J/A+A/574/A50 Chemical abundances of giants and subgiants (Jofre+, 2015)
Stellar parameters and chemical abundances of 223 evolved stars with and
without planets.
Jofre E., Petrucci R., Saffe C., Saker L., Artur de la Villarmois E.,
Chavero C., Gomez M., Mauas P.J.D.
<Astron. Astrophys., 574, A50-50 (2015)>
=2015A&A...574A..50J 2015A&A...574A..50J
ADC_Keywords: Stars, late-type ; Abundances ; Space velocities ; Spectroscopy
Keywords: techniques: spectroscopic - stars: abundances -
stars: fundamental parameters - planetary systems
Abstract:
We present fundamental stellar parameters, chemical abundances, and
rotational velocities for a sample of 86 evolved stars with planets
(56 giants; 30 subgiants), and for a control sample of 137 stars (101
giants; 36 subgiants) without planets. The analysis was based on both
high signal-to-noise and resolution echelle spectra. The main goals of
this work are i) to investigate chemical differences between evolved
stars that host planets and those of the control sample without
planets; ii) to explore potential differences between the properties
of the planets around giants and subgiants; and iii) to search for
possible correlations between these properties and the chemical
abundances of their host stars. Implications for the scenarios of
planet formation and evolution are also discussed. The fundamental
stellar parameters (Teff, logg, [Fe/H], ξt) were computed
homogeneously using the FUNDPAR code. The chemical abundances of 14
elements (Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Zn, and Ba)
were obtained using the MOOG code. Rotational velocities were derived
from the full width at half maximum of iron isolated lines. In
agreement with previous studies, we find that subgiants with planets
are, on average, more metal-rich than subgiants without planets by
∼0.16dex. The [Fe/H] distribution of giants with planets is centered
at slightly subsolar metallicities and there is no metallicity
enhancement relative to the [Fe/H] distribution of giants without
planets. Furthermore, contrary to recent results, we do not find any
clear difference between the metallicity distributions of stars with
and without planets for giants with M*>1.5M☉. With regard to
the other chemical elements, the analysis of the [X/Fe] distributions
shows differences between giants with and without planets for some
elements, particularly V, Co, and Ba. Subgiants with and without
planets exhibit similar behavior for most of the elements. On the
other hand, we find no evidence of rapid rotation among the giants
with planets or among the giants without planets. Finally, analyzing
the planet properties, some interesting trends might be emerging: i)
multi-planet systems around evolved stars show a slight metallicity
enhancement compared with single-planet systems; ii) planets with
a≲0.5AU orbit subgiants with [Fe/H]>0 and giants hosting planets with
a≲1AU have [Fe/H]<0; iii) higher-mass planets tend to orbit more
metal-poor giants with M*≤1.5M☉, whereas planets around
subgiants seem to follow the planet-mass metallicity trend observed on
dwarf hosts; iv) [X/Fe] ratios for Na, Si, and Al seem to increase
with the mass of planets around giants; v) planets orbiting giants
show lower orbital eccentricities than those orbiting subgiants and
dwarfs, suggesting a more efficient tidal circularization or the
result of the engulfment of close-in planets with larger
eccentricities.
