Deep infrared array photometry of globular clusters. 3: M13

1995 ◽  
Vol 445 ◽  
pp. 211 ◽  
Author(s):  
T. J. Davidge ◽  
W. E. Harris
1996 ◽  
Vol 468 ◽  
pp. 641 ◽  
Author(s):  
T. J. Davidge ◽  
Patrick Cote ◽  
W. E. Harris

1995 ◽  
Vol 109 ◽  
pp. 1154 ◽  
Author(s):  
Jay A. Frogel ◽  
Leslie E. Kuchinski ◽  
Glenn P. Tiede

1995 ◽  
Vol 109 ◽  
pp. 1131 ◽  
Author(s):  
Leslie E. Kuchinski ◽  
Jay A. Frogel ◽  
D. M. Terndrup ◽  
S. E. Persson

1995 ◽  
Vol 454 ◽  
pp. 545
Author(s):  
T. J. Davidge ◽  
W. E. Harris

1994 ◽  
Vol 435 ◽  
pp. 207 ◽  
Author(s):  
T. J. Davidge ◽  
D. A. Simons

1996 ◽  
Vol 462 ◽  
pp. 255 ◽  
Author(s):  
T. J. Davidge ◽  
W. E. Harris

1994 ◽  
Vol 423 ◽  
pp. 640 ◽  
Author(s):  
T. J. Davidge ◽  
D. A. Simons

1997 ◽  
Vol 475 (2) ◽  
pp. 584-593 ◽  
Author(s):  
T. J. Davidge ◽  
W. E. Harris

1988 ◽  
Vol 132 ◽  
pp. 525-530
Author(s):  
Raffaele G. Gratton

The use CCD detectors has allowed a major progress in abundance derivations for globular cluster stars in the last years. Abundances deduced from high dispersion spectra now correlates well with other abundance indicators. I discuss some problems concerning the derivation of accurate metal abundances for globular clusters using high dispersion spectra from both the old photographic and the most recent CCD data. The discrepant low abundances found by Cohen (1980), from photographic material for M71 giants, are found to be due to the use of too high microturbulences.


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