J/MNRAS/422/2969 Abundances of 19 K-type giants in moving groups (Liu+, 2012)
Chemical composition of giants from two moving groups.
Liu F., Chen Y.Q., Zhao G., Han I., Lee B.C., Kim K.M., Zhao Z.S.
<Mon. Not. R. Astron. Soc., 422, 2969-2979 (2012)>
=2012MNRAS.422.2969L 2012MNRAS.422.2969L
ADC_Keywords: Clusters, open ; Stars, giant ; Stars, K-type ; Abundances
Keywords: stars: abundances - stars: fundamental parameters -
Galaxy: evolution -
open clusters and associations: individual: moving group 6 -
open clusters and associations: individual: moving group 7
Abstract:
We present the stellar parameters of 19 K-type giants and their
abundances for 13 chemical elements (Al, Ba, Ca, Fe, K, Mg, Mn, Na,
Ni, Sc, Si, Ti and V), selected from two moving groups, covering the
metallicity range of -0.6<[Fe/H]<0.2, based on high-resolution
spectra. Most of the elemental abundances show similar trends as in
previous studies, except for Al, Na and Ba, which are seriously
affected by evolution. The abundance ratios of [Na/Mg] increase
smoothly with higher [Mg/H], and those of [Al/Mg] decrease slightly
with increasing [Mg/H]. The abundance ratios of [Mg/Ba] show a
distinction between these two moving groups, which is mainly induced
by chemical evolution and also partly by kinematic effects. The
inhomogeneous metallicity of each star from the moving groups
demonstrates that these stars had different chemical origins before
they were kinematically aggregated. This favours a dynamical resonant
theory.
Description:
The observations were carried out with the Bohyunsan Optical Echelle
Spectrograph (BOES) attached to the 1.8-m telescope at the Bohyunsan
Optical Astronomy Observatory (BOAO) on two nights: 2009 March 1 and
March 4.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table5.dat 74 19 Stellar abundance ratios [X/Fe]
tablea1.dat 48 2451 All atomic-line data used for each sample star
--------------------------------------------------------------------------------
See also:
J/A+A/328/175 : K + M giants equivalent widths (Aoki+ 1997)
J/ApJ/636/821 : Abundances of Baade's Window K giants (Fulbright+, 2006)
J/ApJ/735/L46 : Spectroscopy of 64 K red giants (Bensby+, 2011)
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Star Star name
10- 13 F4.2 [Sun] [Al/Fe] Abundance ratio [Al/Fe]
15- 18 F4.2 [Sun] [Ba/Fe] Abundance ratio [Ba/Fe] (1)
20- 24 F5.2 [Sun] [Ca/Fe] Abundance ratio [Ca/Fe]
26- 30 F5.2 [Sun] [K/Fe] ?=- Abundance ratio [K/Fe]
32- 35 F4.2 [Sun] [Mg/Fe] Abundance ratio [Mg/Fe]
37- 41 F5.2 [Sun] [Mn/Fe] Abundance ratio [Mn/Fe] (1)
43- 46 F4.2 [Sun] [Na/Fe] Abundance ratio [Na/Fe]
48- 51 F4.2 [Sun] [Ni/Fe] Abundance ratio [Ni/Fe]
53- 57 F5.2 [Sun] [Sc/Fe] Abundance ratio [Sc/Fe] (1)
59- 62 F4.2 [Sun] [Si/Fe] Abundance ratio [Si/Fe]
64- 68 F5.2 [Sun] [Ti/Fe] Abundance ratio [Ti/Fe]
70- 74 F5.2 [Sun] [V/Fe] Abundance ratio [V/Fe] (1)
--------------------------------------------------------------------------------
Note (1): Hyperfine structure (HFS) corrections have been adopted
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Star Star name (and Sun)
10- 17 F8.3 0.1nm lambda Wavelength (Å)
20- 23 A4 --- Ion Element and ionisation
25- 28 F4.2 eV EP excitation potential
31- 35 F5.2 [-] loggf Oscillator strength
38- 41 F4.2 --- fC Enhancement factor
44- 48 F5.1 0.1pm EW Equivalent width (mÅ)
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 21-Jan-2013