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 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:
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RA (2000) DE Designation(s)
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14 58 21.5 +44 02 35 HD 132563 = IDS 14548+4427
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File Summary:
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FileName Lrecl Records Explanations
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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
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Byte-by-byte Description of file: table4.dat table5.dat
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Bytes Format Units Label Explanations
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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
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Acknowledgements:
Silvano Desidera, silvano.desidera(at)oapd.inaf.it
(End) Silvano Desidera [INAF], Patricia Vannier [CDS] 19-Jul-2011