J/A+A/554/A84 Abundances of evolved stars (Maldonado+, 2013)
The metallicity signature of evolved stars with planets.
Maldonado J., Villaver E., Eiroa C.
<Astron. Astrophys. 554, A84 (2013)>
=2013A&A...554A..84M 2013A&A...554A..84M
ADC_Keywords: Stars, late-type ; Abundances, [Fe/H] ; Spectroscopy
Keywords: techniques: spectroscopic - stars: abundances - stars: late-type -
planetary systems
Abstract:
Currently, the core accretion model has its strongest observational
evidence on the chemical signature of mostly main sequence stars with
planets.
We aim to test whether the well-established correlation between the
metallicity of the star and the presence of giant planets found for
main sequence stars still holds for the evolved and generally more
massive giant and subgiant stars. Although several attempts have been
made so far, the results are not conclusive since they are based on
small or inhomogeneous samples.
We determine in a homogeneous way the metallicity and individual
abundances of a large sample of evolved stars, with and without known
planetary companions, and discuss their metallicity distribution and
trends. Our methodology is based on the analysis of high-resolution
echelle spectra (R∼67000) from 2-3 meter class telescopes. It includes
the calculation of the fundamental stellar parameters (effective
temperature, surface gravity, microturbulent velocity, and
metallicity) by applying iron ionisation and excitation equilibrium
conditions to several isolated FeI and FeII lines, as well as,
calculating individual abundances of different elements such as Na,
Mg, Si, Ca, Ti, Cr, Co, or Ni.
Description:
File table2 lists the stars with homogeneous spectroscopic parameters
(effective temperature, surface gravity, microturbulence, and
metallicity) obtained in this work.
File table3 lists values of visual extinction, luminosity, photometric
temperature, evolutionary surface gravity, age, mass, and radius.
File table5 lists the derived abundances of Na, Mg, Al, Si, Ca, TiI,
TiII, V, CrI, CrII, Mn, Co, Ni, and Zn for those stars observed in
this work.
File table7 gives radial velocities and Galactic spatial-velocity
components with respect to the local standard of rest (LSR). The
sample of stars classified as "subgiant without planets" is expanded
with stars from the literature. Results for these stars are also
included in files table3 and table5. For these stars, the radial
velocities shown in table7 have been taken from Kharchenko et al.
2007 (Cat. III/254).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 103 142 Spectroscopic parameters for the stars measured
in this work
table3.dat 97 192 Photometric and evolutionary parameters
table5.dat 186 142 Derived abundances for the stars analysed in
this work
table7.dat 83 192 Radial velocities and Galactic spatial-velocity
components
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See also:
III/254 : 2nd Cat. of Radial Vel. with Astrometric Data (Kharchenko+, 2007)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HIP ? Hipparcos number
8- 13 I6 --- HD ? HD number
15- 28 A14 --- Name Star name (1)
30- 33 I4 K Teff Effective temperature
35- 36 I2 K e_Teff Uncertainty on effective temperature
38- 41 F4.2 [cm/s2] logg Surface gravity
43- 46 F4.2 [cm/s2] e_logg Uncertainty on surface gravity
48- 51 F4.2 km/s Vt Microturbulence
53- 56 F4.2 km/s e_Vt Uncertainty on microturbulence
58- 62 F5.2 [Sun] [Fe/H] Metallicity
64- 67 F4.2 [Sun] e_[Fe/H] Uncertainty on metallicity
69- 72 F4.2 [-] A(FeI) Mean iron abundance derived from FeI lines
74- 77 F4.2 [-] e_A(FeI) Uncertainty on A(FeI)
79- 81 I3 --- n(FeI) Number of FeI lines used
83- 86 F4.2 [-] A(FeII) Mean iron abundance derived from FeII lines
88- 91 F4.2 [-] e_A(FeII) Uncertainty on A(FeII)
