GS100-02-41: a new large HI shell in the outer part of the Galaxy

TL;DR

This study characterizes a large HI shell in the outer Galaxy, analyzing its origin, evolution, and potential role in triggering star formation, using multi-wavelength data including HI, radio continuum, and infrared observations.

Contribution

It provides a detailed multi-wavelength analysis of the large HI shell GS100-02-41, proposing its origin from massive stars in Cep OB1 and suggesting a role in star formation processes.

Findings

The HI shell is expanding with a velocity range from -29 to -51.7 km/s.

No continuum counterpart of the HI shell was found, but three thermal radio sources are associated with it.

The shell's origin is likely due to the action of massive stars in Cep OB1.

Abstract

Massive stars have a profound effect on the surrounding interstellar medium. They ionize and heat the neutral gas, and due to their strong winds, they swept the gas up forming large HI shells. In this way, they generate a dense shell where the physical conditions for the formation of new stars are given. The aim of this study is to analyze the origin and evolution of the large HI shell GS100-02-41 and its role in triggering star forming processes.To characterize the shell and its environs, we carry out a multi-wavelength study. We analyze he HI 21 cm line, the radio continuum, and infrared emission distributions. The analysis of the HI data shows an expanding shell structure centred at (l, b) = (100.6 deg, -2.04 deg) in the velocity range from -29 to -51.7 km/s. We infer for GS100-02-41, a kinematical distance of 2.8 +/- 0.6 kpc. Several massive stars belonging to Cep OB1 are located in projection within the large HI, shell boundaries. The analysis of the radio continuum and infrared data reveal that there is no continuum counterpart of the HI shell. On the other hand, three slightly extended radio continuum sources are observed in projection onto the dense HI shell. From their flux density determinations we infer that they are thermal in nature. An analysis of the HI emission distribution in the environs of these sources shows, for each of them, a region of low emissivity having a good morphological correlation with the ionized gas in a velocity range similar to the one where GS100-02-41 is detected. The origin of GS100-02-41 could have been mainly due to the action of the Cep OB1 massive stars located inside the HI shell. The obtained age difference between the HI shell and the HII regions, together with their relative location, led us to conclude that the ionizing stars could have been created as a consequence of the shell evolution.