J/A+A/701/A153 Chemical composition of planetary hosts II (Sharma+, 2025)
Chemical composition of planetary hosts:
II. Abundances of neutron-capture elements.
Sharma A., Stonkute E., Drazdauskas A., Minkeviciute R., Mikolaitis S.,
Tautvaisiene G., Jonauskaite U.
<Astron. Astrophys. 701, A153 (2025)>
=2025A&A...701A.153S 2025A&A...701A.153S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Abundances ; Optical
Keywords: techniques: spectroscopic - stars: abundances - stars: atmospheres -
planetary systems
Abstract:
We present neutron-capture element abundances for a homogeneous sample
of 160 FGK-type planet-hosting stars (32 of them are multiplanetary
systems). These stars host a total of 175 high-mass planets and 47
Neptunian and Super-Earth planets. Spectra were obtained with the
Vilnius University Echelle Spectrograph (VUES) associated with a 1.65m
telescope installed at Moletai Astronomical Observatory. The
analysed elements include Sr, Y, Zr, Ba, La, Ce, Pr, Nd, and Eu.
Abundances were derived using synthetic spectral fitting with the
TURBOSPECTRUM code and MARCS model atmospheres under LTE, with NLTE
corrections applied for Sr, Y, Ba and Eu. The dataset includes stellar
parameters, and individual elemental abundances ([El/H]).
We investigate the trends of [El/Fe] with [Fe/H] and planet mass, and
examine condensation temperature (Tcond) trends
({DELTA}[El/H]-Tcond> slopes) for potential star-planet chemical
signatures. The results show that most neutron-capture elements trace
Galactic chemical evolution, but [Zr/Fe], [La/Fe], and [Ce/Fe] are
enhanced in stars with planets compared to reference stars at a given
[Fe/H]. Positive correlations between [El/Fe] and planet mass are
observed towards higher-mass planets for most elements excluding
strontium, yttrium, and barium, which exhibit insignificant
correlations across all subsamples. The {DELTA}[El/H]-Tcond slopes
suggest a possible enrichment of refractory elements in planet-hosting
stars, especially in younger and less metal-rich systems. While strong
correlations between {DELTA}[El/H]-Tcond slopes and stellar or
planetary parameters are not observed, the data suggest some notable
trends. Older dwarf stars hosting multiple planets tend to exhibit
smaller or even negative {DELTA}[El/H]-Tcond slopes, whereas younger
dwarfs show larger positive slopes, indicating a possible
age-dependent chemical signature. Additionally, we find that
multiplanetary systems are more frequently associated with metal-rich
stars. This dataset supports ongoing efforts to understand the
chemical signatures associated with planet formation.
Description:
The table includes stellar parameters and derived elemental abundances
for a sample of 160 FGK-type stars hosting planets. Spectra were
obtained using 1.65m telescope and VUES spectrograph at the Moletai
Astronomical Observatory of Institute of Theoretical Physics and
Astronomy, Vilnius University. This spectrograph has a wavelength
coverage from 400 to 900nm and R∼36000, ∼51000, and ∼68000 resolution
modes. We used the R∼68000 mode for this work. Stellar parameters
(Teff, logg, [Fe/H], microturbulence) are derived from FeI and FeII
line analyses. Abundances are provided for Sr, Y, Zr, Ba, La, Ce, Pr,
Nd, and Eu with associated line-to-line uncertainties. NLTE
corrections are included for Sr, Y, Ba, and Eu.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 161 160 Stellar physical and chemical properties
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See also:
J/A+A/691/A160 : Chemical composition of planetary hosts (Sharma+, 2024)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- TYC Tycho-2 catalogue identification
13- 16 I4 K Teff Effective temperature
18- 20 I3 K e_Teff Uncertainty in effective temperature
22- 25 F4.2 [cm/s2] logg Stellar surface gravity
27- 30 F4.2 [cm/s2] e_logg Uncertainty in stellar surface gravity
32- 36 F5.2 [-] [Fe/H] Metallicity
38- 41 F4.2 [-] e_[Fe/H] Uncertainty in metallicity
43- 46 F4.2 km/s Vt Microturbulence velocity
48- 51 F4.2 km/s e_Vt Uncertainty in microturbulence velocity
53- 57 F5.2 [-] [Sr/H] ? Strontium abundance
59- 62 F4.2 [-] e_[Sr/H] ? Uncertainty in Sr abundance
64- 68 F5.2 [-] [Y/H] ? Yttrium abundance
70- 73 F4.2 [-] e_[Y/H] ? Uncertainty in Y abundance
75- 79 F5.2 [-] [ZrI/H] ? Zirconium (neutral) abundance
81- 84 F4.2 [-] e_[ZrI/H] ? Uncertainty in ZrI abundance
86- 90 F5.2 [-] [ZrII/H] ? Zirconium (ionised) abundance
92- 95 F4.2 [-] e_[ZrII/H] ? Uncertainty in ZrII abundance
97-101 F5.2 [-] [Ba/H] ? Barium abundance
103-106 F4.2 [-] e_[Ba/H] ? Uncertainty in Ba abundance
108-112 F5.2 [-] [La/H] ? Lanthanum abundance
114-117 F4.2 [-] e_[La/H] ? Uncertainty in La abundance
119-123 F5.2 [-] [Ce/H] ? Cerium abundance
125-128 F4.2 [-] e_[Ce/H] ? Uncertainty in Ce abundance
130-134 F5.2 [-] [Pr/H] ? Praseodymium abundance
136-139 F4.2 [-] e_[Pr/H] ? Uncertainty in Pr abundance
141-145 F5.2 [-] [Nd/H] ? Neodymium abundance
147-150 F4.2 [-] e_[Nd/H] ? Uncertainty in Nd abundance
152-156 F5.2 [-] [Eu/H] ? Europium abundance
158-161 F4.2 [-] e_[Eu/H] ? Uncertainty in Eu abundance
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History:
From Ashutosh Sharma, ashutosh.sharma(at)ff.stud.vu.lt
Acknowledgements:
We thank the anonymous referee for their helpful and constructive
suggestions. E.S., A.D., R.M., S.M. and G.T. acknowledge funding from
the Research Council of Lithuania (LMTLT, grant No. P-MIP-23-24). This
research has made use of the NASA Exoplanet Archive, which is operated
by the California Institute of Technology, under contract with the
National Aeronautics and Space Administration under the Exoplanet
Exploration Programme. We also acknowledge the use of the SIMBAD
database, operated at CDS, Strasbourg, France. U.J. acknowledge
funding from the Research Council of Lithuania (LMTLT, grant No.
S-LL-24-1). Additionally, we appreciate the Vilnius University's
Moletai Astronomical Observatory for granting us observation time for
this project. The observing time was partially funded by the
Europlanet Telescope Network programme of the Europlanet 2024 Research
Infrastructure project. Europlanet 2024 RI has received funding from
the European Union's Horizon 2020 research and innovation programme
under grant agreement No 871149.
References:
Sharma et al., Paper I 2024A&A...691A.160S 2024A&A...691A.160S, Cat. J/A+A/691/A160
(End) Ashutosh Sharma [ITPA, VU], Patricia Vannier [CDS] 01-Aug-2025