Description:
For most of the objects in our sample we used publicly available high
signal-to-noise (S/N≳150) and high resolution spectra gathered with
four different instruments: HARPS (3.6m ESO telescope, La Silla,
Chile), FEROS (2.2m ESO/MPI telescope, La Silla, Chile), ELODIE (1.93m
telescope, OHP, France), and SOPHIE (1.93m telescope, OHP, France). In
addition we obtained high resolution and high signal-to-noise
(S/N≳150) spectra with the EBASIM spectrograph at the Jorge Sahade
2.15m telescope (CASLEO, San Juan, Argentina) for 7 stars in our
sample. Our EBASIM observations were taken between June 2012 and
August 2013.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 82 223 Fundamental stellar parameters and
rotation velocities
table5.dat 76 223 Photometric and evolutionary parameters
table6.dat 118 223 Derived abundances of Na, Mg, Al, Si, Ca, ScI,
ScII, TiI, and TiII
table7.dat 107 223 Derived abundances of V, CrI, CrII, Mn, Co,
Ni, Zn, and BaII
table9.dat 86 223 Galaxy population membership, radial velocities
and galactic space-velocity components
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Sample Stellar sample (G1)
7- 18 A12 --- Name Star name
19 A1 --- f_Name [*] indicates stars hosting multi-planet
systems
21- 24 I4 K Teff [4145/6391] Effective temperature
26- 27 I2 K e_Teff [9/61] rms uncertainty on Teff
29- 32 F4.2 [cm/s2] logg [1.06/4.28] Surface gravity
34- 37 F4.2 [cm/s2] e_logg [0.01/0.13] rms uncertainty on logg
39- 43 F5.2 [Sun] [Fe/H] [-0.69/0.38] Metallicity
45- 48 F4.2 [Sun] e_[Fe/H] [0.01/0.11] rms uncertainty on [Fe/H]
50- 53 F4.2 km/s vt [0.8/2.2] Microturbulent velocity
55- 58 F4.2 km/s e_vt [0.01/0.2] rms uncertainty on vt
60- 61 I2 --- NFeI [19/67] Number of line of FeI used
63- 64 I2 --- NFeII [5/12] Number of line of FeII used
66- 72 A7 --- Inst Instrument (1)
73- 77 F5.2 km/s vsini [0.3/13] Rotational velocity
79- 82 F4.2 km/s e_vsini [0.2/1.6] rms uncertainty on vsini
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Note (1): Instruments are:
HARPS : ESO-La Silla, 3.6m, R=120000
ELODIE : OHP (France), 1.93m, R=40000
FEROS : ESO-La Silla, 2.20mn R=48000
SOPHIE : OHP (France), 1.93m, R=75000
EBASIM : CASLEO (Argentina), 2.12m, R=30000
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Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Sample Stellar sample (G1)
7- 18 A12 --- Name Star name
19 A1 --- Rem [*n] Remark on physical parameters (2)
21- 24 F4.2 mag AV [0/1.1]?=- Absorption in V band
26- 29 F4.2 [Lsun] logL [0.2/2.9]?=- Luminosity
31- 34 F4.2 [Lsun] e_logL [0.03/0.5]? rms uncertainty on L
36- 40 F5.2 Gyr Age [0.2/12]?=- Age
42- 45 F4.2 Gyr e_Age ? rms uncertainty on Age
47- 50 F4.2 Msun Mass [0.7/3.4]?=- Mass
52- 55 F4.2 Msun e_Mass ? rms uncertainty on Mass
57- 61 F5.2 Rsun Rad [1.3/43]?=- Radius
63- 66 F4.2 Rsun e_Rad ? rms uncertainty on Rad
68- 71 F4.2 [cm/s2] loggt [1.2/4.2]?=- Trigonometric surface gravity
73- 76 F4.2 [cm/s2] e_loggt ? rms uncertainty on loggt
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Note (2): Notes as follows:
* = luminosity, mass and radius were taken from Gettel et al.
