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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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 56 73 Atomic data table8.dat 28 102 Stellar ages table9.dat 345 102 Abundances
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
Bytes Format Units Label Explanations
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)
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), Barklem & O'Mara (1997MNRAS.290..102B, 1998MNRAS.300..863B), and Barklem et al. (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) G67 = Gallagher (1967, Physical Review, 157, 24) LWDS = Lawler et al. (2001ApJ...563.1075L)
Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
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
Byte-by-byte Description of file: table9.dat
Bytes Format Units Label Explanations
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
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)
Global notes: Note (G1): Membership as follows: 1 = Thin disk star 2 = Thick disk star 3 = "Transition object"-------------------------------------------------------------------------------- Acknowledgements: Thomas Bensby, tbensby(at)umich.edu
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
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