J/A+A/433/185 Detailed abundance analysis of 102 F and G dwarfs (Bensby+, 2005)
α-, r-, and s-process element abundance trends in the Galactic thin
and thick disks.
Bensby T., Feltzing S., Lundstroem I., Ilyin I.
<Astron. Astrophys. 433, 185 (2005)>
=2005A&A...433..185B 2005A&A...433..185B
ADC_Keywords: Stars, dwarfs ; Abundances
Keywords: stars: fundamental parameters - stars: abundances - Galaxy: disk -
Galaxy: formation - Galaxy: abundances -
Galaxy: kinematics and dynamics
Description:
From a detailed elemental abundance analysis of 102 F and G dwarf
stars we present abundance trends in the Galactic thin and thick disks
for 14 elements (O, Na, Mg, Al, Si, Ca, Ti, Cr, Fe, Ni, Zn, Y, Ba, and
Eu). Stellar parameters and elemental abundances (except for Y, Ba and
Eu) for 66 of the 102 stars were presented in our previous studies
(Bensby et al. 2003, J/A+A/410/527, 2004, J/A+A/415/155). The 36
stars that are new in this study extend and confirm our previous
results and allow us to draw further conclusions regarding abundance
trends. The s-process elements Y and Ba, and the r-element Eu have
also been considered here for the whole sample for the first time.
To make it easier to gather the elemental abundances for all 102 stars
we have included the abundance data from Bensby et al. (2003, Cat.
J/A+A/410/527) and from Bensby et al. (2004, Cat. J/A+A/415/155)
in table9.dat
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 56 73 Atomic data
table8.dat 28 102 Stellar ages
table9.dat 345 102 Abundances
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See also:
J/A+A/410/527 : Abundances in the Galactic disk (Bensby+, 2003)
J/A+A/415/155 : Oxygen abundances in the Galactic disk (Bensby+, 2004)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- El Element
5 A1 --- Ion Ionisation
8- 15 F8.3 01.nm Lambda Wavelength
18- 21 F4.2 eV LEP Lower excitation potential
24- 27 F4.2 --- dgamma6 ? Correction factor to Unsoeld broadening (1)
30 A1 --- DMP [SU] Method for collisional broadening (2)
33- 39 E7.2 s-1 gammaRad Radiation damping constant
42- 47 F6.3 --- loggf log of oscillator strength
50- 56 A7 --- r_loggf Reference to loggf (3)
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Note (1): Only used if column DMP = "U"
Note (2): An "S" indicates that broadening by collisions have been taken
from Anstee et al. (1995MNRAS.276..859A 1995MNRAS.276..859A), Barklem & O'Mara
(1997MNRAS.290..102B 1997MNRAS.290..102B, 1998MNRAS.300..863B 1998MNRAS.300..863B), and Barklem et al.
(1998MNRAS.296.1057B 1998MNRAS.296.1057B, 2000, Cat. J/A+AS/142/467).
A "U" indicates that the classical Unsold broadening has been used.
Note (3): References to loggf are the following:
PN = Pitts & Newsom (1986, J. Quant. Spectr. Rad. Transf., 35, 383)
SMP = Sneden et al. (1996ApJ...467..819S 1996ApJ...467..819S)
G67 = Gallagher (1967, Physical Review, 157, 24)
LWDS = Lawler et al. (2001ApJ...563.1075L 2001ApJ...563.1075L)
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HIP Hipparcos (Cat. I/239) number
9 I1 --- Mem [1/3] Population membership (G1)
12- 15 F4.1 Gyr Age ? Stellar age
18- 21 F4.1 Gyr AgeMin ? Lower limit on stellar age
24- 27 F4.1 Gyr AgeMax ? Upper limit on stellar age
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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- 6 I6 --- HIP Hipparcos (Cat. I/239) number
8 A1 --- Inst [SFU] Instrument (1)
13 I1 --- Mem [1/3] Membership (G1)
19- 23 F5.2 [Sun] [Fe/H]I Abundance [Fe/H] from Fe I lines
25- 29 F5.2 [Sun] [Fe/H]II Abundance [Fe/H] from Fe II lines
31- 35 F5.2 [Sun] [Na/H] Abundance [Na/H]
37- 41 F5.2 [Sun] [Mg/H] Abundance [Mg/H]
