A spectroscopic study of the Open Cluster NGC 6475 (M 7) Chemical Abundances from stars in the range T = 4500-10000 K

TL;DR

This study analyzes the chemical abundances of stars in the open cluster NGC 6475 across a wide temperature range using high-resolution spectroscopy, applying different methodologies for hot and cool stars to improve cluster parameter estimates.

Contribution

It applies tailored spectroscopic methods to stars of varying temperatures in NGC 6475, providing a comprehensive chemical abundance analysis and more robust cluster parameters.

Findings

Determined chemical abundances for multiple elements in NGC 6475 stars.

Established consistency between different stellar types' abundance measurements.

Refined fundamental parameters of the cluster.

Abstract

Clusters of stars are key objects for the study of the dynamical and chemical evolution of the Galaxy and its neighbors. In particular chemical composition is obtained from different kinds of stars (hot main-sequence stars, cool main-sequence stars, horizontal-branch stars, RGB stars) using different methodologies. Our aim is to apply these methodologies to the stars of the Open Cluster NGC 6475. Obtaining a census of the most important elements we will be able to test their consistence. We finally want to establish more robust fundamental parameters for this cluster.We selected high S/N high resolution spectra of 7 stars of the Open Cluster NGC 6475 from the ESO database covering the T$_{\rm eff}$ range 4500-10000 K and of luminosity class V (dwarf) and III (giants). We determined the chemical abundances of several elements. For hot stars (T$_{\rm eff}$$>$9000 K) we applied the Balmer Lines fitting method to obtained atmospheric parameters. For cool stars (T$_{\rm eff}$$<$6500 K) we used the FeI/II abundance equilibrium method. For the two groups of stars the use of different line-lists was mandatory. LTE approximation was used. For elements affected by NLTE deviation (C,N,O,Na,Mg) corrections were applied. The abundance of many elements were obtained from the measurement of the equivalent width of spectral lines. For those elements for which only blended lines were available (O, He) comparison of real spectrum with synthetic ones was used. Hyperfine structure was taken in account for V and Ba.