Abstract
The differences in the relationships between the physical parameters and the chemical-element abundances in accreted globular star clusters and those formed inside the Galaxy have been investigated. The information on the supposed formation sites of the clusters based on the Gaia DR2 data is borrowed from the literature. Those sources estimate the probability of belonging to the Galactic bulge and disk, as well as to six known events of the merger of dwarf satellite galaxies with the Milky Way, for 151 globular clusters. Orbital elements, initial masses, population types, and ages are taken from the literature; the data on the chemical composition for 69 globular clusters of the Galaxy are taken from the authors’ compiled catalog. It is shown that all metal-poor (\([{\text{Fe/H}}] < - 1.0\)) genetically related globular clusters have high relative abundances of \(\alpha \)‑elements. According to modern views, since type II supernovae release more \(\alpha \)-elements into the interstellar medium with increasing mass, it has been suggested that masses of type II supernovae in the Galaxy were greater than in the accreted galaxies. It is proved that the clusters of the low-energy group, which were considered accreted, are genetically related to a single protogalactic cloud, same as the unstratified clusters UKS 1 and Liller 1, which most likely belong to the bulge. It is shown that not only the lower but also the upper limits of the clusters’ masses decrease with an increase in the average radius of their orbits. The latter fact is explained by a decrease in the masses of emerging clusters with a decrease in the masses of their host galaxies. It is demonstrated that an extremely multicomponent stellar population is observed only in accreted globular clusters with an initial mass >106 \({{M}_{ \odot }}\). It has been suggested that these clusters retained all the matter ejected by their evolved stars, from which new generations of stars formed due to long evolution far from our Galaxy.
Similar content being viewed by others
REFERENCES
R. Ibata, G. Gilmore, and M. Irvin, Nature (London, U.K.) 370, 194 (1994).
J. T. Mackereth, R. P. Schiavon, J. Pfeffer, C. R. Hayes, et al., Mon. Not. R. Astron. Soc. 482, 3426 (2019).
A. Helmi, C. Babusiaux, H. H. Koppelman, D. Massari, J. Veljanoski, and A. G. A. Brown, Nature (London, U.K.) 563, 85 (2018).
D. Massari, H. H. Koppelman, and A. Helmi, Astron. Astrophys. 630, 4 (2019).
V. A. Marsakov, V. V. Koval’, and M. L. Gozha, Astron. Rep. 63, 274 (2019).
V. A. Marsakov, V. V. Koval’, and M. L. Gozha, Astrophys. Bull. 74, 404 (2019).
V. A. Marsakov, V. V. Koval’, and M. L. Gozha, Astrophys. Bull. 75, 21 (2020).
T. Bensby, S. Feldsing, and I. Lundstrem, Astron. A-strophys. 410, 527 (2003).
W. E. Harris, Astron. J. 112, 1487 (1996); arX-iv:1012.3224 [astro-ph.GA].
E. Carretta, in The General Assembly of Galaxy Halos: Structure, Origin and Evolution, Ed. by A. Bragaglia, M. Arnaboldi, M. Rejkuba, and D. Romano, Proc. IAU Symp. 317, 97 (2016).
J. Pritzl, K. A. Venn, and M. Irwin, Astron. J. 130, 2140 (2005).
K. A. Venn, M. Irwin, M. D. Shetrone, C. A. Tout, V. Hill, and E. Tolstoy, Astron. J. 128, 1177 (2004).
T. Bensby, S. Feltzing, and M. S. Oey, Astron. Astrophys. 562, 71 (2014).
D. A. VandenBerg, K. Brogaard, R. Leaman, and L. Casagrande, Astrophys. J. 775, 134 (2013).
E. Carretta, A. Bragaglia, R. Gratton, V. d’Orazi, and S. Lucatello, Astron. Astrophys. 508, 695 (2009).
A. F. Marino, A. P. Milone, A. Renzini, F. D’Antona, et al., Mon. Not. R. Astron. Soc. 487, 3815 (2019).
H. Baumgardt, M. Hilker, A. Sollima, and A. Bellini, Mon. Not. R. Astron. Soc. 482, 5138 (2019).
T. V. Borkova and V. A. Marsakov, Bull. SAO 54, 61 (2002).
R. Zinn, in The Globular Cluster-Galaxy Connection, Ed. by H. Smith and J. Brodee, ASP Conf. Ser. 48, 38 (1993).
G. S. da Costa and T. E. Armandroff, Astron. J. 109, 253 (1995).
V. A. Marsakov and T. V. Borkova, Astron. Lett. 32, 545 (2006).
P. E. Nissen and W. J. Schuster, Astron. Astrophys. 511, L10 (2010).
J. J. Cowan, C. Sneden, J. E. Lawler, A. Aprahamian, M. Wiescher, K. Langanke, G. Martinez-Pinedo, and F.-K. Thielemann, arXiv:1901.01410 [astro-ph.HE] (2010).
D. Horta, R. P. Schiavon, J. T. Mackereth, T. C. Beers, et al., Mon. Not. R. Astron. Soc. 493, 3363 (2020).
C. Travaglio, D. Galli, R. Gallino, M. Busso, F. Ferrini, and O. Straniero, Astrophys. J. 521, 691 (1999).
J. Köppen, C. Weidner, and P. Kroupa, Mon. Not. R. Astron. Soc. 375, 673 (2007).
J. Pritzl, K. A. Venn, and M. Irwin, Astron. J. 130, 2140 (2005).
S. L. J. Gibbons, V. Belokurov, and N. W. Evans, Mon. Not. R. Astron. Soc. 464, 794 (2017).
H. H. Koppelman, A. Helmi, D. Massari, A. M. Price-Whelan, and T. K. Starkenburg, Astron. Astrophys. 631, L9 (2019).
M. G. Abadi, J. F. Navarro, M. Steinmetz, and V. R. Eke, Astrophys. J. 591, 499 (2003).
ACKNOWLEDGMENTS
The authors are grateful to Davide Massari for providing the unpublished ages of the globular clusters and Holger Baumgardt for providing the updated initial globular cluster masses.
Funding
The research was funded by the Southern Federal University, 2020 (Ministry of Science and Higher Education of the Russian Federation).
Author information
Authors and Affiliations
Corresponding authors
Additional information
Translated by M. Chubarova
Rights and permissions
About this article
Cite this article
Marsakov, V.A., Koval’, V.V. & Gozha, M.L. Physical and Chemical Properties of Galactic Global Clusters with Various Origins Identified from the Gaia DR2 Data. Astron. Rep. 64, 805–814 (2020). https://doi.org/10.1134/S1063772920110062
Received:
Revised:
Accepted:
Published:
Issue Date:
DOI: https://doi.org/10.1134/S1063772920110062