The dynamics of the globular cluster M22 (NGC 6656)

2019 ◽  
Vol 14 (S351) ◽  
pp. 422-425
Author(s):  
D. Chen ◽  
L. Chen ◽  
J. J. Wang

AbstractWe have used the Hubble Space Telescope (HST) observations to measure proper motion of the globular cluster NGC 6656 (M22) with respect to the background bulge stars and its internal velocity dispersion profile. Based on the proper motion of the clusters, its space velocity and orbit are also calculated. The central velocity dispersion in radial and tangential components of the internal motion of cluster stars is 16.99 km s−1. We derive the mass-to-light ratio M/LV∼3.3 ± 0.2 which is relatively higher than the previous works.

2008 ◽  
Vol 4 (S252) ◽  
pp. 269-270
Author(s):  
Chen Ding

AbstractWe have used the Hubble Space Telescope (HST) to measure proper motion of the globular cluster NGC 6656 (M22) with respect to the background bulge stars and its internal velocity dispersion profile. With the space velocity of (Π, Θ, W) = (184±3, 209±14, 132±15) km s−1, we also calculate the orbit of the cluster. The central velocity dispersion in both components of the proper motion of cluster stars is 16.99 km s−1. We derive the mass-to-ration (M/L)∼1.7 which is relatively higher than the past works.


2018 ◽  
Vol 861 (2) ◽  
pp. 99 ◽  
Author(s):  
Mattia Libralato ◽  
Andrea Bellini ◽  
Roeland P. van der Marel ◽  
Jay Anderson ◽  
Laura L. Watkins ◽  
...  

1994 ◽  
Vol 107 ◽  
pp. 1745 ◽  
Author(s):  
Brian Yanny ◽  
Puragra Guhathakurta ◽  
John N. Bahcall ◽  
Donald P. Schneider

2019 ◽  
Vol 488 (3) ◽  
pp. 3857-3865
Author(s):  
L R Bedin ◽  
M Salaris ◽  
J Anderson ◽  
M Libralato ◽  
D Apai ◽  
...  

ABSTRACT We report on the white dwarf (WD) cooling sequence of the old globular cluster NGC 6752, which is chemically complex and hosts a blue horizontal branch. This is one of the last globular cluster WD cooling sequences accessible to imaging by the Hubble Space Telescope. Our photometry and completeness tests show that we have reached the peak of the luminosity function of the WD cooling sequence, at a magnitude mF606W  = 29.4 ± 0.1, which is consistent with a formal age of ∼14 Gyr. This age is also consistent with the age from fits to the main-sequence turn-off (13–14 Gyr), reinforcing our conclusion that we observe the expected accumulation of WDs along the cooling sequence.


2010 ◽  
Vol 513 ◽  
pp. A16 ◽  
Author(s):  
R. H. H. Huang ◽  
W. Becker ◽  
P. D. Edmonds ◽  
R. F. Elsner ◽  
C. O. Heinke ◽  
...  

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