naa a22 4500 510732054 CHVBK 20180411082956.0 cr unu---uuuuu 180411e20130601xx s 000 0 eng 10.1134/S1063772913060061 doi (NATIONALLICENCE)springer-10.1134/S1063772913060061 Modeling and analysis of the spectrum of the globular cluster NGC 2419 [Elektronische Daten] [M. Sharina, V. Shimansky, E. Davoust] The properties of the stellar population of the unusual object NGC 2419 are studied; this is the most distant high-mass globular cluster of the Galaxy's outer halo, and a spectrum taken with the 1.93-m telescope of the Haute Provence Observatory displays elemental abundance anomalies. Since traditional high-resolution spectroscopicmethods are applicable to bright stars only, spectroscopic information for the cluster's stellar population as a whole, integrated along the spectrograph slit placed in various positions, is used. Population synthesis is carried out for the spectrum of NGC 2419 using synthetic spectra calculated from a grid of stellar model atmospheres, based on the theoretical isochrone from the literature that best fits the color-magnitude diagram of the cluster. The derived age (12.6 billion years), metallicity ([Fe/H] = −2.25 dex), and abundances of helium (Y = 0.26) and other chemical elements (a total of 14) are in a good qualitative agreement with estimates from the literature made from high-resolution spectra of eight red giants in the cluster. The influence on the spectrum of deviations from local thermodynamic equilibrium is considered for several elements. The derived abundance of α-elements ([α/Fe] = 0.13 dex, as the mean of [O/Fe], [Mg/Fe], and [Ca/Fe]) differs from the mean value in the literature ([α/Fe] = 0.4 for the eight brightest red giants) and may be explained by recently discovered in NGC2419 large [a/Fe] dispersion. Further studies of the integrated properties of the stellar population in NGC 2419 using higher-resolution spectrographs in various wavelength ranges should help improve our understanding of the cluster's chemical anomalies. Pleiades Publishing, Ltd., 2013 Sharina M. Special Astrophysical Observatory, Russian Academy of Sciences, 369167, Nizhnii Arkhyz, Karachai-Cherkessian Republic, Russia aut Shimansky V. Kazan (Volga Region) Federal University, ul. Kremlevskaya 18, 420008, Kazan, Russia aut Davoust E. Research Institute for Astrophysics and Planetology, National Center for Scientific Research and Toulouse University, av. du Colonel Roche 9, 31028, Toulouse Cedex 4, France aut Astronomy Reports SP MAIK Nauka/Interperiodica 57/6(2013-06-01), 410-422 1063-7729 57:6<410 2013 57 11444 https://doi.org/10.1134/S1063772913060061 text/html Onlinezugriff via DOI 1 research-article jats NATIONALLICENCE 856 40 https://doi.org/10.1134/S1063772913060061 text/html Onlinezugriff via DOI NATIONALLICENCE 700 1- Sharina M. Special Astrophysical Observatory, Russian Academy of Sciences, 369167, Nizhnii Arkhyz, Karachai-Cherkessian Republic, Russia aut NATIONALLICENCE 700 1- Shimansky V. Kazan (Volga Region) Federal University, ul. Kremlevskaya 18, 420008, Kazan, Russia aut NATIONALLICENCE 700 1- Davoust E. Research Institute for Astrophysics and Planetology, National Center for Scientific Research and Toulouse University, av. du Colonel Roche 9, 31028, Toulouse Cedex 4, France aut NATIONALLICENCE 773 0- Astronomy Reports SP MAIK Nauka/Interperiodica 57/6(2013-06-01), 410-422 1063-7729 57:6<410 2013 57 11444 Metadata rights reserved Springer special CC-BY-NC licence nationallicence BK010053 XK010053 XK010000 NATIONALLICENCE NATIONALLICENCE NL-springer