J/MNRAS/468/4151 Spectroscopic properties for 107 stars (Ivanyuk+, 2017)
The metal-rich abundance pattern - spectroscopic properties and abundances
for 107 main-sequence stars.
Ivanyuk O.M., Jenkins J.S., Pavlenko Y.V., Jones H.R.A., Pinfield D.J.
<Mon. Not. R. Astron. Soc., 468, 4151-4169 (2017)>
=2017MNRAS.468.4151I 2017MNRAS.468.4151I (SIMBAD/NED BibCode)
ADC_Keywords: Stars, late-type ; Stars, fundamental ; Abundances, [Fe/H] ;
Rotational velocities ; Spectroscopy
Keywords: stars: abundances - stars: atmospheres -
stars: fundamental parameters - stars: late-type - stars: rotation -
stars: solar-type
Abstract:
We report results from the high-resolution spectral analysis of the
107 metal-rich (mostly [Fe/H]≥7.67dex) target stars from the
Calan-Hertfordshire Extrasolar Planet Search programme observed with
HARPS. Using our procedure of finding the best fit to the absorption
line profiles in the observed spectra, we measure the abundances of
Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Ni, Cu and Zn, and then compare
them with known results from different authors. Most of our abundances
agree with these works at the level of ±0.05dex or better for the
stars we have in common. However, we do find systematic differences
that make direct inferences difficult. Our analysis suggests that the
selection of line lists and atomic line data along with the adopted
continuum level influence these differences the most. At the same
time, we confirm the positive trends of abundances versus metallicity
for Na, Mn, Ni and, to a lesser degree, Al. A slight negative trend is
observed for Ca, whereas Si and Cr tend to follow iron. Our analysis
allows us to determine the positively skewed normal distribution of
projected rotational velocities with a maximum peaking at 3km/s.
Finally, we obtained a Gaussian distribution of microturbulent
velocities that has a maximum at 1.2km/s and a full width at
half-maximum Δv1/2=0.35km/s, indicating that metal-rich dwarfs
and subgiants in our sample have a very restricted range in
microturbulent velocity.
Description:
The tables contain derived stellar parameters and abundances along
with the spectral ranges that we used for the line profile fitting.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea2.dat 206 107 Parameters and abundances for all target stars
tablea3.dat 25 183 Spectral ranges for the line profile fitting
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See also:
J/A+A/275/101 : Chemical evolution of the galactic disk I (Edvardsson+ 1993)
J/A+AS/129/237 : G and K dwarfs abundances (Feltzing+ 1998)
J/ApJS/159/141 : Spectroscopic properties of cool stars I (Valenti+ 2005)
J/A+A/485/571 : Abundance distribution of stars with planets (Jenkins+ 2008)
J/A+A/531/A8 : Activity indexes and velocities for 890 stars (Jenkins+ 2011)
J/A+A/545/A32 : Chemical abundances of 1111 FGK stars (Adibekyan+ 2012)
J/A+A/552/A27 : Stellar activity and kinematics of FGK stars (Murgas+ 2013)
J/A+A/562/A71 : Chemical abundances of solar neighbour dwarfs (Bensby+ 2014)
J/A+A/577/A9 : Sc, V, Mn, and Co in Milky Way stars (Battistini+ 2015)
J/ApJS/225/32 : Extended abundance analysis of cool stars (Brewer+ 2016)
Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Object name
11- 16 F6.2 pc Dist Distance (1)
18- 21 I4 K Teff Photometric effective temperature (1)
23- 26 F4.2 [cm/s2] loggSp Spectroscopic surface gravity
28- 31 F4.2 [cm/s2] loggPh Photometric surface gravity (1)
33- 36 F4.2 [Sun] [M/H]Ph Photometric metallicity (1)
38- 40 F3.1 km/s Vt Microturbulent velocity
42- 44 F3.1 km/s e_Vt Uncertainty on microturbulent velocity
46- 48 F3.1 km/s vsini Projected rotational velocity (2)
50- 52 F3.1 km/s e_vsini Uncertainty on projected rotational velocity
54- 58 F5.2 [Sun] [FeI/H] Spectroscopic metallicity (3)
60- 63 F4.2 [Sun] e_[FeI/H] Uncertainty on spectroscopic metallicity
65- 69 F5.2 [Sun] [FeII/H] Ionized Fe abundance
71- 74 F4.2 [Sun] e_[FeII/H] Uncertainty on ionized Fe abundance
76- 80 F5.2 [Sun] [Na/H] Neutral Na abundance
82- 85 F4.2 [Sun] e_[Na/H] Uncertainty on neutral Na abundance
87- 91 F5.2 [Sun] [Mg/H] Neutral Mg abundance
93- 96 F4.2 [Sun] e_[Mg/H] Uncertainty on neutral Mg abundance
98-102 F5.2 [Sun] [Al/H] Neutral Al abundance
104-107 F4.2 [Sun] e_[Al/H] Uncertainty on neutral Al abundance
109-113 F5.2 [Sun] [Si/H] Neutral Si abundance
115-118 F4.2 [Sun] e_[Si/H] Uncertainty on neutral Si abundance
120-124 F5.2 [Sun] [Ca/H] Neutral Ca abundance
126-129 F4.2 [Sun] e_[Ca/H] Uncertainty on neutral Ca abundance
131-135 F5.2 [Sun] [TiI/H] Neutral Ti abundance
137-140 F4.2 [Sun] e_[TiI/H] Uncertainty on neutral Ti abundance
142-146 F5.2 [Sun] [TiII/H] Ionized Ti abundance
148-151 F4.2 [Sun] e_[TiII/H] Uncertainty on ionized Ti abundance
153-157 F5.2 [Sun] [Cr/H] Neutral Cr abundance
159-162 F4.2 [Sun] e_[Cr/H] Uncertainty on neutral Cr abundance
164-168 F5.2 [Sun] [Mn/H] Neutral Mn abundance
170-173 F4.2 [Sun] e_[Mn/H] Uncertainty on neutral Mn abundance
175-179 F5.2 [Sun] [Ni/H] Neutral Ni abundance
181-184 F4.2 [Sun] e_[Ni/H] Uncertainty on neutral Ni abundance
186-190 F5.2 [Sun] [Cu/H] Neutral Cu abundance
192-195 F4.2 [Sun] e_[Cu/H] Uncertainty on neutral Cu abundance
197-201 F5.2 [Sun] [Zn/H] ? Neutral Zn abundance
203-206 F4.2 [Sun] e_[Zn/H] ? Uncertainty on neutral Zn abundance
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Note (1): The description of the photometric values used in this work
can be found in Jenkins et al. (2008, Cat. J/A+A/485/571).
Note (2): Projected rotational velocities were estimated using the neutral
iron lines.
Note (3): The reference solar abundances were taken from Anders & Grevesse
(1989, Geochim. Cosmochim. Acta, 53, 197).
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 5 F5.2 --- Element Code of the chemical element
7- 14 F8.3 0.1nm lambda1 Starting wavelength of the fitting range
16- 23 F8.3 0.1nm lambda2 Ending wavelength of the fitting range
25 I1 --- Nlines Number of lines for a given element in
this fitting range according to VALD-2 (1)
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Note (1): We used the atomic line data from VALD-2 (Kupka et al.,
1999, AAS, 138, 119).
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Acknowledgements:
Oleksiy M. Ivanyuk, oi(at)mao.kiev.ua
(End) Oleksiy M. Ivanyuk [MAO NAS, Ukraine], Patricia Vannier [CDS] 12-Sep-2017