Multi-wavelength characterization of the outskirts of spiral galaxies

Bakos, J.; Trujillo, Ignacio

doi:10.1017/s174392131000298x

Cited by 1 publication

(4 citation statements)

References 8 publications

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“…Our finding that the planet is about 4.23 times bigger than the Earth in radius agrees closely with the NEA value of 4.68 R ⊕ , and in apparent exact agreement with that of Bakos et al (2010). Bakos et al (2009Bakos et al ( , 2010 found an eccentricity of 0.198 to the planetary orbit, having a periastron longitude of ∼355 • with a formal error of about 15 • . In other words, the major axis of the elliptical orbit is not far from the plane of the sky, the planet exiting from the transit more quickly than its entrance.…”

Section: Individual Systemssupporting

confidence: 89%

“…3.3 KOI 3.01 KOI 3.01 is another object whose planetary status was studied by the earlier HATNet Project (Bakos et al, 2002(Bakos et al, , 2009(Bakos et al, , 2010. The star is also known as HAT-P-11 and, as a confirmed planet, Kepler-3.…”

Section: Individual Systemsmentioning

confidence: 99%

“…Disentangling the photometric effects of maculation from those of orbital eccentricity is not straightforward for the empirical analysis of a single transit, as we are doing. Bakos et al (2009) also noted the complications to parameter estimation arising from the interactions of such varied causes of data variation. For the present, therefore, this apparent confirmation of the orbital eccentricity should be regarded cautiously.…”

Section: Individual Systemsmentioning

confidence: 99%

“…In the case of KOI 3.01, the mass estimate comes fromBakos et al (2009). This yields a mass ∼50% more than that of the formula.…”

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confidence: 99%

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Analysis of selected Kepler Mission planetary light curves

Rhodes

Budding

2014

Astrophys Space Sci

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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.

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Section: Individual Systemssupporting

confidence: 89%

Section: Individual Systemsmentioning

confidence: 99%

Section: Individual Systemsmentioning

confidence: 99%

“…In the case of KOI 3.01, the mass estimate comes fromBakos et al (2009). This yields a mass ∼50% more than that of the formula.…”

mentioning

confidence: 99%

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