutionary models for low mass stars.

show abstract

Binarity of transit host stars

Cited by 122 publications

References 34 publications

Planetary transit observations at the University Observatory Jena: TrES‐2

Planetary transit observations at the University Observatory Jena: TrES‐2

Analysis of selected Kepler Mission planetary light curves

Characterization of close visual binaries from the AstraLux Large M Dwarf Survey

Contact Info

Product

Resources

About