J/A+A/562/A71 Chemical abundances of solar neighbourhood dwarfs (Bensby+, 2014)
Exploring the Milky Way stellar disk. A detailed elemental abundance study of
714 F and G dwarf stars in the solar neighbourhood.
Bensby T., Feltzing S., Oey M.S.
<Astron. Astrophys. 562, A71 (2014)>
=2014A&A...562A..71B 2014A&A...562A..71B
ADC_Keywords: Abundances ; Spectroscopy ; Stars, ages ; Stars, dwarfs ;
Stars, nearby
Keywords: Galaxy: disk - Galaxy: formation - Galaxy: evolution -
stars: abundances - stars: fundamental parameters -
stars: kinematics and dynamics
Abstract:
We present a detailed elemental abundance study of 714 F and G dwarf
and subgiant stars in the Solar neighbourhood. The analysis is based
on high-resolution spectra obtained with MIKE on the Magellan
telescope, FEROS on the ESO 1.5m and 2.2m telescopes, HARPS on the
ESO 3.6m telescope, UVES on the ESO Very Large Telescope, SOFIN and
FIES on the Nordic Optical Telescope. Our data show that there is an
old and alpha-enhanced disk population, and a younger and less
alpha-enhanced disk population. While they overlap greatly in
metallicity between -0.7<[Fe/H]<+0.1, they show a bimodal
distribution in [alpha/Fe]. This bimodality becomes even clearer if
stars where stellar parameters and abundances show larger
uncertainties (Teff<5400K) are discarded, showing that it is
important to constrain the data set to a narrow range in the stellar
parameters if small differences between stellar populations are to be
revealed. In addition, we find that the alpha-enhanced population has
orbital parameters placing the stellar birthplaces in the inner
Galactic disk while the low-alpha stars mainly come from the outer
Galactic disk, fully consistent with the recent claims of a short
scale-length for the alpha-enhanced Galactic thick disk. We have also
investigated the properties of the Hercules stream and the Arcturus
moving group.
Description:
In the following tables we give stellar parameters, stellar ages,
kinematical parameters, orbital parameters, and detailed elemental
abundances for O, Na, Mg, Al, Si, Ca, Ti, Cr, Fe, Ni, Zn, Y, and Ba
for 714 nearby F and G dwarf stars. We also list the atomic data used
(oscillator strengths), as well as equivalent widths and abundances
for individual lines in the Sun. Finally we list stars that were
observed but not analysed as they turned out to be either
spectroscopic binaries or rotated too fast to allow a proper abundance
analysis.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 8 161 Stars rejected from analysis
tablec2.dat 38 496 Atomic line data, solar equivalent widths, and
solar abundances
tablec3.dat 796 714 Elemental abundances, stellar ages, kinematics
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See also:
I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)
J/AJ/118/895 : Milky way and stellar distributions (Tiede+ 1999)
J/A+A/377/911 : Solar neighborhood age-metallicity relation (Feltzing+ 2001)
J/MNRAS/325/1365 : Solar neighborhood metallicity distribution (Haywood+ 2001)
J/PAZh/30/173 : Space velocities of solar neighborhood stars (Borkova+ 2004)
J/ApJ/714/663 : Stellar density map of the Milky Way (de Jong+, 2010)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HIP Hipparcos number
8 I1 --- Rej [1/2] Reason for rejection (1)
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Note (1): Spectrographs and observing runs have the following codes:
1 = Wide spectral lines, probably due to high vsini
2 = Double or wide spectral lines, probably due to spectroscopic binary
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Byte-by-byte Description of file: tablec2.dat
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Bytes Format Units Label Explanations
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2- 3 A2 --- El Element
5 I1 --- Ion Ion (1=neutral, 2=ionised)
7- 14 F8.3 0.1nm lambda Line wavelength
16- 21 F6.2 [-] loggf Oscillator strength (1)
23- 27 F5.2 eV LEP Lower excitation potential
29- 33 F5.1 pm EW Line equivalent width
35- 38 F4.2 [-] Abun Absolute abundance 12+log(N/H) (2)
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Note (1): References for the oscillator strengths can be found in
Bensby et al., 2003, Cat. J/A+A/410/527.
