Understanding the mechanisms triggering the formation of massive SCs is one of the primary goals of contemporary astrophysics. Young embedded SCs presently undergoing star formation have been discovered in dense molecular clouds. Because of the enormous extinction and density of matter near the Galactic plane and because of their loose structure, OCs have only been studied within a radius of R gc ~8 kpc from the Sun (Kharchenko et al. They are generally less massive and more metal-rich than GCs and lose stars from tidal interactions with the interstellar medium. Open clusters (OCs) reside in the thin disk. The high-metallicity GCs ( > − 0.4 dex) belong to the bulge or the thick disk, but their origin is still an open subject. The old globular clusters (GCs), which populate galactic haloes, were enriched in α-elements during their formation due to explosions of SNeII (Kruijssen & Diederik, and references therein). SCs are prime targets for improving our understanding of stellar evolution using deep colour–magnitude diagrams (CMD) and high-resolution spectroscopy. The age, distance, and metal content of SCs can be determined more easily than for single stars. The knowledge of their chemical, structural, and dynamical properties is indispensable for understanding how the Galaxy formed and how much dwarf satellites contributed to its formation. Star clusters (SCs) are important tracers of the evolutionary history of our Galaxy. It may have originated as a massive star cluster after the encounter of the forming thin disk with a high-velocity gas cloud or as a satellite dwarf galaxy.īased on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência, Tecnologia e Inovação (Brazil), and the Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina). BH176 is a member of old Galactic open clusters that presumably belong to the thick disk. We determine the following parameters for BH176: V h = 0 ± 15 km s -1, = −0.1 ± 0.1, age 7 ± 0.5 Gyr, E( V − I) = 0.79 ± 0.03, distance 15.2 ± 0.2 kpc, α-element abundance ~ 0.25 dex (the mean of, and ).Ĭonclusions. We derive radial velocities, metallicities, effective temperatures, and surface gravities of the observed stars and use these parameters to distinguish member stars from field objects. We present medium-resolution observations of red clump and red giant branch stars in BH176 obtained with the Gemini South Multi-Object Spectrograph. The best way to reach this goal is to combine spectroscopic and photometric methods. Our aim is to determine the origin of this unique object by accurately determining its distance, metallicity, and age. It is larger in size and more distant from the Galactic plane than typical open clusters, and it does not belong to the Galactic bulge.Īims. It is spatially and kinematically consistent with belonging to the Monoceros Ring. des Maillettes, 1290 Versoix, 12 February 2014Ĭontext. Belin, 31400 Toulouse, Kazan Federal University, Kremlevskaya 18, 420008 Kazan, Geneva Observatory, University of Geneva, 51 Ch. Arkhyz, KChR, 369167, Instituto de Astronomía Teórica y Experimental IATE, CONICET − Observatorio Astronómico, Universidad Nacional de Córdoba, Laprida 854, X5000BGR Córdoba, IRAP, Université de Toulouse, CNRS, 14 avenue E. Charbonnel 5ġ Special Astrophysical Observatory, Russian Academy of Sciences, N. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
0 Comments
Leave a Reply. |
AuthorWrite something about yourself. No need to be fancy, just an overview. ArchivesCategories |