Ionized Gas Characteristics in the Cavities of the Gas and Dust Disc of the Spiral Galaxy NGC 6946

TL;DR

This study investigates ionized gas in NGC 6946's cavities, revealing foreground Galactic emission, shock excitation signs, and the relationship between dust morphology and ionized gas properties.

Contribution

It provides new insights into the ionized gas components in NGC 6946, distinguishing Galactic foreground emission from galaxy-specific features and analyzing shock excitation in cavities.

Findings

Ionized gas lines decompose into two components, one from the Milky Way's diffuse ionized gas.

Shock excitation signs are detected in the cavities of NGC 6946.

The morphology of warm dust and HI is nearly identical, with shock features observable in IR images.

Abstract

The parameters of the ionized gas in NGC 6946 (in the [NII]6548,6583, H-alpha and [SII]6717,6731 lines) are investigated with the SAO RAS BTA telescope along three positions of the long slit of the SCORPIO focal reducer, passing through a number of large and small cavities of the gaseous disc of the galaxy. Most of these cavities correspond exactly to the cavities in warm dust. We found that everywhere in the direction of NGC 6946 the lines of ionized gas are decomposed into two Gaussians, one of which shows almost constant [SII]/H-alpha and [NII]/H-alpha ratios, as well as an almost constant radial velocity within the measurement errors (about -35 - -50 km/s). This component is in fact the foreground radiation from the diffuse ionized gas of our Galaxy; a similar component is also present in the emission of neutral hydrogen. The analysis of the component of ionized gas, occurring in NGC 6946, has revealed that it shows signs of shock excitation in the cavities of the gaseous disc of the galaxy. It is as well typical for the extraplanar diffuse ionized gas (EDIG), observed in a number of spiral galaxies at their high Z-coordinates. This can most likely be explained by low density of the gas in the NGC 6946 disc (with the usual photoionization) inside the cavities, due to what we see the spectral features of the EDIG gas of NGC 6946, projected onto them. In the absence of separation of ionized gas into two components by radial velocities, there is an increasing contribution to the integral line parameters by the EDIG of our Galaxy when the gas density in NGC 6946 decreases, which explains some strange results, obtained in the previous studies. The morphology of warm dust, visible in the infrared range and HI is almost the same. The shock excitation of the ionized gas is detected also in the smallest holes, well distinguishable only in the IR images.