Late-type members of young stellar kinematic groups - I. Single stars

Montes, D.; López‐Santiago, J.; Gálvez, M. C.; Fernández-Figueroa, M. J.; Castro, E. de; Cornide, M.

doi:10.1046/j.1365-8711.2001.04781.x

Cited by 408 publications

(540 citation statements)

References 87 publications

(187 reference statements)

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“…This is shown in Fig. 7, where we show the location of the stars from Table 9 in the (U, V) and (V, W) planes, together with the location of the mean space velocities for several nearby young moving groups (ages 20−600 Myr; Montes et al 2001).…”

Section: Space Velocitiesmentioning

confidence: 96%

Proper motions of young stars in Chamaeleon

Martí

Jiménez-Esteban

Bayo

et al. 2013

A&A

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Context. The study of the motion of the members of a given open cluster or stellar association provides key information about their formation and early evolution. The Chamaeleon cloud complex constitutes one of the closest and best studied low-mass star-forming regions in the Galaxy. Aims. We want to provide further evidence of the origin of the proposed stellar members of Chamaeleon and to identify interlopers from the foreground Cha and η Cha associations. Methods. We have compiled lists of spectroscopically confirmed members of Chamaeleon I and II, Cha and η Cha, and of background objects in the same line of sight. Using Virtual Observatory tools, we cross-match these lists with the UCAC3 catalogue to get the proper motions of the objects. In the vector point diagram, we identify the different moving groups, and use this information to study the membership of proposed candidate members of the associations from the literature. For those objects with available radial velocities, we compute their Galactic space velocities. We look for correlations between the known properties of the objects and their proper motions. Results. The members of the dark clouds exhibit clearly different proper motions from those of the foreground associations and of the background stars. The data suggest that Chamaeleon II could have different dynamical properties from Chamaeleon I. Although the two foreground clusters and η Chamaeleontis constitute two different proper motion groups, they have similar spatial motions, which are different from the spatial motion of Chamaeleon I. On the other hand, the space motions of the Chamaeleon II stars look more similar to those of the foreground clusters than to the Chamaeleon I stars, but the numbers are low. We find no correlations between the proper motions and the properties of the objects in either of the clouds. Conclusions. On the basis of proper motion, Chamaeleon I and II constitute two physical entities unrelated to the foreground and η Chamaeleontis clusters, but with the available data it is unclear to what extent the stellar populations in both clouds are physically connected to each other.

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Section: Space Velocitiesmentioning

confidence: 96%

Proper motions of young stars in Chamaeleon

Martí

Jiménez-Esteban

Bayo

et al. 2013

A&A

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“…The last star in our sample is HD 70573, a young lithium bearing star classified as a member of the Local Association (Pleiades moving group) by Montes et al (2001). The age is therefore estimated to be between 78-125 Myr (only 3%-6% the age of the Sun, where moving groups are thought to be associations of young stars, see Murgas et al 2013).…”

Section: Hd 70573mentioning

confidence: 99%

RAFT – I. Discovery of new planetary candidates and updated orbits from archival FEROS spectra

Soto

Jenkins

Jones

2015

Monthly Notices of the Royal Astronomical Society

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A recent reanalysis of archival data has lead several authors to arrive at strikingly different conclusions for a number of planet-hosting candidate stars. In particular, some radial velocities measured using FEROS spectra have been shown to be inaccurate, throwing some doubt on the validity of a number of planet detections. Motivated by these results, we have begun the Reanalysis of Archival FEROS specTra (RAFT) program and here we discuss the first results from this work. We have reanalyzed FEROS data for the stars HD 11977, HD 47536, HD 70573, HD 110014 and HD 122430, all of which are claimed to have at least one planetary companion. We have reduced the raw data and computed the radial velocity variations of these stars, achieving a long-term precision of ∼ 10 m s −1 on the known stable star τ Ceti, and in good agreement with the residuals to our fits. We confirm the existence of planets around HD 11977, HD 47536 and HD 110014, but with different orbital parameters than those previously published. In addition, we found no evidence of the second planet candidate around HD 47536, nor any companions orbiting HD 122430 and HD 70573. Finally, we report the discovery of a second planet around HD 110014, with a minimum mass of 3.1 M Jup and a orbital period of 130 days. Analysis of activity indicators allow us to confirm the reality of our results and also to measure the impact of magnetic activity on our radial velocity measurements. These results confirm that very metal-poor stars down to [Fe/H]∼-0.7 dex, can indeed form giant planets given the right conditions.

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“…4. HR 8734 (= HD 217107) is a G8IV double star at 19.72 pc (Montes et al 2001;van Leeuwen 2007) made of the CDM J22583−0224A and CDM J22583−0224B components (Høg et al 2000;Fabricius et al 2002) with a separation of ∼10 au and orbited by two Jupiter-mass planets (Wright et al 2009). 5.…”

Section: Known Planet-host Star Binaries In Vhsmentioning

confidence: 99%

Binary frequency of planet-host stars at wide separations

Lodieu

Pérez‐Garrido

Béjar

et al. 2014

A&A

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Aims. The aim of the project is to improve our knowledge on the multiplicity of planet-host stars at wide physical separations. Methods. We cross-matched approximately 6200 square degree area of the southern sky imaged by the Visible Infrared Survey Telescope for Astronomy (VISTA) Hemisphere Survey (VHS) with the Two Micron All Sky Survey (2MASS) to look for wide common proper motion companions to known planet-host stars. We complemented our astrometric search with photometric criteria. Results. We confirmed spectroscopically the co-moving nature of seven sources out of 16 companion candidates and discarded eight, while the remaining one stays as a candidate. Among these new wide companions to planet-host stars, we discovered a T4.5 dwarf companion at 6.3 arcmin (∼9000 au) from HIP 70849, a K7V star which hosts a 9 Jupiter mass planet with an eccentric orbit. We also report two new stellar M dwarf companions to one G and one metal-rich K star. We infer stellar and substellar binary frequencies for our complete sample of 37 targets of 5.4 ± 3.8% and 2.7 ± 2.7% (1σ confidence level), respectively, for projected physical separations larger than ∼60-160 au assuming the range of distances of planet-host stars (24-75 pc). These values are comparable to the frequencies of non planet-host stars. We find that the period-eccentricity trend holds with a lack of multiple systems with planets at large eccentricities (e > 0.2) for periods less than 40 days. However, the lack of planets more massive than 2.5 Jupiter masses and short periods (<40 days) orbiting single stars is not so obvious due to recent discoveries by ground-based transit surveys and space missions.

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Late-type members of young stellar kinematic groups - I. Single stars

Cited by 408 publications

References 87 publications

Proper motions of young stars in Chamaeleon

Proper motions of young stars in Chamaeleon

RAFT – I. Discovery of new planetary candidates and updated orbits from archival FEROS spectra

Binary frequency of planet-host stars at wide separations

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