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Mass Assembly and Chemical Complexity in the Milky Way

Pamela Klaassen, David Eden, Alessio Traficante, Henrik Beuther, Maite Beltrán, Caroline Bot, Elias Brinks, Laura Colzi, Timea Csengeri, Antoine Gusdorf, Doug Johnstone, Jes K. Jørgensen, Jonathan Marshall, Elena Redaelli, Víctor M. Rivilla, Thomas Stanke

Abstract

(Sub-)millimeter spectral lines can be used not only to understand the chemical complexity and enrichment history of an observed portion of our Galaxy, but with spectrally resolved lines, they reveal the physical conditions, dynamics, and even the ionisation state and magnetic field strengths of the gas component of our Galaxy. They are prime tracers of mass assembly and structure formation across scales.

Mass Assembly and Chemical Complexity in the Milky Way

Abstract

(Sub-)millimeter spectral lines can be used not only to understand the chemical complexity and enrichment history of an observed portion of our Galaxy, but with spectrally resolved lines, they reveal the physical conditions, dynamics, and even the ionisation state and magnetic field strengths of the gas component of our Galaxy. They are prime tracers of mass assembly and structure formation across scales.

Paper Structure

This paper contains 3 sections, 1 figure.

Table of Contents

  1. Mass Assembly from Large Scales to Small
  2. Technical Requirements

Figures (1)

  • Figure 1: Left: Current state of Galactic Plane Line surveys of a single species (CO). View modelled after Figure 1 of Schuller21 (Background Image Credit: R. Hurt [NASA/JPL/Caltech]). Right: What spectral lines could be detected homogeneously across the plane with large scale studies with next generation facilities.