Star formation in isolated AMIGA galaxies: dynamical influence of bars

TL;DR

This study investigates how internal dynamics, especially bars, influence star formation in isolated galaxies by analyzing H-alpha emission, galaxy morphology, and gas-star interactions to understand secular evolution.

Contribution

It provides new insights into the role of bars and spiral structures in isolated galaxies, including their evolution and star formation patterns, supported by Fourier analysis and numerical simulations.

Findings

Barred and unbarred galaxies are equally common in isolation.

Star formation laws may differ from the classical Schmidt law in these environments.

Observed morphologies constrain galaxy evolution timescales.

Abstract

Star formation depends strongly both on the local environment of galaxies, and on the internal dynamics of the interstellar medium. To disentangle the two effects, we obtained, in the framework of the AMIGA project, Ha and Gunn r photometric data for more than 200 spiral galaxies lying in very low-density regions of the local Universe. We characterise the Ha emission, tracing current star formation, of the 45 largest and less inclined galaxies observed for which we estimate the torques between the gas and the bulk of the optical matter. We could subsequently study the Ha morphological aspect of these isolated spiral galaxies. Using Fourier analysis, we focus on the modes of the spiral arms and also on the strength of the bars, computing the torques between the gas and newly formed stars (Ha) and the bulk of the optical matter (Gunn r). We interpret the various bar/spiral morphologies observed in terms of the secular evolution experienced by galaxies in isolation. We also classify the different spatial distributions of star forming regions in barred galaxies. The observed frequency of particular patterns brings constraints on the lifetime of the various evolution phases. We propose an evolutive sequence accounting for the transitions between the different phases we could observe. Isolated galaxies appear not to be preferentially barred or unbarred. Through numerical simulations, trying to fit the Ha distributions yields constraints on the star formation law, which is likely to differ from a genuine Schmidt law. In particular, it is probable that the relative velocity of the gas in the bar also needs to be taken into account.