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WFPC2 observations of the globular cluster M30
Yanny, Brian; Guhathakurta, Puragra; Schneider, Donald P.; Bahcall, John N.
AA(Inst. for Advanced Study, Princeton, NJ, US), AB(Inst. for Advanced Study, Princeton, NJ, US), AC(Inst. for Advanced Study, Princeton, NJ, US), AD(Inst. for Advanced Study, Princeton, NJ, US)
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 435, no. 1, p. L59-L62 (ApJL Homepage)
Publication Date:
NASA/STI Keywords:
Blue Stars, Globular Clusters, Radial Distribution, Color-Magnitude Diagram, Computerized Simulation, Hubble Space Telescope, Power Series, Stellar Luminosity
Bibliographic Code:


We describe images of the center of the dense globular cluster M30 (NGC 7099) obtained with the Hubble Space Telescope Wide Field/Planetary Camera 2 (HST WFPC2). Data taken in the F336W, F439W, and F555W filters (approximately U, B, and V) yield a color-magnitude diagram with photometric errors of 1 sigma = 0.05 mag for stars with V less than 17.5, and 1 sigma approximately 0.1 mag at V = 20, which is 1.5 mag fainter than the main-sequence turnoff. Simulations show that the star identifications are essentially complete for stars with V less than 19.5, even in the densest regions of the cluster. The projected radial distribution of stars can be represented by a power law distribution: N(r) approximately ralpha, with slope alpha = -0.4 +/- 0.15, into radii less than 0.4 sec (0.015 pc). The radial profile is also consistent with a flat core of any radius smaller than approximately 1.5 sec (0.05 pc), but inconsistent with any core radius larger than 2.5 sec (0.09 pc). A total of 30 blue straggler candidates within 20 sec of the cluster center have been identified from the three-color data. Their radial distribution is strongly centrally concentrated when compared to the horizontal branch, red giant branch, or main-sequence stars in the cluster. The abundance of blue stragglers (relative to red giants and subgiants) within r approximately less than 20 sec of the center of M30 is fBS = 0.19 =/- 0.04, about twice as high as in other dense clusters.

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