J/MNRAS/460/1356 Hercules stream K giants analysis (Ramya+, 2016)
Chemical compositions and kinematics of the Hercules stream.
Ramya P., Reddy B.E., Lambert D.L., Musthafa M.M.
<Mon. Not. R. Astron. Soc., 460, 1356-1370 (2016)>
=2016MNRAS.460.1356R 2016MNRAS.460.1356R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, K-type ; Stars, giant ; Abundances
Keywords: stars: abundances - stars: late-type - Galaxy: disc -
Galaxy: kinematics and dynamics
Abstract:
An abundance analysis is reported of 58-K giants identified by Famaey
et al. (2005, J/A+A/430/165) as highly probable members of the
Hercules stream selected from stars north of the celestial equator in
the Hipparcos catalogue. The giants have compositions spanning the
interval [Fe/H] from -0.17 to +0.42 with a mean value of +0.15 and
relative elemental abundances [El/Fe] representative of the Galactic
thin disc. Selection effects may have biased the selection from the
Hipparcos catalogue against the selection of metal-poor stars. Our
reconsideration of the recent extensive survey by Bensby et al. of FG
dwarfs, including metal-poor stars, provides a [Fe/H] distribution for
the Hercules stream, which is similar to that from the 58 giants. It
appears that the stream is dominated by metal-rich stars from the thin
disc. We discuss suggestions in the literature that the stream
includes metal-poor stars from the thick disc.
Description:
Our sample of giants was chosen from Famaey et al. (2005, Cat.
J/A+A/430/165).
Spectra of 58 giants in the Hercules stream were obtained using the
Robert G. Tull coude spectrograph at the Harlan J. Smith Telescope.
Observed spectra cover the wavelength range 3800-10000Å. However,
beyond ∼5800Å, coverage is incomplete because of gaps between the
recorded portions of the spectral orders, which progressively increase
towards redder wavelengths.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 37 70 Adopted Fe line data
table2.dat 59 58 Derived atmospheric parameters of giants from
the Hercules stream
table3.dat 37 77 Adopted line list for elements other than Fe
table4.dat 34 17 Derived solar abundances compared with the
values of Asplund et al. (2009ARA&A..47..481A 2009ARA&A..47..481A)
table5.dat 113 58 *Abundances for Hercules stream members for the
elements Na, Mg, Al, Si, Ca and Sc given as
[El/Fe]
table6.dat 128 58 Abundances for Hercules stream members for the
elements Ti, V, Cr, Mn, Co, Ni, Zn and Ba
given as [El/Fe]
table7.dat 42 17 Abundance sensitivities to various parameters
for the star HIP 8926
table8.dat 114 11 Comparisons with Pakhomov et al.
(2011, Cat. J/AZh/88/284) for common stars
table9.dat 92 14 El/Fe for three [Fe/H] intervals for our sample
of Hercules stream giants and the local giants
of Luck & Heiter (2007, Cat. J/AJ/133/2464)
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Note on table5.dat: Mean of [FeI/Fe] and [FeII/Fe] is used as [Fe/Fe]
throughout.
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See also:
J/A+A/430/165 : Radial velocities for 6691 K and M giants (Famaey+, 2005)
J/AJ/133/2464 : Parameters and abundances of nearby giants (Luck+, 2007)
J/AZh/88/284 : Chemical abundance of Hercules moving group (Pakhomov+, 2011)
Byte-by-byte Description of file: table1.dat table3.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- El Element
7- 13 F7.2 0.1nm lambda Wavelength
15- 19 F5.3 eV LEP Lower excitation potential
21- 26 F6.3 [-] loggf Oscillator strength
28- 32 F5.1 0.1pm Wlambda Solar line width
34- 37 F4.2 [-] logEps Solar abundance
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Star Star name
12- 15 I4 K Teff(J-K) ?=- Effective temperature from J-K
colour index
17- 20 I4 K Teff(V-K) ?=- Effective temperature from V-K
colour index
22- 25 I4 K Teff(sp) Effective temperature from spectrum
27- 30 F4.2 [cm/s2] logg(ph) Photometric surface gravity
32- 35 F4.2 [cm/s2] e_logg(ph) rms uncertainty on logg(ph)
37- 40 F4.2 [cm/s2] logg(sp) Spectroscopic surface gravity
42- 45 F4.2 km/s vt Microturbulent velocity
47- 51 F5.2 [-] [M/H] Metallicity
53- 55 F3.1 Gyr Age Age
57- 59 F3.1 Gyr e_Age rms uncertainty on Age
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- El Element
7- 10 F4.2 [-] logEpsC Current abundance