Note (2): The reported O and Na abundances are not corrected for NLTE effects.
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Byte-by-byte Description of file: tablec3.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HIP Hipparcos number
9- 10 I2 --- Spec [1/77] Spectrograph + date (1)
13- 16 I4 K Teff Effective temperature
19- 21 I3 K e_Teff Uncertainty in Teff
24- 27 F4.2 [cm/s2] logg Surface gravity
30- 33 F4.2 [cm/s2] e_logg Uncertainty in logg
36- 39 F4.2 km/s xi Microturbulence velocity ξ
42- 45 F4.2 km/s e_xi Uncertainty in xi
48- 51 F4.2 [-] Fe1 Absolute FeI abundance
54- 57 F4.2 [-] Fe2 Absolute FeII abundance
60- 63 F4.2 Sun M Stellar mass
66- 69 F4.2 Sun b_M Lower limit on M
72- 75 F4.2 Sun B_M Upper limit on M
78- 81 F4.1 Gyr Age Stellar age
84- 87 F4.1 Gyr b_Age Lower limit on Age
90- 93 F4.1 Gyr B_Age Upper limit on Age
95- 99 F5.2 [Sun] Fe/H Abundance ratio Fe/H normalised to Sun
102-106 F5.2 [Sun] O/Fe ? Abundance ratio O/Fe normalised to Sun
109-113 F5.2 [Sun] Na/Fe ? Abundance ratio Na/Fe normalised to Sun
116-120 F5.2 [Sun] Mg/Fe ? Abundance ratio Mg/Fe normalised to Sun
123-127 F5.2 [Sun] Al/Fe ? Abundance ratio Al/Fe normalised to Sun
130-134 F5.2 [Sun] Si/Fe ? Abundance ratio Si/Fe normalised to Sun
137-141 F5.2 [Sun] Ca/Fe ? Abundance ratio Ca/Fe normalised to Sun
144-148 F5.2 [Sun] Ti/Fe ? Abundance ratio Ti/Fe normalised to Sun
151-155 F5.2 [Sun] Cr/Fe ? Abundance ratio Cr/Fe normalised to Sun
158-162 F5.2 [Sun] Ni/Fe ? Abundance ratio Ni/Fe normalised to Sun
165-169 F5.2 [Sun] Zn/Fe ? Abundance ratio Zn/Fe normalised to Sun
172-176 F5.2 [Sun] Y/Fe ? Abundance ratio Y/Fe normalised to Sun
179-183 F5.2 [Sun] Ba/Fe ? Abundance ratio Ba/Fe normalised to Sun
185-188 F4.2 [Sun] e_Fe/H Uncertainty on abundance ratio Fe/H
191-194 F4.2 [Sun] e_O/Fe ? Uncertainty on abundance ratio O/Fe
197-200 F4.2 [Sun] e_Na/Fe ? Uncertainty on abundance ratio Na/Fe
203-206 F4.2 [Sun] e_Mg/Fe ? Uncertainty on abundance ratio Mg/Fe
209-212 F4.2 [Sun] e_Al/Fe ? Uncertainty on abundance ratio Al/Fe
215-218 F4.2 [Sun] e_Si/Fe ? Uncertainty on abundance ratio Si/Fe
221-224 F4.2 [Sun] e_Ca/Fe ? Uncertainty on abundance ratio Ca/Fe
227-230 F4.2 [Sun] e_Ti/Fe ? Uncertainty on abundance ratio Ti/Fe
233-236 F4.2 [Sun] e_Cr/Fe ? Uncertainty on abundance ratio Cr/Fe
239-242 F4.2 [Sun] e_Ni/Fe ? Uncertainty on abundance ratio Ni/Fe
245-248 F4.2 [Sun] e_Zn/Fe ? Uncertainty on abundance ratio Zn/Fe
251-254 F4.2 [Sun] e_Y/Fe ? Uncertainty on abundance ratio Y/Fe
257-260 F4.2 [Sun] e_Ba/Fe ? Uncertainty on abundance ratio Ba/Fe
262-266 F5.2 [Sun] Ti/H ? Abundance ratio Ti/H normalised to Sun
269-273 F5.2 [Sun] O/Ti ? Abundance ratio O/Ti normalised to Sun
