Análisis del gas molecular presente en la zona de colisión de cáscaras y supercáscaras de H I

Abstract

The H I shells and supershells are structures detected in the H I emission distribution as minima surrounded by walls of enhanced emission. It is believed that their expansion and collision can induce the formation of molecular gas in the collision zones that are compressed, but there exist few observational examples of this phenomenon. In this work, we search for evidence of molecular gas that could have been created for the action of shell and supershell collisions. Based on H I data from the HI4PI survey in a rectangular area of ∼ 5° per side, centered at (l, b) = (107°, -3°), several shells and supershells were detected in the velocity range between -45 and -67 km s-1 that could be in collision. Using CO emission data obtained from the FCRAO survey, we have identified molecular gas in the collision zone of the shells and supershells. In this work, we present a preliminary study on the characteristics of the H I structures and of the molecular clouds present in this region of the Galaxy.