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J/A+A/533/A90       Radial velocity curves of HD 132563      (Desidera+, 2011)

A giant planet in the triple system HD 132563. Desidera S., Carolo E., Gratton R., Martinez Fiorenzano A.F., Endl M., Mesa D., Barbieri M., Bonavita M., Cecconi M., Claudi R.U., Cosentino R., Marzari F., Scuderi S. <Astron. Astrophys. 533, A90 (2011)> =2011A&A...533A..90D
ADC_Keywords: Stars, double and multiple ; Planets ; Radial velocities Keywords: stars: individual: HD 132563 - planetary systems - binaries: visual - binaries: spectroscopic - techniques: spectroscopic Abstract: As part of our radial velocity planet-search survey performed with SARG at TNG, we monitored the components of HD 132563 for ten years. It is a binary system formed by two rather similar solar type stars with a projected separation of 4.1arcsec, which corresponds to 400AU at the distance of 96 pc. The two components are moderately metal-poor and the age of the system is about 5Gyr. We detected RV variations of HD 132563B with period of 1544 days and semi-amplitude of 26m/s. From the star characteristics and line profile measurements, we infer their Keplerian origin. Therefore HD 132563B turns out to host a planet with a projected mass msini=1.49MJup at 2.6AU with a moderately eccentric orbit (e=0.22). The planet around HD 132563B is one of the few that are known in triple stellar systems, as we found that the primary HD 132563A is itself a spectroscopic binary with a period longer than 15 years and an eccentricity higher than 0.65. The spectroscopic component was not detected in adaptive-optics images taken with AdOpt@TNG, since it expected at a projected separation that was smaller than 0.2 arcsec at the time of our observations. A small excess in K band difference between the components with respect to the difference in V band is compatible with a companion of about 0.55M. A preliminary statistical analysis of the occurrence of planets in triple systems indicate a similar frequency of planets around the isolated component in a triple system, components of wide binaries and single stars. There is no significant iron abundance difference between the components. The lack of stars in binary systems and open clusters showing strong enhancements of iron abundance, comparable to the typical metallicity difference between stars with and without giant planets, agrees with the idea that accretion of planetary material producing iron abundance anomalies larger than 0.1dex is rare. Description: Relative radial velocity time series of HD132563A (Table 4) and HD132563B (Table 5) along with their internal errors. Objects: ----------------------------------------------------- RA (2000) DE Designation(s) ----------------------------------------------------- 14 58 21.5 +44 02 35 HD 132563 = IDS 14548+4427 ----------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 28 53 Relative radial velocity time serie of HD132563A table5.dat 28 47 Relative radial velocity time serie of HD132563B
Byte-by-byte Description of file: table4.dat table5.dat
Bytes Format Units Label Explanations
1- 12 F12.4 d HJD Heliocentric Julian Date 14- 20 F7.1 m/s RV Relative Radial Velocity 25- 28 F4.1 m/s e_RV Radial Velocity error
Acknowledgements: Silvano Desidera, silvano.desidera(at)oapd.inaf.it
(End) Silvano Desidera [INAF], Patricia Vannier [CDS] 19-Jul-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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