Investigating chemical variations between interstellar gas clouds in the solar neighbourhood

¹ Department of Astronomy, University of Geneva, Chemin Pegasi 51, Versoix, Switzerland
² European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
³ Université Claude Bernard Lyon 1, Centre de Recherche Astrophysique de Lyon UMR5574, 9 Av. Charles André, 69230 Saint-Genis-Laval, France
⁴ French-Chilean Laboratory for Astronomy (FCLA), CNRS-IRL3386, U. de Chile, Camino el Observatorio 1515, Casilla 36-D, Santiago, Chile
⁵ European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago, Chile
⁶ Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544-1001, USA
⁷ AURA for ESA, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
⁸ Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA
⁹ Institute of Astronomy, Kharkiv National University, 4 Svobody Sq., Kharkiv 61022, Ukraine

^★ Corresponding author; tanita.ramburuth-hurt@unige.ch

Received: 31 July 2024
Accepted: 31 January 2025

Abstract

The interstellar medium (ISM) is a fundamental component of the Milky Way. Studying its chemical composition and the level of its chemical diversity gives us insight into the evolution of the Milky Way and the role of gas in the Galactic environment. In this study we used a novel simulation technique to model the distribution of total hydrogen between gas components and, therefore, derive new constraints on the dust depletion and metallicity. We studied individual gas components along the lines of sight towards eight bright O/B stars within 1.1 kpc of the Sun using high-resolution HST/STIS absorption spectra (R ∼ 114 000). We measured the level of dust depletion for these individual components and find components with higher levels of dust depletion compared to Milky Way sightlines in the literature. We find large ranges in the level of dust depletion among components along lines of sight, up to a factor of 15 (or 1.19 dex). Although it is not possible to directly measure the metallicity of individual components due to the saturated and damped Lyman-α line, we investigated possible metallicity ranges for individual gas components by exploring many different distributions of the total hydrogen gas between components. We selected possible combinations of these gas fractions that produce the minimum metallicity difference between components, and for these cases we determine individual metallicities to accuracies that range between ∼ 0.1 and 0.4 dex. This work shows that full line-of-sight analyses do not capture the level of diversity along lines of sight, and that component-by-component studies give a more in-depth understanding of the chemical intricacies of the ISM.