43- 47 F5.2 [Sun] [Al/H] Abundance [Al/H]
49- 53 F5.2 [Sun] [Si/H] Abundance [Si/H]
55- 59 F5.2 [Sun] [Ca/H] Abundance [Ca/H]
61- 65 F5.2 [Sun] [Ti/H]I Abundance [Ti/H] from Ti I lines
67- 71 F5.2 [Sun] [Ti/H]II Abundance [Ti/H] from Ti II lines
73- 77 F5.2 [Sun] [Cr/H]I Abundance [Cr/H] from Cr I lines
79- 83 F5.2 [Sun] [Cr/H]II Abundance [Cr/H] from Cr II lines
85- 89 F5.2 [Sun] [Ni/H] Abundance [Ni/H]
91- 95 F5.2 [Sun] [Zn/H] Abundance [Zn/H]
97-101 F5.2 [Sun] [Y/H] Abundance [Y/H]
103-107 F5.2 [Sun] [Ba/H] Abundance [Ba/H]
111-114 F4.2 [Sun] s[Fe/H]I spread in [Fe/H] from Fe I lines
117-120 F4.2 [Sun] s[Fe/H]II spread in [Fe/H] from Fe II lines
123-126 F4.2 [Sun] s[Na/H] spread in [Na/H]
129-132 F4.2 [Sun] s[Mg/H] spread in [Mg/H]
135-138 F4.2 [Sun] s[Al/H] spread in [Al/H]
141-144 F4.2 [Sun] s[Si/H] spread in [Si/H]
147-150 F4.2 [Sun] s[Ca/H] spread in [Ca/H]
153-156 F4.2 [Sun] s[Ti/H]I spread in [Ti/H] from Ti I lines
159-162 F4.2 [Sun] s[Ti/H]II spread in [Ti/H] from Ti II lines
165-168 F4.2 [Sun] s[Cr/H]I spread in [Cr/H] from Cr I lines
171-174 F4.2 [Sun] s[Cr/H]II spread in [Cr/H] from CR II lines
177-180 F4.2 [Sun] s[Ni/H] spread in [Ni/H]
183-186 F4.2 [Sun] s[Zn/H] spread in [Zn/H]
189-192 F4.2 [Sun] s[Y/H] spread in [Y/H]
195-198 F4.2 [Sun] s[Ba/H] spread in [Ba/H]
203-205 I3 --- o_[Fe/H]I number of Fe I lines used for [Fe/H]
209-211 I3 --- o_[Fe/H]II number of Fe II lines used for [Fe/H]
215-217 I3 --- o_[Na/H] number of lines used for [Na/H]
221-223 I3 --- o_[Mg/H] number of lines used for [Mg/H]
227-229 I3 --- o_[Al/H] number of lines used for [Al/H]
233-235 I3 --- o_[Si/H] number of lines used for [Si/H]
239-241 I3 --- o_[Ca/H] number of lines used for [Ca/H]
245-247 I3 --- o_[Ti/H]I number of Ti I lines used for [Ti/H]
251-253 I3 --- o_[Ti/H]II number of Ti II lines used for [Ti/H]
257-259 I3 --- o_[Cr/H]I number of Cr I lines used for [Cr/H]
263-265 I3 --- o_[Cr/H]II number of Cr II lines used for [Cr/H]
269-271 I3 --- o_[Ni/H] number of lines used for [Ni/H]
275-277 I3 --- o_[Zn/H] number of lines used for [Zn/H]
281-283 I3 --- o_[Y/H] number of lines used for [Y/H]
287-289 I3 --- o_[Ba/H] number of lines used for [Ba/H]
294-299 F6.3 [Sun] [O/H]6300 ? [O/H] from forbidden O line at 630.0nm (2)
301-306 F6.3 [Sun] [O/H]6363 ? [O/H] from forbidden O line at 636.3nm
309-313 F5.2 [Sun] [O/H]7771 ? [O/H] from permitted O line at 777.1nm
316-320 F5.2 [Sun] [O/H]7773 ? [O/H] from permitted O line at 777.3nm
323-327 F5.2 [Sun] [O/H]7774 ? [O/H] from permitted O line at 777.4nm
331-336 F6.3 [Sun] [Eu/H]6645 ? [Eu/H] from europium line at 664.5nm
339-343 F5.2 [Sun] [Eu/H]4129 ? [Eu/H] from europium line at 412.9nm
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Note (1): Instrument is coded as follows:
S = SOFIN spectrograph on Nordic Optical Telescope
F = FEROS spectrograph on ESO-2.2m telescope
U = UVES spectrograph on VLT Kueyen
Note (2): Apart from the SOFIN stars, the indications in column "Inst"
do generally not apply to this column. Most of the FEROS stars have
been observed with the CES spectrograph on the ESO-3.6m telescope from
which spectra the forbidden oxygen abundances were determined (see
Bensby et al., 2004, Cat. J/A+A/415/155)
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Global notes:
Note (G1): Membership as follows:
1 = Thin disk star
2 = Thick disk star
3 = "Transition object"
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Acknowledgements: Thomas Bensby, tbensby(at)umich.edu
History:
* 20-Dec-2004: Original version
* 21-Apr-2005: HIP 116740 membership corrected in table8
(End) Thomas Bensby [Dept. of Astronomy, Univ. of Michigan] 20-Dec-2004