12- 15 F4.2 [-] e_logEpsC rms uncertainty on logEpsC
(line-to-line scatter)
17- 18 I2 --- N Number of line used
20- 23 F4.2 [-] logEpsA Asplund et al. (2009ARA&A..47..481A 2009ARA&A..47..481A) abundance
25- 28 F4.2 [-] e_logEpsA rms uncertainty on logEpsA
(line-to-line scatter)
30- 34 F5.2 [-] DlogEps Difference (logEpsC-logEpsA)
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Star Star name
12- 16 F5.2 [-] [FeI/H] Abundance [FeI/H]
18- 21 F4.2 [-] e_[FeI/H] rms uncertainty on [FeI/H]
(line-to-line scatter)
23- 24 I2 --- o_FeI Number of FeI line used
26- 30 F5.2 [-] [FeII/H] Abundance [FeII/H]
32- 35 F4.2 [-] e_[FeII/H] rms uncertainty on [FeII/H]
(line-to-line scatter)
37 I1 --- o_FeII Number of FeII line used
39- 43 F5.2 [-] [Na/Fe] Abundance [Na/Fe]
45- 48 F4.2 [-] e_[Na/Fe] rms uncertainty on [Na/Fe]
(line-to-line scatter)
50 I1 --- o_Na Number of Na line used
52- 56 F5.2 [-] [Mg/Fe] Abundance [Mg/Fe]
58- 61 F4.2 [-] e_[Mg/Fe] rms uncertainty on [Mg/Fe]
(line-to-line scatter)
63 I1 --- o_Mg Number of Mg line used
65- 68 F4.2 [-] [Al/Fe] Abundance [Al/Fe]
70- 73 F4.2 [-] e_[Al/Fe] rms uncertainty on [Al/Fe]
(line-to-line scatter)
75 I1 --- o_Al Number of Al line used
77- 80 F4.2 [-] [Si/Fe] Abundance [Si/Fe]
82- 85 F4.2 [-] e_[Si/Fe] rms uncertainty on [Si/Fe]
(line-to-line scatter)
87 I1 --- o_Si Number of Si line used
89- 93 F5.2 [-] [Ca/Fe] Abundance [Ca/Fe]
95- 98 F4.2 [-] e_[Ca/Fe] rms uncertainty on [Ca/Fe]
(line-to-line scatter)
100 I1 --- o_Ca Number of Ca line used
102-106 F5.2 [-] [Sc/Fe] Abundance [Sc/Fe] (1)
108-111 F4.2 [-] e_[Sc/Fe] rms uncertainty on [Sc/Fe]
(line-to-line scatter)
113 I1 --- o_Sc Number of Sc line used
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Note (1): Hyperfine corrections are applied for Sc.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Star Star name
12- 16 F5.2 [-] [TiI/Fe] Abundance [TiI/Fe]
18- 21 F4.2 [-] e_[TiI/Fe] rms uncertainty on [TiI/Fe]
(line-to-line scatter)
23 I1 --- o_TiI Number of TiI line used
25- 29 F5.2 [-] [TiII/Fe] Abundance [TiII/Fe]
31- 34 F4.2 [-] e_[TiII/Fe] rms uncertainty on [TiII/Fe]
(line-to-line scatter)
36 I1 --- o_TiII Number of TiII line used
38- 42 F5.2 [-] [V/Fe] Abundance [V/Fe] (1)
44- 47 F4.2 [-] e_[V/Fe] rms uncertainty on [V/Fe]
(line-to-line scatter)
49 I1 --- o_V Number of V line used
51- 55 F5.2 [-] [Cr/Fe] Abundance [Cr/Fe]
57- 60 F4.2 [-] e_[Cr/Fe] rms uncertainty on [Cr/Fe]
(line-to-line scatter)
62 I1 --- o_Cr Number of Cr line used
64- 68 F5.2 [-] [Mn/Fe] Abundance [Mn/Fe] (1)
70- 73 F4.2 [-] e_[Mn/Fe] rms uncertainty on [Mn/Fe]
(line-to-line scatter)
75 I1 --- o_Mn Number of Mn line used
77- 81 F5.2 [-] [Co/Fe] Abundance [Co/Fe] (1)
83- 86 F4.2 [-] e_[Co/Fe] rms uncertainty on [Co/Fe]
(line-to-line scatter)
88 I1 --- o_Co Number of Co line used
90- 94 F5.2 [-] [Ni/Fe] Abundance [Ni/Fe]
96- 99 F4.2 [-] e_[Ni/Fe] rms uncertainty on [Ni/Fe]
(line-to-line scatter)
101-102 I2 --- o_Ni Number of Ni line used
104-108 F5.2 [-] [Zn/Fe] Abundance [Zn/Fe]
110-113 F4.2 [-] e_[Zn/Fe] rms uncertainty on [Zn/Fe]
(line-to-line scatter)
115 I1 --- o_Zn Number of Zn line used
117-121 F5.2 [-] [Ba/Fe] Abundance [Ba/Fe] (1)
123-126 F4.2 [-] e_[Ba/Fe] rms uncertainty on [Ba/Fe]
(line-to-line scatter)
128 I1 --- o_Ba Number of Ba line used
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Note (1): Hyperfine correction are applied for V, Mn, Co and Ba.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Param Abundance ratio identification
11- 12 I2 --- N Number of line used
14- 17 F4.2 [-] sigma(Teff) Uncertainty in abundance ratio due to
effective temperature
19- 22 F4.2 [-] sigma(logg) Uncertainty in abundance ratio due to
surface gravity
24- 27 F4.2 [-] sigma(vt) Uncertainty in abundance ratio due to
microturbulent velocity
29- 32 F4.2 [-] sigma([M/H]) Uncertainty in abundance ratio due to
metallicity
34- 37 F4.2 [-] sigma(W) Uncertainty in abundance due to line width
39- 42 F4.2 [-] sigmaNet Net uncertainty in abundance ratio (1)
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Note (1): Assuming that the uncertainties in the parameters are unrelated and
independent, the net uncertainty in the abundance ratio was calculated as
a quadratic sum.
