Giant planets around two intermediate-mass evolved stars and confirmation of the planetary nature of HIP 67851<i>c</i>

Jones, M. I.; Jenkins, James S.; Rojo, P.; Olivares, F.; Melo, C.

doi:10.1051/0004-6361/201525853

Cited by 19 publications

(20 citation statements)

References 51 publications

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“…brown-dwarf candidates, with orbital periods exceeding the total observational timespan of our survey (P 2200 d; see Bluhm et al 2016). We also note that in the case of HIP 67851 c (Jones et al 2015b), we used ESO archive data to fully cover its orbital period (P = 2132 d; a = 3.82 AU). Figure 6 shows a histogram of the planetary occurrence rate as a function of the stellar mass in our sample.…”

Section: Preliminary Statistical Results Of the Express Projectmentioning

confidence: 99%

“…On the other hand, for FEROS spectra, we used the simultaneous calibration method (Baranne et al 1996) to extract the stellar radial velocities, reaching a typical precision of ∼5 m s −1 . Details on the data reduction and RV calculations have been given in several papers (e.g., Jones et al 2013Jones et al , 2014Jones et al , 2015aJones et al , 2015b. In addition, we present complementary observations from the Pan-Pacific Planet Search (PPPS; Wittenmyer et al 2011).…”

Section: Observations and Rv Calculationmentioning

confidence: 99%

“…The stellar mass and radius was derived by comparing the position of the star in the HR diagram with the evolutionary tracks from Salasnich et al (2000). A detailed description of the method is presented in Jones et al (2011Jones et al ( , 2015b. Table A.1 and are shown in Fig.…”

Section: Observations and Rv Calculationmentioning

confidence: 99%

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Four new planets around giant stars and the mass-metallicity correlation of planet-hosting stars

Jones

Jenkins

Brahm

et al. 2016

A&A

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Context. Exoplanet searches have revealed interesting correlations between the stellar properties and the occurrence rate of planets. In particular, different independent surveys have demonstrated that giant planets are preferentially found around metal-rich stars and that their fraction increases with the stellar mass. Aims. During the past six years we have conducted a radial velocity follow-up program of 166 giant stars to detect substellar companions and to characterize their orbital properties. Using this information, we aim to study the role of the stellar evolution in the orbital parameters of the companions and to unveil possible correlations between the stellar properties and the occurrence rate of giant planets. Methods. We took multi-epoch spectra using FEROS and CHIRON for all of our targets, from which we computed precision radial velocities and derived atmospheric and physical parameters. Additionally, velocities computed from UCLES spectra are presented here. By studying the periodic radial velocity signals, we detected the presence of several substellar companions. Results. We present four new planetary systems around the giant stars HIP 8541, HIP 74890, HIP 84056, and HIP 95124. Additionally, we study the correlation between the occurrence rate of giant planets with the stellar mass and metallicity of our targets. We find that giant planets are more frequent around metal-rich stars, reaching a peak in the detection of f = 16.7 +15.5 −5.9 % around stars with [Fe/H] ∼ 0.35 dex. Similarly, we observe a positive correlation of the planet occurrence rate with the stellar mass, between M ∼ 1.0 and 2.1 M , with a maximum of f = 13.0Conclusions. We conclude that giant planets are preferentially formed around metal-rich stars. In addition, we conclude that they are more efficiently formed around more massive stars, in the stellar mass range of ∼1.0-2.1 M . These observational results confirm previous findings for solar-type and post-MS hosting stars, and provide further support to the core-accretion formation model.

