UBV(RI)C photometry of transiting planet hosting stars

Maxted, P. F. L.; Koen, C.; Smalley, B.

doi:10.1111/j.1365-2966.2011.19554.x

Cited by 21 publications

(25 citation statements)

References 47 publications

(30 reference statements)

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“…The T eff values obtained from CORALIE spectra have been found to be in agreement with those from the infrared flux method (Maxted et al 2011), suggesting that a change of more than 100 K is unlikely. However, Doyle et al (2012) found that [Fe/H] obtained using CORALIE spectra is, on average, 0.08 ± 0.06 dex lower than found using higher S/N HARPS spectra.…”

Section: Discussionsupporting

confidence: 67%

WASP-78b and WASP-79b: two highly-bloated hot Jupiter-mass exoplanets orbiting F-type stars in Eridanus

Smalley

Anderson

Cameron

et al. 2012

A&A

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We report the discovery of WASP-78b and WASP-79b, two highly-bloated Jupiter-mass exoplanets orbiting F-type host stars. WASP-78b orbits its V = 12.0 host star (TYC 5889-271-1) every 2.175 days and WASP-79b orbits its V = 10.1 host star (CD-30 1812) every 3.662 days. Planetary parameters have been determined using a simultaneous fit to WASP and TRAPPIST transit photometry and CORALIE radial-velocity measurements. For WASP-78b a planetary mass of 0.89 ± 0.08 M Jup and a radius of 1.70 ± 0.11 R Jup is found. The planetary equilibrium temperature of T P = 2350 ± 80 K for WASP-78b makes it one of the hottest of the currently known exoplanets. WASP-79b its found to have a planetary mass of 0.90 ± 0.08 M Jup , but with a somewhat uncertain radius due to lack of sufficient TRAPPIST photometry. The planetary radius is at least 1.70 ± 0.11 R Jup , but could be as large as 2.09 ± 0.14 R Jup , which would make WASP-79b the largest known exoplanet.

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Section: Discussionsupporting

confidence: 67%

WASP-78b and WASP-79b: two highly-bloated hot Jupiter-mass exoplanets orbiting F-type stars in Eridanus

Smalley

Anderson

Cameron

et al. 2012

A&A

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“…In the case of SWP, we do not deeply check whether the different sources give photometry de-reddened or not because neither SWEET-Cat nor the Exoplanets Data Explorer report any reddening information. We explicitely account for reddening in the case of those TPH listed in Maxted et al (2011), who report the colour excess E(B − V). Anyway, by a posteriori catalogue cross-matching, we were able to recover E(B − V) index for 154 stars out of the 335 SWP, and we found that more than 80% of them has E(B − V) = 0.…”

Section: Isochrone Placement: Implementationmentioning

confidence: 99%

“…The metallicity [Fe/H] and the logarithm of the surface gravity log g are always available from Sweet-Cat. If available, we took V magnitude and B − V colour index from Maxted et al (2011), otherwise we collected V from SWEET-Cat and B − V from The Site of California and Carnegie Program for Extrasolar Planet Search: Exoplanets Data Explorer 2 . As reported by Maxted et al (2011), the target stars of surveys that aim to discover exoplanets through transits are typically characterized by optical photometry of poor quality in the range V = 8.5−13 mag.…”

Section: Introductionmentioning

confidence: 99%

“…If available, we took V magnitude and B − V colour index from Maxted et al (2011), otherwise we collected V from SWEET-Cat and B − V from The Site of California and Carnegie Program for Extrasolar Planet Search: Exoplanets Data Explorer 2 . As reported by Maxted et al (2011), the target stars of surveys that aim to discover exoplanets through transits are typically characterized by optical photometry of poor quality in the range V = 8.5−13 mag. For stars brighter than V ≈ 12, optical photometry is usually available from Tycho catalogue, nevertheless, this catalogue is only complete up to V ≈ 11 and photometric accuracy rapidly deteriorates for V 9.5.…”

Section: Introductionmentioning

confidence: 99%

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Age consistency between exoplanet hosts and field stars

