HKII17435_00532: found in 1 paper(s).

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/I.U.Roederer et al.(2008)/

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A0172

Title The Hobby-Eberly Telescope Chemical Abundances of Stars in the Halo (CASH) Project. I. The Lithium-, s-, and r-enhanced Metal-poor Giant HKII 17435-00532
ADS I.U.Roederer et al.,ApJ, 679, 1549, 2008
Authors I. U. Roederer, A. Frebel, M. D. Shetrone, C. AllendePrieto, J. Rhee, R. Gallino, S. Bisterzo, C. Sneden, T. C. Beers, J. J. Cowan

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Basic Informations

Observation Date JD Facility Resolution S/N Exposure Time Vrad
2007-02-09 2454140.79715 N/A 15000 50-160 600 38.61+-0.64
2007-02-28 2454159.73386 N/A 15000 50-160 600 38.77+-0.57
2007-07-15 2454297.61639 N/A 60000 10-25 1200 39.36+-0.59
2007-08-05 2454318.60116 N/A 60000 10-25 1200 38.79+-1.07
Galactic Longitude (l) N/A
Galactic Latitude (b) N/A
Declination N/A
Right Ascension N/A

Photometric data

V 13.145+-0.166
H 11.121+-0.023
J 11.534+-0.021
K 11.049+-0.020
EB-V 0.042

Atmospheric data

Teff 5200+-150
log g 2.15+-0.4
vturb 2.0+-0.3

Chemical Abundances

Element Nline [X/H] [X/Fe] log-e
Li I...0.90+-0.163.13+-0.162.06+-0.16
C...-1.55+-0.3+0.68+-0.36.97+-0.3
O I...-1.17+-0.27+1.06+-0.277.56+-0.27
Na I...-1.54+-0.16+0.69+-0.164.79+-0.16
Mg I...-1.81+-0.25+0.42+-0.255.77+-0.25
K I...-1.79+-0.17+0.44+-0.173.33+-0.17
Ca I...-1.80+-0.19+0.43+-0.194.56+-0.19
Sc II...-2.03+-0.21+0.20+-0.211.14+-0.21
Ti I...-2.01+-0.22+0.22+-0.223.01+-0.22
Ti II...-1.90+-0.20+0.33+-0.203.12+-0.20
Cr I...-2.38+-0.16-0.15+-0.163.29+-0.16
Mn I...-2.54+-0.24-0.31+-0.242.85+-0.24
Fe I...-2.23...5.27
Fe II...-2.23...5.27
Ni I...-2.12+-0.18+0.11+-0.184.13+-0.18
Sr II...-1.87+-0.26+0.36+-0.261.05+-0.26
Y II...-2.06+-0.19+0.17+-0.190.18+-0.19
Zr II...-1.46+-0.27+0.77+-0.271.14+-0.27
Ba II...-1.37+-0.29+0.86+-0.290.76+-0.29
La II...-1.45+-0.21+0.78+-0.21-0.28+-0.21
Ce II...-1.06+-0.20+1.17+-0.200.52+-0.20
Pr II...-1.13+-0.20+1.10+-0.20-0.42+-0.20
Nd II...-1.19+-0.19+1.04+-0.190.31+-0.19
Sm II...-1.50+-0.22+0.73+-0.22-0.49+-0.22
Eu II...-1.75+-0.20+0.48+-0.20-1.24+-0.20
    : Data presented in the paper
    : Data converted with the solar abundance from Grevesse et al. (1996)