276-280 F5.2 [Sun] Na/Ti ? Abundance ratio Na/Ti normalised to Sun
283-287 F5.2 [Sun] Mg/Ti ? Abundance ratio Mg/Ti normalised to Sun
290-294 F5.2 [Sun] Al/Ti ? Abundance ratio Al/Ti normalised to Sun
297-301 F5.2 [Sun] Si/Ti ? Abundance ratio Si/Ti normalised to Sun
304-308 F5.2 [Sun] Ca/Ti ? Abundance ratio Ca/Ti normalised to Sun
311-315 F5.2 [Sun] Cr/Ti ? Abundance ratio Cr/Ti normalised to Sun
318-322 F5.2 [Sun] Ni/Ti ? Abundance ratio Ni/Ti normalised to Sun
325-329 F5.2 [Sun] Fe/Ti ? Abundance ratio Fe/Ti normalised to Sun
332-336 F5.2 [Sun] Zn/Ti ? Abundance ratio Zn/Ti normalised to Sun
339-343 F5.2 [Sun] Y/Ti ? Abundance ratio Y/Ti normalised to Sun
346-350 F5.2 [Sun] Ba/Ti ? Abundance ratio Ba/Ti normalised to Sun
352-355 F4.2 [Sun] e_Ti/H ? Uncertainty on abundance ratio Ti/H
358-361 F4.2 [Sun] e_O/Ti ? Uncertainty on abundance ratio O/Ti
364-367 F4.2 [Sun] e_Na/Ti ? Uncertainty on abundance ratio Na/Ti
370-373 F4.2 [Sun] e_Mg/Ti ? Uncertainty on abundance ratio Mg/Ti
376-379 F4.2 [Sun] e_Al/Ti ? Uncertainty on abundance ratio Al/Ti
382-385 F4.2 [Sun] e_Si/Ti ? Uncertainty on abundance ratio Si/Ti
388-391 F4.2 [Sun] e_Ca/Ti ? Uncertainty on abundance ratio Ca/Ti
394-397 F4.2 [Sun] e_Cr/Ti ? Uncertainty on abundance ratio Cr/Ti
400-403 F4.2 [Sun] e_Ni/Ti ? Uncertainty on abundance ratio Ni/Ti
406-409 F4.2 [Sun] e_Fe/Ti ? Uncertainty on abundance ratio Fe/Ti
412-415 F4.2 [Sun] e_Zn/Ti ? Uncertainty on abundance ratio Zn/Ti
418-421 F4.2 [Sun] e_Y/Ti ? Uncertainty on abundance ratio Y/Ti
424-427 F4.2 [Sun] e_Ba/Ti ? Uncertainty on abundance ratio Ba/Ti
429-431 I3 --- nFe1 Number of lines per Fe1 ion
434-436 I3 --- nFe2 Number of lines per Fe2 ion
439-441 I3 --- nO1 ? Number of lines per O1 ion
444-446 I3 --- nNa1 ? Number of lines per Na1 ion
449-451 I3 --- nMg1 ? Number of lines per Mg1 ion
454-456 I3 --- nAl1 ? Number of lines per Al1 ion
459-461 I3 --- nSi1 ? Number of lines per Si1 ion
464-466 I3 --- nCa1 ? Number of lines per Ca1 ion
469-471 I3 --- nTi1 ? Number of lines per Ti1 ion
474-476 I3 --- nTi2 ? Number of lines per Ti2 ion
479-481 I3 --- nCr1 ? Number of lines per Cr1 ion
484-486 I3 --- nCr2 ? Number of lines per Cr2 ion
489-491 I3 --- nNi1 ? Number of lines per Ni1 ion
494-496 I3 --- nZn1 ? Number of lines per Zn1 ion
499-501 I3 --- nY2 ? Number of lines per Y2 ion
504-506 I3 --- nBa2 ? Number of lines per Ba2 ion
508-511 F4.2 --- sFe1 1-σ line-to-line dispersion per Fe1 ion
514-517 F4.2 --- sFe2 1-σ line-to-line dispersion per Fe2 ion
520-523 F4.2 --- sO1 ? 1-σ line-to-line dispersion per O1 ion
526-529 F4.2 --- sNa1 ? 1-σ line-to-line dispersion per Na1 ion
532-535 F4.2 --- sMg1 ? 1-σ line-to-line dispersion per Mg1 ion