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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- 10 A10 --- Star Star name
13- 17 F5.2 [-] D[NaI/H] Abundance difference [NaI/H]
(mean 0.06±0.09) (1)
19- 23 F5.2 [-] D[MgI/H] Abundance difference [MgI/H]
(mean 0.01±0.08) (1)
25- 29 F5.2 [-] D[AlI/H] Abundance difference [AlI/H]
(mean 0.03±0.09) (1)
31- 35 F5.2 [-] D[SiI/H] Abundance difference [SiI/H]
(mean -0.04±0.09) (1)
37- 41 F5.2 [-] D[CaI/H] Abundance difference [CaI/H]
(mean -0.15±0.14) (1)
43- 47 F5.2 [-] D[ScII/H] Abundance difference [ScII/H]
(mean 0.03±0.14) (1)
49- 53 F5.2 [-] D[TiI/H] Abundance difference [TiI/H]
(mean 0.06±0.14) (1)
55- 59 F5.2 [-] D[VI/H] Abundance difference [VI/H]
(mean 0.01±0.15) (1)
61- 65 F5.2 [-] D[CrI/H] Abundance difference [CrI/H]
(mean 0.01±0.09) (1)
67- 71 F5.2 [-] D[MnI/H] Abundance difference [MnI/H]
(mean 0.16±0.12) (1)
73- 77 F5.2 [-] D[FeI/H] Abundance difference [FeI/H]
(mean 0.03±0.08) (1)
79- 83 F5.2 [-] D[FeII/H] Abundance difference [FeII/H]
(mean 0.05±0.09) (1)
85- 89 F5.2 [-] D[CoI/H] Abundance difference [CoI/H]
(mean 0.06±0.09) (1)
91- 95 F5.2 [-] D[NiI/H] Abundance difference [NiI/H]
(mean 0.07±0.09) (1)
97-100 F4.2 [-] D[BaII/H] Abundance difference [BaII/H]
(mean 0.25±0.17) (1)
102-104 I3 K DTeff Effective temperature difference
(mean 115±98) (1)
106-109 F4.2 [cm/s2] Dlogg Surface gravity difference
(mean 0.35±0.33) (1)
111-114 F4.2 km/s Dvt Microturbulent velocity difference
(mean 0.12±0.08) (1)
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Note (1): represents the difference (current value - Pakhomov et al.).
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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- 7 A7 --- Param Entity
9- 13 F5.2 [-] MeanLH1 Mean entity value for
[Fe/H] interval= -0.2 to 0.0 (1)
15- 18 F4.2 [-] e_MeanLH1 Uncertainty on Mean1
20- 22 I3 --- NLH1 Number of line used for Mean1
24- 28 F5.2 [-] MeanH1 Mean entity value for
[Fe/H] interval= -0.2 to 0.0 (2)
30- 33 F4.2 [-] e_MeanH1 Uncertainty on MeanH1
35 I1 --- NH1 Number of line used for MeanH1
37- 41 F5.2 [-] MeanLH2 Mean entity value for
[Fe/H] interval= 0.0 to +2.00 (1)
43- 46 F4.2 [-] e_MeanLH2 Uncertainty on MeanLH2
48- 50 I3 --- NLH2 Number of line used for MeanLH2
52- 56 F5.2 [-] MeanH2 Mean entity value for
[Fe/H] interval= 0.0 to +2.00 (2)
58- 61 F4.2 [-] e_MeanH2 Uncertainty on MeanH2
63- 64 I2 --- NH2 Number of line used for MeanH2
66- 70 F5.2 [-] MeanLH3 ?=- Mean entity value for
[Fe/H] interval= +0.20 to +0.40 (1)
72- 75 F4.2 [-] e_MeanLH3 ?=- Uncertainty on MeanLH3
77- 78 I2 --- NLH3 ?=- Number of line used for MeanLH3
80- 84 F5.2 [-] MeanH3 Mean entity value for
[Fe/H] interval= +0.20 to +0.40 (2)
86- 89 F4.2 [-] e_MeanH3 Uncertainty on MeanH3
91- 92 I2 --- NH3 Number of line used for MeanH3
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Note (1): for Luck & Heiter (2007, Cat. J/AJ/133/2464) local giants
Note (2): for Hercules stream giants, this paper
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 06-Oct-2017