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s- and r-Process Element Abundances in the CMD of 47 Tucanæ Using the Robert Stobie Spectrograph on SALT*

Published online by Cambridge University Press:  05 March 2013

C. C. Worley*
Affiliation:
Department of Physics & Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand
P. L. Cottrell
Affiliation:
Department of Physics & Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand
E. C. Wylie de Boer
Affiliation:
Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, Cotter Rd, Weston, ACT 2611, Australia
*
CCorresponding author. Email: clare.worley@pg.canterbury.ac.nz
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Abstract

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A recent study by Wylie et al. (2006) has revealed that s-process element abundances are enhanced relative to iron in both red giant branch and asymptotic giant branch stars of 47 Tuc. A more detailed investigation into s-process element abundances throughout the colour-magnitude diagram of 47 Tuc is vital in order to determine whether the observed enhancements are intrinsic to the cluster. This paper explores this possibility through observational and theoretical means. The visibility of s- and r-process element lines in synthetic spectra of giant and dwarf stars throughout the colour magnitude diagram of 47 Tuc has been explored. It was determined that a resolving power of 10 000 was sufficient to observe s-process element abundance variations in globular cluster giant-branch stars. These synthetic results were compared with the spectra of eleven 47 Tuc giant branch stars observed during the performance verification of the Robert Stobie Spectrograph on the Southern African Large Telescope. Three s-process elements (Zr, Ba and Nd) and one r-process element (Eu) were investigated. No abundance variations were found such that [X/Fe] = 0.0 ± 0.5 dex. It was concluded that this resolving power, R ∼ 5000, was not sufficient to obtain exact abundances but upper limits on the s-process element abundances could be determined.

Type
Research Article
Copyright
Copyright © Astronomical Society of Australia 2008

Footnotes

*

Based on observations made with the Southern African Large Telescope (SALT).

References

Alonso, A., Arribas, S. & Martínez-Roger, C., 1999, A&AS, 140, 261 Google Scholar
Biemont, E., Grevesse, N., Hannaford, P. & Lowe, R. M., 1981, ApJ, 248, 867 Google Scholar
Buckley, D. A. H., Burgh, E. B., Cottrell, P. L., Nordsieck, K. H., O'Donoghue, D. & Williams, T. B., 2006, in Proc. SPIE 6269, Ground-Based and Airborne Instrumentation for Astronomy, Eds. McLean, I. S. & Masanori, I., 62690AGoogle Scholar
Busso, M., Gallino, R., Lambert, D. L., Travaglio, C. & Smith, V. V., 2001, ApJ, 557, 802 Google Scholar
Cannon, R., da Costa, G., Norris, J., Stanford, L. & Croke, B., 2003, in ASPC 296, New Horizons in Globular Cluster Astronomy, Eds. Piotto, G., Meylan, G., Djorgovski, S. G. & Riello, M., 175 Google Scholar
Cannon, R. D., Croke, B. F. W., Bell, R. A., Hesser, J. E. & Stathakis, R. A., 1998, MNRAS, 298, 601 CrossRefGoogle Scholar
Cottrell, P., Albrow, M., Barnes, S. & Kershaw, G., 2005, Critical Design Review for the Southern African Large Telescope High-Resolution SpectrographGoogle Scholar
Den Hartog, E. A., Lawler, J. E., Sneden, C. & Cowan, J. J., 2003, ApJS, 148, 543 Google Scholar
Gilliland, R. L., Bono, G., Edmonds, P. D., Caputo, F., Cassisi, S., Petro, L. D., Saha, A. & Shara, M. M., 1998, ApJ, 507, 818 CrossRefGoogle Scholar
Gratton, R., Sneden, C. & Carretta, E., 2004, ARA&A, 42, 385 Google Scholar
Hannaford, P., Lowe, R. M., Grevesse, N., Biemont, E. & Whaling, W., 1982, ApJ, 261, 736 CrossRefGoogle Scholar
Harris, W. E., 1996, AJ, 112, 1487 CrossRefGoogle Scholar
Hartwick, F. D. A. & Hesser, J. E., 1974, BAAS, 6, 216 Google Scholar
Kurucz, R. L. & Peytremann, E., 1975, SAO Special Report, 362 Google Scholar
Lawler, J. E., Bonvallet, G. & Sneden, C., 2001, ApJ, 556, 452 CrossRefGoogle Scholar
Lee, S. W., 1977, A&AS, 27, 381 Google Scholar
McWilliam, A. & Bernstein, R. A., 2008, ApJ, in press (astro-ph/0709.1964v2)Google Scholar
Nordsieck, K. H., Burgh, E. B., Kobulnicky, H. A., Williams, T. B., O'Donoghue, D., Percival, J. W. & Smith, M. P., 2001, BAAS, 33, 1465 Google Scholar
Sharp, R. et al., 2006, in Proc. SPIE 6269, Ground-Based and Airborne Instrumentation for Astronomy, Eds. McLean, I. S. & Masanori, I., 62690GGoogle Scholar
Sneden, C., 1973, PhD Thesis, University of Texas at Austin Google Scholar
Wylie, E. C., Cottrell, P. L., Sneden, C. A. & Lattanzio, J. C., 2006, ApJ, 649, 248 CrossRefGoogle Scholar