538-541 F4.2 --- sAl1 ? 1-σ line-to-line dispersion per Al1 ion
544-547 F4.2 --- sSi1 ? 1-σ line-to-line dispersion per Si1 ion
550-553 F4.2 --- sCa1 ? 1-σ line-to-line dispersion per Ca1 ion
556-559 F4.2 --- sTi1 ? 1-σ line-to-line dispersion per Ti1 ion
562-565 F4.2 --- sTi2 ? 1-σ line-to-line dispersion per Ti2 ion
568-571 F4.2 --- sCr1 ? 1-σ line-to-line dispersion per Cr1 ion
574-577 F4.2 --- sCr2 ? 1-σ line-to-line dispersion per Cr2 ion
580-583 F4.2 --- sNi1 ? 1-σ line-to-line dispersion per Ni1 ion
586-589 F4.2 --- sZn1 ? 1-σ line-to-line dispersion per Zn1 ion
592-595 F4.2 --- sY2 ? 1-σ line-to-line dispersion per Y2 ion
598-601 F4.2 --- sBa2 ? 1-σ line-to-line dispersion per Ba2 ion
604-609 F6.2 mas plx Hipparcos parallax
614-619 F6.2 mas e_plx Uncertainty in plx
623-628 F6.4 kpc Dist Heliocentric distance
632-638 F7.3 deg GLON Galactic longitude
642-648 F7.3 deg GLAT Galactic latitude
652-656 I5 km/s Ulsr U velocity relative to LSR
660-664 I5 km/s Vlsr V velocity relative to LSR
668-672 I5 km/s Wlsr W velocity relative to LSR
676-680 F5.2 kpc Rmin Perigalactic distance of stellar orbit
683-688 F6.2 kpc Rmax Apogalactic distance of stellar orbit
692-696 F5.2 kpc zmax Maximum distance from galactic plane
699-704 F6.4 --- e [0/1] Eccentricity of stellar orbit
708-712 I5 kpc.km/s Lz Orbital angular momentum
715-720 F6.4 --- Elsr Orbital energy normalised to LSR
724-731 E8.3 --- td/d Thick disk-to-thin disk probability ratio
734-741 E8.3 --- td/h Thick disk-to-halo probability ratio
744-751 E8.3 --- her/td Hercules-to-thick disk probability ratio
754-761 E8.3 --- her/d Hercules-to-thin disk probability ratio
763-766 I4 K TeffI Uncorrected ion.bal. temperature
769-772 F4.2 [cm/s2] loggI Uncorrected ion.bal. gravity
775-778 I4 K TeffH Teff when using Hipparcos parallax for logg
781-784 F4.2 [cm/s2] loggH logg when using Hipparcos parallax
787-790 F4.2 [-] Fe1H Absolute FeI abundance when using
Hipparcos parallax
793-796 F4.2 [-] Fe2H Absolute FeII abundance when using
Hipparcos parallax
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Note (1): Spectrographs and observing runs have the following codes:
1 = MIKE, August 2005
2 = MIKE, January 2006
3 = MIKE, April 2006
4 = MIKE, August 2006
5 = MIKE, April 2007
6 = UVES, July 2002
7 = UVES, 2003/2004
8 = UVES POP archive
9 = SOFIN, 2002
10 = SOFIN, 2002
11 = SOFIN, 2003
12 = SOFIN, 2004
13 = SOFIN, 2006
14 = FEROS, September 2000
15 = FEROS, August 2001
16 = FEROS, 2005
17 = MIKE, May 2007
18 = MIKE, July 2007
19 = MIKE, November 2007
77 = FIES, HARPS
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Acknowledgements:
Thomas Bensby, tbensby(at)astro.lu.se
(End) Thomas Bensby [Lund Obs., Sweden], Patricia Vannier [CDS] 03-Jan-2014