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The GOTHAM survey: chemical evolution of Milky Way globular clusters

Published online by Cambridge University Press:  02 August 2018

Bruno Dias Open the ORCID record for Bruno Dias [Opens in a new window] ,
Beatriz Barbuy ,
Ivo Saviane ,
Enrico V. Held ,
Gary Da Costa ,
Sergio Ortolani  and
Marco Gullieuszik
Bruno Dias
Affiliation:
European Southern Observatory, Alonso de Cordova 3107, Santiago, Chile email: bdias@eso.org
Beatriz Barbuy
Affiliation:
Universidade de São Paulo, Dept. de Astronomia, Rua do Matão 1226, São Paulo 05508-090, Brazil
Ivo Saviane
Affiliation:
European Southern Observatory, Alonso de Cordova 3107, Santiago, Chile email: bdias@eso.org
Enrico V. Held
Affiliation:
INAF, Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
Gary Da Costa
Affiliation:
Research School of Astronomy & Astrophysics, Australian National University, Mount Stromlo Observatory, via Cotter Road, Weston Creek, ACT 2611, Australia
Sergio Ortolani
Affiliation:
INAF, Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy Università di Padova, Dipartimento di Astronomia, Vicolo dell’Osservatorio 2, 35122 Padova, Italy
Marco Gullieuszik
Affiliation:
INAF, Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
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Abstract

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Milky Way globular clusters are excellent laboratories for stellar population detailed analysis that can be applied to extragalactic environments with the advent of the 40m-class telescopes like the ELT. The globular cluster population traces the early evolution of the Milky Way which is the field of Galactic archaeology. We present our GlObular clusTer Homogeneous Abundance Measurement (GOTHAM) survey. We derived radial velocities, Teff, log(g), [Fe/H], [Mg/Fe] for red giant stars in one third of all Galactic globular clusters that represent well the Milky Way globular cluster system in terms of metallicity, mass, reddening, and distance. Our method is based on low-resolution spectroscopy and is intrinsically reddening free and efficient even for faint stars. Our [Fe/H] determinations agree with high-resolution results to within 0.08 dex. The GOTHAM survey provides a new metallicity scale for Galactic globular clusters with a significant update of metallicities higher than [Fe/H] > -0.7. We show that the trend of [Mg/Fe] with metallicity is not constant as previously found, because now we have more metal-rich clusters. Moreover, peculiar clusters whose [Mg/Fe] does not match Galactic stars for a given metallicity are discussed. We also measured the CaII triplet index for all stars and we show that the different chemical evolution of Milky Way open clusters, field stars, and globular clusters implies different calibrations of calcium triplet to metallicity.

Keywords

surveysstars: abundancesstars: Population IIGalaxy: abundancesGalaxy: bulgeGalaxy: haloglobular clusters: generalglobular clusters: individual (NGC 104, 2298, 2808, 3201, 4372, 4590, 5634, 5694, 5824, 5897, 5904, 5927, 5946, 6121, 6171, 6254, 6284, 6316, 6356, 6355, 6352, 6366, 6401, 6397, 6426, 6440, 6441, 6453, 6528, 6539, 6553, 6558, 6569, 6656, 6749, 6752, 6838, 6864, 7006, 7078, Pal 6, 10, 11, 14, Rup 106, BH 176, Lynga 7, HP 1, Djorg 2, IC 1276, Terzan 8)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 25 - 28
Copyright
Copyright © International Astronomical Union 2018 

References

Barbuy, B., Perrin, M.-N., Katz, D., et al. 2003, A&A, 404, 661Google Scholar
Carretta, E., Bragaglia, A., Gratton, R., & Lucatello, S., 2009, A&A, 505, 139Google Scholar
Coelho, P., Barbuy, B., Meléndez, J., Schiavon, R. P., & Castilho, B. V., 2005, A&A, 443, 735Google Scholar
Da Costa, G. S., Held, E. V., Saviane, I., & Gullieuszik, M., 2009, ApJ, 705, 1481Google Scholar
Da Costa, G. S., Norris, J. E., & Yong, D., 2013, ApJ, 769, 8Google Scholar
Dias, B., Barbuy, B., Saviane, I., et al. 2015, A&A, 573, A13Google Scholar
Dias, B., Barbuy, B., Saviane, I., et al. 2016a, A&A, 590, A9Google Scholar
Dias, B., Saviane, I., Barbuy, B., et al. 2016b, The Messenger, 165, 19Google Scholar
Muñoz, C., Geisler, D., & Villanova, S., 2013, MNRAS, 433, 2006Google Scholar
Saviane, I., da Costa, G. S., Held, E. V., et al. 2012a, A&A, 540, A27Google Scholar
Saviane, I., Held, E. V., Da Costa, G. S., et al. 2012b, The Messenger, 149, 23Google Scholar
Villanova, S., Geisler, D., Carraro, G., Moni Bidin, C., & Muñoz, C., 2013, ApJ, 778, 186Google Scholar