93- 94 I2 --- n(FeII) Number of FeII lines used
96 I1 --- Spg [1/2] Spectrograph: 1=MERCATOR/HERMES,
2=NOT/FIES
98-103 A6 --- Sample Stellar sample (G1)
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Note (1): other name only for those stars without HIP or HD number,
else HIP or HD name.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Star name
16- 19 F4.2 mag Av Visual extinction
21- 24 F4.2 mag e_Av Uncertainty on Av
26- 30 F5.2 [Lsun] log(L) Stellar luminosity (log(L/L☉))
32- 35 F4.2 [Lsun] e_log(L) Uncertainty on log(L)
37- 40 I4 K Te.ph ? Photometric effective temperature
42- 44 I3 K e_Te.ph ? Uncertainty on Te.phot
46- 49 F4.2 [cm/s2] logge Evolutionary surface gravity
51- 54 F4.2 [cm/s2] e_logge Uncertainty on logge
56- 60 F5.2 Gyr Age Stellar age
62- 65 F4.2 Gyr e_Age Uncertainty on age
67- 70 F4.2 [Msun] Mass Stellar mass
72- 75 F4.2 [Msun] e_Mass Uncertainty on Mass
77- 81 F5.2 [Rsun] Rad Stellar radius
83- 86 F4.2 [Rsun] e_Rad Uncertainty on Rad
88- 97 A10 --- Sample Stellar sample (G1)
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Star name
16- 20 F5.2 [Sun] [Na/H] Na abundance
22- 25 F4.2 [Sun] e_[Na/H] Uncertainty on Na abundance
27- 31 F5.2 [Sun] [Mg/H] Mg abundance
33- 36 F4.2 [Sun] e_[Mg/H] Uncertainty on Mg abundance
38- 42 F5.2 [Sun] [Al/H] Al abundance
44- 47 F4.2 [Sun] e_[Al/H] Uncertainty on Al abundance
49- 53 F5.2 [Sun] [Si/H] Si abundance
55- 58 F4.2 [Sun] e_[Si/H] Uncertainty on Si abundance
60- 64 F5.2 [Sun] [Ca/H] Ca abundance
66- 69 F4.2 [Sun] e_[Ca/H] Uncertainty on Ca abundance
71- 75 F5.2 [Sun] [Sc/H] Sc abundance
77- 80 F4.2 [Sun] e_[Sc/H] Uncertainty on Sc abundance
82- 86 F5.2 [Sun] [TiI/H] TiI abundance
88- 91 F4.2 [Sun] e_[TiI/H] Uncertainty on TiI abundance
93- 97 F5.2 [Sun] [TiII/H] TiII abundance
99-102 F4.2 [Sun] e_[TiII/H] Uncertainty on TiII abundance
104-108 F5.2 [Sun] [V/H] V abundance
110-113 F4.2 [Sun] e_[V/H] Uncertainty on V abundance
115-119 F5.2 [Sun] [CrI/H] CrI abundance
121-124 F4.2 [Sun] e_[CrI/H] Uncertainty on CrI abundance
126-130 F5.2 [Sun] [CrII/H] CrII abundance
132-135 F4.2 [Sun] e_[CrII/H] Uncertainty on CrII abundance
137-141 F5.2 [Sun] [Mn/H] Mn abundance
143-146 F4.2 [Sun] e_[Mn/H] Uncertainty on Mn abundance
148-152 F5.2 [Sun] [Co/H] Co abundance
154-157 F4.2 [Sun] e_[Co/H] Uncertainty on Co abundance
159-163 F5.2 [Sun] [Ni/H] Ni abundance
165-168 F4.2 [Sun] e_[Ni/H] Uncertainty on Ni abundance
170-174 F5.2 [Sun] [Zn/H] Zn abundance
176-179 F4.2 [Sun] e_[Zn/H] Uncertainty on Zn abundance
181-186 A6 --- Sample Stellar sample (G1)
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Star name
16- 21 F6.2 km/s RV Radial velocity
23- 26 F4.2 km/s e_RV ? Uncertainty on RV
28- 34 F7.2 km/s U(LSR) Galactic-spatial velocity component U
with respect to the LSR
36- 41 F6.2 km/s e_U(LSR) ? Uncertainty on U(LSR)
43- 48 F6.2 km/s V(LSR) Galactic-spatial velocity component V
with respect to the LSR
50- 55 F6.2 km/s e_V(LSR) ? Uncertainty on V(LSR)
57- 62 F6.2 km/s W(LSR) Galactic-spatial velocity component W
with respect to the LSR
64- 69 F6.2 km/s e_W(LSR) ? Uncertainty on W(LSR)
71- 72 A2 --- Pop Population classification: D=Thin Disk,
TD=Thick Disk, R=transition
74- 83 A10 --- Sample Stellar sample (G1)
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Global notes:
Note (G1): Stellar sample classes as follows:
GWPs = Giants with planets
GWOPs = Giants without planets
SGWPs = Subgiants with planets
SGWOPs = Subgiants without planets
SGWOPs(tw) = Subgiants without planets from this work
SGWOPs(l) = Subgiants without planets from the literature
LMSWPs = Late main-sequence with planets
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Acknowledgements:
Jesus Maldonado, jesus.maldonado(at)uam.es
(End) Jesus Maldonado [UAM, Spain], Patricia Vannier [CDS] 17-Apr-2013