A VLT VIMOS study of the anomalous BCD Mrk 996: mapping the ionised gas kinematics and abundances

TL;DR

This study uses high-resolution VLT VIMOS integral field spectroscopy to analyze the ionized gas kinematics and chemical abundances in the peculiar blue compact dwarf galaxy Mrk 996, revealing complex multi-component emission and unusual excitation conditions.

Contribution

It provides the first detailed spatially-resolved analysis of Mrk 996's ionized gas, including kinematics, temperature, density, and chemical enrichment, highlighting its unique dense core and excitation mechanisms.

Findings

Detection of multi-component line emission with a mini-spiral structure.

Identification of high-density, high-temperature broad line regions.

Evidence of nitrogen enrichment in broad line regions.

Abstract

A study of the blue compact dwarf (BCD) galaxy Mrk 996 based on high resolution optical VLT VIMOS integral field unit spectroscopy is presented. Mrk 996 displays multi-component line emission, with most line profiles consisting of a narrow, central Gaussian with an underlying broad component. The broad HI Balmer component splits into two separate broad components inside a 1".5 radius from the nucleus; these are attributed to a two-armed mini-spiral. The rotation curve of Mrk 996 derived from the H\alpha narrow component yields a total mass of 5x10^8 Msol within a radius of 3 kpc. The high excitation energy, high critical density [O III] 4363 and [N II] 5755 lines are only detected from the inner region and exist purely in broad component form, implying unusual excitation conditions. Surface brightness, radial velocity, and FWHM maps for several emission components are presented. A separate physical analysis of the broad and narrow emission line regions is undertaken. We derive an upper limit of 10,000 K for the electron temperature of the narrow line gas, together with an electron density of 170 cm^-3, typical of normal H II regions. For the broad line component, we estimate a temperature of 11,000 K and an electron density of 10^7 cm^-3. The broad line emission regions show a N/H enrichment factor of ~20 relative to the narrow line regions, but no He/H, O/H, S/H, or Ar/H enrichment is inferred. The dominant line excitation mechanism is photoionisation by the ~3000 WR stars and ~150,000 O-type stars estimated to be present in the core. This is indeed a peculiar BCD, with extremely dense zones of gas in the core, through which stellar outflows and possible shock fronts permeate contributing to the excitation of the broad line emission. [Abridged]