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Section: Preliminary Statistical Results Of the Express Projectmentioning

confidence: 99%

Section: Observations and Rv Calculationmentioning

confidence: 99%

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Four new planets around giant stars and the mass-metallicity correlation of planet-hosting stars

Jones

Jenkins

Brahm

et al. 2016

A&A

Self Cite

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“…The planetary companion was presented in Jones et al (2015) as an exoplanet around an intermediate-mass evolved star. The stellar parameters were obtained from the analysis by Jones et al (2011) using the same method as presented here, but with a different line list, which might lead to some disagreements.…”

Section: Hip 107773mentioning

confidence: 99%

SWEET-Cat update and FASMA

Andreasen¹,

Sousa²,

Tsantaki³

et al. 2017

A&A

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Context. Thanks to the importance that the star-planet relation has to our understanding of the planet formation process, the precise determination of stellar parameters for the ever increasing number of discovered extrasolar planets is of great relevance. Furthermore, precise stellar parameters are needed to fully characterize the planet properties. It is thus important to continue the efforts to determine, in the most uniform way possible, the parameters for stars with planets as new discoveries are announced. Aims. In this paper we present new precise atmospheric parameters for a sample of 50 stars with planets. The results are presented in the catalogue: SWEET-Cat. Methods. Stellar atmospheric parameters and masses for the 50 stars were derived assuming local thermodynamic equilibrium and using high-resolution and high signal-to-noise spectra. The methodology used is based on the measurement of equivalent widths with ARES2 for a list of iron lines. The line abundances were derived using MOOG. We then used the curve of growth analysis to determine the parameters. We implemented a new minimization procedure which significantly improves the computational time.Results. The stellar parameters for the 50 stars are presented and compared with previously determined literature values. For SWEETCat, we compile values for the effective temperature, surface gravity, metallicity, and stellar mass for almost all the planet host stars listed in the Extrasolar Planets Encyclopaedia. This data will be updated on a continuous basis. The data can be used for statistical studies of the star-planet correlation, and for the derivation of consistent properties for known planets.

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“…About 3500 exoplanets have been discovered with various methods so far (The NASA Exoplanet Archive; Akeson et al (2017)), of which about 640 have been found with the RV technique. While most of the known exoplanets (∼75%) orbit around G, K-type dwarfs, a small fraction (∼4%) of these exoplanets have been found around evolved intermediate-mass (1.3 − 5M ⊙ ) stars (e.g., Niedzielski et al (2016); Ortiz et al (2016); Giguere et al (2015); Jones et al (2015); Lee et al (2014); Nowak et al (2013); Mitchell et al (2013); Sato et al (2010Sato et al ( , 2013; Omiya et al (2012); Wang et al (2012); Johnson et al (2011);Wittenmyer et al (2011)). In spite of about 130 planets discovered around G-K giant stars, only few of these planets (∼ 20) are close to the mass of Jupiter.…”

Section: Introductionmentioning

confidence: 99%

A Jupiter-mass planet around the K0 giant HD 208897

Yılmaz

Sato

Bikmaev

et al. 2017

A&A

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For over 10 years, we have carried out a precise radial velocity (RV) survey to find substellar companions around evolved G,K-type stars to extend our knowledge of planet formation and evolution. We performed high precision RV measurements for the giant star HD 208897 using an iodine (I 2 ) absorption cell. The measurements were made at TÜBİTAK National Observatory (TUG; RTT150) and Okayama Astrophysical Observatory (OAO). For the origin of the periodic variation seen in the RV data of the star, we adopted a Keplerian motion caused by an unseen companion. We found that the star hosts a planet with a minimum mass of m 2 sini = 1.40M J , which is relatively low compared to those of known planets orbiting evolved intermediate-mass stars. The planet is in a nearly circular orbit with a period of P = 353 days at about 1 AU distance from the host star. The star is metal rich and located at the early phase of ascent along the red giant branch. The photometric observations of the star at Ankara University Kreiken Observatory (AUKR) and the HIPPARCOS photometry show no sign of variation with periods associated with the RV variation. Neither bisector velocity analysis nor analysis of the Ca II and Hα lines shows any correlation with the RV measurements.

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Giant planets around two intermediate-mass evolved stars and confirmation of the planetary nature of HIP 67851c

Cited by 19 publications

References 51 publications

Four new planets around giant stars and the mass-metallicity correlation of planet-hosting stars

Four new planets around giant stars and the mass-metallicity correlation of planet-hosting stars

SWEET-Cat update and FASMA

A Jupiter-mass planet around the K0 giant HD 208897

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