Formation and evolution of blue compact dwarfs: The origin of their steep rotation curves

TL;DR

This study uses numerical simulations to explore how mergers of gas-rich dwarf irregular galaxies lead to the steep rotation curves observed in blue compact dwarf galaxies, highlighting the role of central gas concentration.

Contribution

It demonstrates that central gas concentration from dwarf mergers explains the steep rotation curves and starburst activity in BCDs, advancing understanding of their formation.

Findings

Dark matter central concentration increases post-merger

Gas transfer causes steep rotation curve gradients

Central gas concentration correlates with starburst activity

Abstract

The origin of the observed steep rotation curves of blue compact dwarf galaxies (BCDs) remains largely unexplained by theoretical models of BCD formation. We therefore investigate the rotation curves in BCDs formed from mergers between gas-rich dwarf irregular galaxies based on the results of numerical simulations for BCD formation. The principal results are as follows. The dark matter of merging dwarf irregulars undergoes a central concentration so that the central density can become up to six times higher than those of the initial dwarf irregulars. However, the more compact dark matter halo alone can not reproduce the gradient differences observed between dwarf irregulars and BCDs. We provide further support that the central concentration of gas due to rapid gas-transfer to the central regions of dwarf--dwarf mergers is responsible for the observed difference in rotation curve gradients. The BCDs with central gas concentration formed from merging can thus show steeply rising rotation curves in their central regions. Such gas concentration is also responsible for central starbursts of BCDs and the high central surface brightness and is consistent with previous BCD studies. We discuss the relationship between rotational velocity gradient and surface brightness, the dependence of BCD rotation curves on star formation threshold density, progenitor initial profile, interaction type and merger mass ratio, as well as potential evolutionary links between dwarf irregulars, BCDs and compact dwarf irregulars.