A study of the ISM with large massive-star optical spectroscopic surveys

TL;DR

This study analyzes optical spectra from massive-star surveys to investigate the interstellar medium's properties, focusing on diffuse interstellar bands and interstellar lines, providing a comprehensive dataset within 3 kpc of the Sun.

Contribution

It combines intermediate and high-resolution spectroscopic data to create the most extensive collection of optical ISM information within 3 kpc, enabling detailed correlation analysis.

Findings

Identification of correlations between DIBs and interstellar lines.

Insights into the origins of DIBs based on spectral analysis.

Enhanced understanding of ISM properties near the Sun.

Abstract

We are conducting a study on the imprint of the ISM on optical spectra based on two types of ongoing spectroscopic massive-star surveys: on the one hand, intermediate-resolution (R = 2500) green-blue spectra for ~3000 stars obtained with the Galactic O Star Spectroscopic Survey (GOSSS). On the other hand, high-resolution (R = 23 000 - 65 000) optical spectra for 600 stars obtained from three different surveys, OWN, IACOB, and NoMaDS. The R = 2500 data allows us to reach a larger sample with an average larger extinction while the R = 23 000 - 65 000 sample provides access to more diffuse interstellar bands (DIBs) and allows for the resolution in velocity of some ISM features. For each spectrum we are measuring the equivalent widths, FWHMs, and central wavelengths of 10-40 DIBs and interstellar lines (e.g. Ca II H+K, Na I D1+D2) and, in the case of GOSSS, the existence of an H II region around the star. We have also derived from auxiliary data or compiled from the literature values for the reddening, extinction law, H I column density, parallax, and H alpha emission. All of this constitutes the most complete collection ever of optical information on the ISM within 3 kpc of the Sun. We are analyzing the correlations between all of the collected quantities to discriminate between different possible origins of the DIBs.