Abundances in globular cluster red giants. II - M92 and M15

Fluorine Abundance Variations in Red Giants of the Globular Cluster M4 and Early-Cluster Chemical Pollution

We present fluorine abundances in seven red-giant members of the globular cluster M4 (NGC 6121). These abundances were derived from the HF (1–0) R9 line at 2.3357μm in high-resolution infrared spectra obtained with the Phoenix spectrograph on Gemini-South. Many abundances in the target stars have been studied previously, so that their overall abundance distributions are well-mapped. The abundan...

Nearby Spiral Galaxy Globular Cluster Systems II : Globular Cluster Abundances in NGC 300

We present new metallicity estimates for globular cluster candidates in the Sd spiral NGC 300, one of the nearest spiral galaxies outside the Local Group. We have obtained optical spectroscopy for 44 Sculptor Group globular cluster candidates with the Boller and Chivens (B&C) spectrograph on the Baade Telescope at Las Campanas Observatory. Nine of these objects appear to be genuine old globular...

Carbon abundances and 12 C / 13 C from globular cluster giants

The behaviour of the ∆ν=2 CO bands around 2.3 μm was examined by comparing observed and synthetic spectra in stars in globular clusters of different metallicity. Changes in the C/C isotopic ratio and the carbon abundances were investigated in stars from 3500–4900 K in the galactic globular clusters M71, M5, M3 and M13, covering the metallicity range from –0.7 to –1.6. We found relatively low ca...

The Spatial Distribution of the Red Giants in the Distant Galactic Globular Cluster Cluster NGC2419

Se p 19 99 Chemical Abundances of Bright Giants in the Mildly Metal - Poor Globular Cluster

We present a chemical composition analysis of three dozen giant stars in the nearby “CN-bimodal” mildly metal-poor (<[Fe/H]> = -1.18) globular cluster M4. The analysis combined traditional spectroscopic abundance methods with modifications to the line-depth ratio technique pioneered by Gray (1994). Silicon and aluminum are found to be primordially overabundant by factors exceeding the mild over...