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Blue Stragglers: Spectra of Globular Clusters

Published online by Cambridge University Press:  13 April 2010

A. J. Cenarro ,
J. L. Cervantes ,
M. A. Beasley ,
A. Marin-Franch  and
A. Vazdekis
A. J. Cenarro
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea s/n, E-38200 La Laguna, Tenerife, Spain email: [email protected] Centro de Estudios de Física del Cosmos de Aragón, C/ General Pizarro 1, E-44001 Teruel, Spain
J. L. Cervantes
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea s/n, E-38200 La Laguna, Tenerife, Spain email: [email protected]
M. A. Beasley
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea s/n, E-38200 La Laguna, Tenerife, Spain email: [email protected]
A. Marin-Franch
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea s/n, E-38200 La Laguna, Tenerife, Spain email: [email protected]
A. Vazdekis
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea s/n, E-38200 La Laguna, Tenerife, Spain email: [email protected]
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Abstract

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The integrated Balmer lines of unresolved stellar systems have been widely used as age indicators, since they are sensitive to the temperature of the main sequence turn-off. However, the existence of “non-canonical” stellar stages such as hot horizontal branch stars and blue straggler stars (BSSs) can lead to underestimations of the true stellar population ages. Using an optimized Hβ index in conjunction with HST/WFPC2 color-magnitude diagrams (CMDs), we find that Galactic globular clusters of similar metallicity exhibit a large scatter in their Hβ strengths, which does not correlate with their CMD-derived ages. Instead, we demonstrate that the specific frequency of BSSs is responsible for the observed Hβ scatter at intermediate-to-high metallicity, in the sense that, at fixed metallicity, higher BSS ratios lead to larger integrated Hβ strengths. Therefore, the specific frequency of BSSs sets a fundamental limit on the accuracy for which integrated spectroscopic ages can be determined for globular clusters and, probably, other stellar systems like galaxies. The observational implications of this result are discussed.

Keywords

blue stragglers — globular clusters: general — galaxies: star clusters — galaxies: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 23 - 26
Copyright
Copyright © International Astronomical Union 2010

References

Alonso, A., Arribas, S., & Martínez-Roger, C. 1996, A&A, 313, 873Google Scholar
Cenarro, A. J., Peletier, R. F., Sńchez-Blzquez, P., Selam, S. O., Toloba, E., Cardiel, N., Falcón-Barroso, J., Gorgas, J., Jiménez-Vicente, J., & Vazdekis, A. 2007a, MNRAS, 374, 664CrossRefGoogle Scholar
Cenarro, A. J., Beasley, M. A., Strader, J., Brodie, J. P., & Forbes, D. A. 2007b, AJ, 134, 391CrossRefGoogle Scholar
Cenarro, A. J., Cervantes, J.L., Beasley, M. A., Marin-Franch, A., & Vazdekis, A., 2008, ApJ, 689L, 29CrossRefGoogle Scholar
Cervantes, J. L. & Vazdekis, A. 2009, MNRAS, 391, 691CrossRefGoogle Scholar
Davies, M. B., Benz, W., & Hills, J. G. 1994, ApJ, 424, 870CrossRefGoogle Scholar
Harris, W. E. 1996, AJ, 112, 1487CrossRefGoogle Scholar
Lee, H., Yoon, S., & Lee, Y. 2000, AJ, 120, 998CrossRefGoogle Scholar
Mapelli, M., Ripamonti, E., Tolstoy, E., Sigurdsson, S., Irwin, M. J., & Battaglia, G. 2007, MNRAS, 380, 1127CrossRefGoogle Scholar
McCrea, W. H. 1964, MNRAS, 128, 147CrossRefGoogle Scholar
Momany, Y., Held, E. V., Saviane, I., Zaggia, S., Rizzi, L., & Gullieuszik, M. 2007, A&A, 468, 973Google Scholar
Moretti, A., De Angeli, F., & Piotto, G. 2008, A&A, 483, 183 (M08)Google Scholar
Piotto, et al. 2002, A&A, 391, 945Google Scholar
Puzia, T. H., Kissler-Patig, M., Thomas, D., Maraston, C., Saglia, R. P., Bender, R., Goudfrooij, P., & Hempel, M., 2005, A&A, 439, 997Google Scholar
Rose, J. A. 1985, AJ, 90, 1927CrossRefGoogle Scholar
Sánchez-Blázquez, P., Peletier, R. F., Jiménez-Vicente, J., Cardiel, N., Cenarro, A. J., Falcón-Barroso, J., Gorgas, J., Selam, S., & Vazdekis, A. 2006, MNRAS, 371, 703CrossRefGoogle Scholar
Schiavon, R. P., Rose, J. A., Courteau, S., & MacArthur, L. A. 2004, ApJ, 608, 33CrossRefGoogle Scholar
Schiavon, R. P., Rose, J. A., Courteau, S., & MacArthur, L. A. 2005, ApJS, 160, 163 (S05)CrossRefGoogle Scholar
Trager, S. C., Worthey, G., Faber, S. M., & Dressler, A. 2005, MNRAS, 362, 2CrossRefGoogle Scholar
Vazdekis, A., Salaris, M., Arimoto, N., & Rose, J. A. 2001, ApJ, 549, 274CrossRefGoogle Scholar
Vazdekis, A., Sánchez-Blázquez, P., Falcón-Barroso, J., Cenarro, A. J., Beasley, M. A., Cardiel, N., Gorgas, J., & Peletier, R., 2009, MNRAS, submitted, arXiv:XXXXGoogle Scholar
Vazdekis, A., Cenarro, A. J., Gorgas, J., Cardiel, N., & Peletier, R. F. 2003, MNRAS, 340, 1317CrossRefGoogle Scholar