Bonfanti

Ortolani

Nascimbeni

2015

A&A

117

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Context. Transiting planets around stars are discovered mostly through photometric surveys. Unlike radial velocity surveys, photometric surveys do not tend to target slow rotators, inactive or metal-rich stars. Nevertheless, we suspect that observational biases could also impact transiting-planet hosts. Aims. This paper aims to evaluate how selection effects reflect on the evolutionary stage of both a limited sample of transiting-planet host stars (TPH) and a wider sample of planet-hosting stars detected through radial velocity analysis. Then, thanks to uniform derivation of stellar ages, a homogeneous comparison between exoplanet hosts and field star age distributions is developed. Methods. Stellar parameters have been computed through our custom-developed isochrone placement algorithm, according to Padova evolutionary models. The notable aspects of our algorithm include the treatment of element diffusion, activity checks in terms of log R HK and v sin i, and the evaluation of the stellar evolutionary speed in the Hertzsprung-Russel diagram in order to better constrain age. Working with TPH, the observational stellar mean density ρ allows us to compute stellar luminosity even if the distance is not available, by combining ρ with the spectroscopic log g. Results. The median value of the TPH ages is ∼5 Gyr. Even if this sample is not very large, however the result is very similar to what we found for the sample of spectroscopic hosts, whose modal and median values are [3, 3.5) Gyr and ∼4.8 Gyr, respectively. Thus, these stellar samples suffer almost the same selection effects. An analysis of MS stars of the solar neighbourhood belonging to the same spectral types bring to an age distribution similar to the previous ones and centered around solar age value. Therefore, the age of our Sun is consistent with the age distribution of solar neighbourhood stars with spectral types from late F to early K, regardless of whether they harbour planets or not. We considered the possibility that our selected samples are older than the average disc population.

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“…The host star WASP-2A is an R = 11.3 spectral type K1 dwarf, with an effective temperature of T eff = 5110 ± 60 inferred from optical and infrared colors (Maxted et al 2011), T eff = 5150 ± 80 K using photospheric fitting of spectroscopic data (Triaud et al 2010), and metallicity of [Fe/H] = 0.08 ± 0.08 (Triaud et al 2010). In our modeling we included photometric data from previous publications including Southworth et al (2010), who converted the timings from Cameron et al (2007), Charbonneau et al (2007), and Hrudková et al (2009) into the common time standard BJD(TDB) as outlined by Eastman et al (2010), as well as one transit epoch from Sada et al (2012).…”

Section: Apostle Programmentioning

confidence: 99%

Observations of the Wasp-2 System by the Apostle Program

Becker¹,

Kundurthy²,

Agol³

et al. 2013

ApJ

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We present transit observations of the WASP-2 exoplanet system by the Apache Point Survey of Transit Lightcurves of Exoplanets (APOSTLE) program. Model fitting to these data allows us to improve measurements of the hot-Jupiter exoplanet WASP-2b and its orbital parameters by a factor of ∼2 over prior studies; we do not find evidence for transit depth variations. We do find reduced χ 2 values greater than 1.0 in the observed minus computed transit times. A sinusoidal fit to the residuals yields a timing semi-amplitude of 32 s and a period of 389 days. However, random rearrangements of the data provide similar quality fits, and we cannot with certainty ascribe the timing variations to mutual exoplanet interactions. This inconclusive result is consistent with the lack of incontrovertible transit timing variations (TTVs) observed in other hot-Jupiter systems. This outcome emphasizes that unique recognition of TTVs requires dense sampling of the libration cycle (e.g., continuous observations from space-based platforms). However, even in systems observed with the Kepler spacecraft, there is a noted lack of transiting companions and TTVs in hot-Jupiter systems. This result is more meaningful, and indicates that hotJupiter systems, while they are easily observable from the ground, do not appear to be currently configured in a manner favorable to the detection of TTVs. The future of ground-based TTV studies may reside in resolving secular trends, and/or implementation at extreme quality observing sites to minimize atmospheric red noise.

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UBV(RI)C photometry of transiting planet hosting stars

Cited by 21 publications

References 47 publications

WASP-78b and WASP-79b: two highly-bloated hot Jupiter-mass exoplanets orbiting F-type stars in Eridanus

WASP-78b and WASP-79b: two highly-bloated hot Jupiter-mass exoplanets orbiting F-type stars in Eridanus

Age consistency between exoplanet hosts and field stars

Observations of the Wasp-2 System by the Apostle Program

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