(2012ApJ...745...28G 2012ApJ...745...28G)
n = no data for this star
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Sample Stellar sample (G1)
7- 18 A12 --- Name Star name
21- 25 F5.2 [Sun] [Na/H] Abundance [Na/H]
27- 30 F4.2 [Sun] e_[Na/H] rms uncertainty on [Na/H]
32- 36 F5.2 [Sun] [Mg/H] Abundance [Mg/H]
38- 41 F4.2 [Sun] e_[Mg/H] rms uncertainty on [Mg/H]
43- 47 F5.2 [Sun] [Al/H] Abundance [Al/H]
49- 52 F4.2 [Sun] e_[Al/H] rms uncertainty on [Al/H]
54- 58 F5.2 [Sun] [Si/H] Abundance [Si/H]
60- 63 F4.2 [Sun] e_[Si/H] rms uncertainty on [Si/H]
65- 69 F5.2 [Sun] [Ca/H] Abundance [Ca/H]
71- 74 F4.2 [Sun] e_[Ca/H] rms uncertainty on [Ca/H]
76- 80 F5.2 [Sun] [ScI/H] Abundance [ScI/H]
82- 85 F4.2 [Sun] e_[ScI/H] rms uncertainty on [ScI/H]
87- 91 F5.2 [Sun] [ScII/H] ?=- Abundance [ScII/H]
93- 96 F4.2 [Sun] e_[ScII/H] ? rms uncertainty on [ScII/H]
98-102 F5.2 [Sun] [TiI/H] Abundance [TiI/H]
104-107 F4.2 [Sun] e_[TiI/H] rms uncertainty on [TiI/H]
109-113 F5.2 [Sun] [TiII/H] Abundance [TiII/H]
115-118 F4.2 [Sun] e_[TiII/H] rms uncertainty on [TiII/H]
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Sample Stellar sample (G1)
7- 18 A12 --- Name Star name
21- 25 F5.2 [Sun] [V/H] Abundance [V/H]
27- 30 F4.2 [Sun] e_[V/H] rms uncertainty on [V/H]
32- 36 F5.2 [Sun] [CrI/H] Abundance [CrI/H]
38- 41 F4.2 [Sun] e_[CrI/H] rms uncertainty on [CrI/H]
43- 47 F5.2 [Sun] [CrII/H] Abundance [CrII/H]
49- 52 F4.2 [Sun] e_[CrII/H] rms uncertainty on [CrII/H]
54- 58 F5.2 [Sun] [Mn/H] Abundance [Mn/H]
60- 63 F4.2 [Sun] e_[Mn/H] rms uncertainty on [Mn/H]
65- 69 F5.2 [Sun] [Co/H] Abundance [Co/H]
71- 74 F4.2 [Sun] e_[Co/H] rms uncertainty on [Co/H]
76- 80 F5.2 [Sun] [Ni/H] Abundance [Ni/H]
82- 85 F4.2 [Sun] e_[Ni/H] rms uncertainty on [Ni/H]
87- 91 F5.2 [Sun] [Zn/H] ?=- Abundance [Zn/H]
93- 96 F4.2 [Sun] e_[Zn/H] ? rms uncertainty on [Zn/H]
98-102 F5.2 [Sun] [BaII/H] Abundance [BaII/H]
104-107 F4.2 [Sun] e_[BaII/H] rms uncertainty on [BaII/H]
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Byte-by-byte Description of file: table9.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Sample Stellar sample (G1)
7- 18 A12 --- Name Star name
19 A1 --- Note [a] a indicates no galactic space-velocity (3)
21- 32 A12 --- Pop Population classification:
"Thin", "Thick", "Transition" or "unclassified"
34- 40 F7.2 km/s RV [-101/144] Radial velocity
42- 45 F4.2 km/s e_RV [0.01/0.9] rms uncertainty on RV
47- 53 F7.2 km/s Ulsr ?=- LSR U velocity
55- 59 F5.2 km/s e_Ulsr ? rms uncertainty on Ulsr
61- 67 F7.2 km/s Vlsr ?=- LSR V velocity
69- 73 F5.2 km/s e_Vlsr ? rms uncertainty on Vlsr
75- 80 F6.2 km/s Wlsr ?=- LSR W velocity
82- 86 F5.2 km/s e_Wlsr ? rms uncertainty on Wlsr
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Note (3): "a" indicates that no galactic space-velocity components were
derived due to the lack of astrometry and hence this star remains
unclassified
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Global notes:
Note (G1): Stellar sample classes as follows:
GWP = Giant stars with planets
GWOP = giant stars without planets
SGWP = Subgiant stars with planets
SGWOP = Subgiant stars without planets
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Acknowledgements: Emiliano Jofre, emiliano(at)oac.uncor.edu
(End) Emiliano Jofre [OAC, Argentina], Patricia Vannier [CDS] 27-Oct-2014