BD+80_245: found in 2 paper(s).
Labels:
/J.P.Fulbright(2000)/
/I.I.Ivans et al.(2003)/
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A0126
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Basic Informations
| Observation Date | JD | Facility | Resolution | S/N | Exposure Time | Vrad |
|---|
| 1999-03-23 | N/A | KECKHIRES | N/A | 145 | 600 | |
Photometric data
Atmospheric data
| Teff | 5225 |
| log g | 3 |
| vturb | 1.35 |
Chemical Abundances
| Element | Nline | [X/H] | [X/Fe] | log-e |
|---|
| Na I | ... | -2.55 | -0.5 | 3.78 |
| Mg I | ... | -2.13 | -0.08 | 5.45 |
| Ca I | ... | -2.17 | -0.12 | 4.19 |
| Ti | ... | -2.25 | -0.2 | 2.77 |
| Cr I | ... | -2.17 | -0.12 | 3.50 |
| Fe | ... | -2.05 | ... | 5.45 |
| Ni I | ... | -2.07 | -0.02 | 4.18 |
| Ba II | ... | -3.92 | -1.87 | -1.79 |
| Eu II | ... | -3.09 | -1.04 | -2.58 |
: Data presented in the paper
: Data converted with the solar abundance from Grevesse et al. (1996)
A0188
| Title | Chemical Substructure in the Milky Way Halo: A New Population of Old Stars |
| ADS | I.I.Ivans et al.,ApJ, 592, 906, 2003 |
| Authors | I. I. Ivans, C. Sneden, C. R. James, G. W. Preston, J. P. Fulbright, P. A. Hoflich, B. W. Carney, J. C. Wheeler |
Get more information of this paper.
Basic Informations
| Observation Date | JD | Facility | Resolution | S/N | Exposure Time | Vrad |
|---|
| 1998-02-05 | N/A | MCDONALD | 60000 | 35-100 | 5400 | N/A |
| 1998-03-26 | N/A | KECKHIRES | 45000 | N/A | 3600 | N/A |
| Galactic Longitude (l) | N/A |
| Galactic Latitude (b) | N/A |
| Declination | +795430 |
| Right Ascension | 081106.2 |
Photometric data
| V | 10.07 |
| B-V | 0.50 |
| EB-V | 0.03 |
Atmospheric data
| Teff | 5225 |
| log g | 3.00 |
| vturb | 1.25 |
Chemical Abundances
| Element | Nline | [X/H] | [X/Fe] | log-e |
|---|
| Li I | ... | 0.28 | 2.37 | 1.44 |
| O I | ... | <-1.25 | <+0.84 | <7.62 |
| Na I | ... | -2.50+-0.01 | -0.41+-0.01 | 3.83+-0.01 |
| Mg I | ... | -2.31+-0.11 | -0.22+-0.11 | 5.27+-0.11 |
| Al I | ... | -3.42 | -1.33 | 3.05 |
| Si I | ... | -2.20 | -0.11 | 5.35 |
| K I | ... | -2.32 | -0.23 | 2.80 |
| Ca I | ... | -2.27+-0.13 | -0.18+-0.13 | 4.09+-0.13 |
| Ca II | ... | -2.25 | -0.16 | 4.11 |
| Sc II | ... | -2.51+-0.10 | -0.42+-0.10 | 0.66+-0.10 |
| Ti I | ... | -2.43+-0.05 | -0.34+-0.05 | 2.59+-0.05 |
| Ti II | ... | -2.34+-0.08 | -0.25+-0.08 | 2.68+-0.08 |
| V I | ... | -2.48 | -0.39 | 1.52 |
| V II | ... | <-1.65 | <+0.44 | <2.35 |
| Cr I | ... | -2.24+-0.09 | -0.15+-0.09 | 3.43+-0.09 |
| Cr II | ... | -1.92+-0.08 | +0.17+-0.08 | 3.75+-0.08 |
| Mn I | ... | -2.35+-0.08 | -0.26+-0.08 | 3.04+-0.08 |
| Fe I | ... | -2.09+-0.11 | ... | 5.41+-0.11 |
| Fe II | ... | -2.04+-0.11 | ... | 5.46+-0.11 |
| Co I | ... | -2.27+-0.10 | -0.18+-0.10 | 2.65+-0.10 |
| Ni I | ... | -2.18+-0.09 | -0.09+-0.09 | 4.07+-0.09 |
| Cu I | ... | <-3.12 | <-1.03 | <1.09 |
| Zn I | ... | -2.51 | -0.42 | 2.09 |
| Ga I | ... | -2.39+-0.10 | -0.30+-0.10 | 0.49+-0.10 |
| Sr II | ... | -2.94+-0.10 | -0.85+-0.10 | 0.03+-0.10 |
| Y II | ... | <-3.36 | <-1.27 | <-1.12 |
| Ba II | ... | -3.98 | -1.89 | -1.85 |
| La II | ... | -2.91+-0.05 | -0.82+-0.05 | -1.74+-0.05 |
| Eu II | ... | -2.73+-0.18 | -0.64+-0.18 | -2.22+-0.18 |
: Data presented in the paper
: Data converted with the solar abundance from Grevesse et al. (1996)