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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 (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:
FileName Lrecl Records Explanations
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) 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)
Note on table5.dat: Mean of [FeI/Fe] and [FeII/Fe] is used as [Fe/Fe] throughout.
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
Bytes Format Units Label Explanations
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
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
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
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
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) abundance 25- 28 F4.2 [-] e_logEpsA rms uncertainty on logEpsA (line-to-line scatter) 30- 34 F5.2 [-] DlogEps Difference (logEpsC-logEpsA)
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
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
Note (1): Hyperfine corrections are applied for Sc.
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
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
Note (1): Hyperfine correction are applied for V, Mn, Co and Ba.
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
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)
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.
Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
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)
Note (1): represents the difference (current value - Pakhomov et al.).
Byte-by-byte Description of file: table9.dat
Bytes Format Units Label Explanations
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
Note (1): for Luck & Heiter (2007, Cat. J/AJ/133/2464) local giants Note (2): for Hercules stream giants, this paper
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 06-Oct-2017
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