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• W2047559799 startingPage "2264" @default.
• W2047559799 abstract "We present the results of our ongoing radial-velocity (RV) survey of the old (7 Gyr) open cluster NGC 188. Our WIYN 3.5 m data set spans a time baseline of 11 years, a magnitude range of 12 ⩽ V ⩽ 16.5 (1.18–0.94 M☉), and a 1° diameter region on the sky. With the addition of a Domain Astrophysical Observatory data set we extend our bright limit to V = 10.8 and, for some stars, extend our time baseline to 35 years. Our magnitude limits include solar-mass main-sequence stars, subgiants, giants, and blue stragglers (BSs), and our spatial coverage extends radially to 17 pc (∼13 core radii). For the WIYN data we present a detailed description of our data reduction process and a thorough analysis of our measurement precision of 0.4 km s−1 for narrow-lined stars. We have measured radial velocities for 1046 stars in the direction of NGC 188, and have calculated RV membership probabilities for stars with ⩾3 measurements, finding 473 to be likely cluster members. We detect 124 velocity-variable cluster members, all of which are likely to be dynamically hard-binary stars. Using our single member stars, we find an average cluster radial velocity of −42.36 ± 0.04 km s−1. We use our precise RV and proper-motion membership data to greatly reduce field-star contamination in our cleaned color–magnitude diagram, from which we identify six stars of note that lie far from a standard single-star isochrone. We present a detailed study of the spatial distribution of cluster-member populations, and find the binaries to be centrally concentrated, providing evidence for the presence of mass segregation in NGC 188. We observe the BSs to populate a bimodal spatial distribution that is not centrally concentrated, suggesting that we may be observing two populations of BSs in NGC 188, including a centrally concentrated distribution as well as a halo population. Finally, we find NGC 188 to have a global RV dispersion of 0.64 ± 0.04 km s−1, which may be inflated by up to 0.23 km s−1 from unresolved binaries. When corrected for unresolved binaries, the NGC 188 RV dispersion has a nearly isothermal radial distribution. We use this mean-corrected velocity dispersion to derive a virial mass of 2300 ± 460 M☉ ." @default.
• W2047559799 created "2016-06-24" @default.
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• W2047559799 date "2008-05-13" @default.
• W2047559799 modified "2023-10-17" @default.
• W2047559799 title "WIYN OPEN CLUSTER STUDY. XXXII. STELLAR RADIAL VELOCITIES IN THE OLD OPEN CLUSTER NGC 188" @default.
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• W2047559799 doi "https://doi.org/10.1088/0004-6256/135/6/2264" @default.
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