H$\alpha$ Kinematics of Superbubbles and Supernova Remnants of the Dwarf galaxy NGC 4214

TL;DR

This study uses high-resolution Fabry-Perot interferometry to analyze the ionised gas kinematics, superbubbles, and supernova remnants in dwarf galaxy NGC 4214, revealing their physical properties and dynamics.

Contribution

First detailed 3D kinematic maps of NGC 4214's ionised gas complexes and analysis of superbubbles and supernova remnants' expansion velocities and ages.

Findings

Superbubbles expand at ~50 km/s with ~2 Myr age.

Supernova remnants have expansion velocities of 48-80 km/s and ~10^4 years age.

Superbubbles and remnants' physical parameters suggest massive stars influence their dynamics.

Abstract

We analysed the ionised gas kinematics of the dwarf galaxy NGC 4214 using high resolution Fabry-Perot interferometry observations and present a set of narrowband images in the H$\alpha$, [SII] $\lambda$6717 $\r{A}$, [NII] $\lambda$6584 $\r{A}$ and [OIII] $\lambda$5007 $\r{A}$ emission lines. The high-resolution Fabry-Perot observations of the H$\alpha$ emission line, allowed us to derive the velocity field, the velocity dispersion $\sigma$, and the rotation curve of the galaxy. We also present for the first time, three-dimensional kinematic maps of the complexes NGC 4214-I and NGC 4214-II and analysed the kinematics of the ionised gas of two new superbubbles, as well as the supernova remnants previously detected in this galaxy by other authors, in radio, optical and X-ray emission. We computed the expansion velocities of the superbubbles and supernova remnants fitting their velocity profiles and obtained their respective physical parameters. We found that the superbubbles have an expansion velocity of ~50 km s$^{-1}$, dynamical age about $\sim$2 Myr and wind luminosity L$_W$ of ~9X10$^{38}$ erg s$^{-1}$ produced probably by massive stars in OB associations. For supernova remnants, their expansion velocities are between $\sim$48 to $\sim$80 km s$^{-1}$ with ages of about 10$^{4}$ years and kinetic energy of about 10$^{51}$ erg assuming they are in the radiative phase of evolution.