The N2K Consortium. III. Short‐Period Planets Orbiting HD 149143 and HD 109749

Fischer, Debra A.; Laughlin, Gregory; Marcy, Geoffrey W.; Butler, R. Paul; Vogt, Steven S.; Johnson, John Asher; Henry, Gregory W.; McCarthy, C.; Ammons, Mark; Robinson, Sarah E.; Strader, Jay; Valenti, Jeff A.; McCullough, P. R.; Charbonneau, David; Haislip, J.; Knutson, Heather A.; Reichart, D.; McGee, Padric; Monard, B.; Wright, Jason T.; Ida, Shigeru; Sato, B.; Minniti, D.

doi:10.1086/498557

Cited by 53 publications

(10 citation statements)

References 41 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The Hipparcos magnitude of the secondary transformed to the standard system following Bessell (2000) yields V = 10.76, about 2.5 mag fainter than the primary (V = 8.09, Fischer et al 2006; see Table A.2). Table A.3 shows the relative astrometry for the two components.…”

Section: A2 Hd 109749mentioning

confidence: 98%

Properties of planets in binary systems

Desidera¹,

Barbieri

2006

A&A

214

248

View full text Add to dashboard Cite

Aims. The statistical properties of planets in binaries were investigated. Any difference to planets orbiting single stars can shed light on the formation and evolution of planetary systems. As planets were found around components of binaries with very different separation and mass ratio, it is particularly important to study the characteristics of planets as a function of the effective gravitational influence of the companion. Methods. A compilation of planets in binary systems was made; a search for companions orbiting stars recently shown to host planets was performed, resulting in the addition of two further binary planet hosts (HD 20782 and HD 109749). The probable original properties of the three binary planet hosts with white dwarfs companions were also investigated. Using this updated sample of planets in binaries we performed a statistical analysis of the distributions of planet mass, period, and eccentricity, fraction of multiplanet systems, and stellar metallicity for planets orbiting components of tight and wide binaries and single stars. Results. The only highly significant difference revealed by our analysis concerns the mass distribution of short-period planets. Massive planets in short period orbits are found in most cases around the components of rather tight binaries. The properties of exoplanets orbiting the components of wide binaries are compatible with those of planets orbiting single stars, except for a possible greater abundance of high-eccentricity planets. The previously suggested lack of massive planets with P > 100 days in binaries is not confirmed. Conclusions. We conclude that the presence of a stellar companion with separation smaller than 100-300 AU is able to modify the formation and/or migration and/or the dynamical evolution history of giant planets while wide companions play a more limited role.

show abstract

Section: A2 Hd 109749mentioning

confidence: 98%

Properties of planets in binary systems

Desidera¹,

Barbieri

2006

A&A

214

248

View full text Add to dashboard Cite

show abstract

“…HD 109749 is a double G3IV star at 59 pc (van Leeuwen 2007) with a physical separation of approximately 750 au. The system harbours a 0.28 M Jup planet with a period of 5.24 days (Nordström et al 2004;Fischer et al 2006). 2.…”

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

View full text Add to dashboard Cite

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.

show abstract

“…Of the 290 planets, only 24 (8.3%) were published with less than one orbital cycle of data. The outlier with an unusually large fractional error in period (σ P /P =17.2%) is HD 149143 (Fischer et al 2006). That planet was first published with only 17 observations, which may account for the large uncertainty in its 4-day period.…”

Section: False Positives and False Negativesmentioning

confidence: 99%

On the Frequency of Jupiter Analogs

Wittenmyer¹,

Tinney²,

O'Toole

et al. 2011

ApJ

View full text Add to dashboard Cite

The Anglo-Australian Planet Search has now accumulated 12 years of radialvelocity data with long-term instrumental precision better than 3 m s −1 . In this paper, we expand on earlier simulation work, to probe the frequency of nearcircular, long-period gas-giant planets residing at orbital distances of 3-6 AUthe so-called "Jupiter analogs." We present the first comprehensive analysis of the frequency of these objects based on radial-velocity data. We find that 3.3% of stars in our sample host Jupiter analogs; detailed, star-by-star simulations show that no more than 37% of stars host a giant planet between 3-6 AU.

show abstract

The N2K Consortium. III. Short‐Period Planets Orbiting HD 149143 and HD 109749

Cited by 53 publications

References 41 publications

Properties of planets in binary systems

Properties of planets in binary systems

Binary frequency of planet-host stars at wide separations

On the Frequency of Jupiter Analogs

Contact Info

Product

Resources

About