The counter-rotating stellar core of NGC 4494

TL;DR

This study reveals that NGC 4494 hosts a counter-rotating stellar core approximately 1 kpc in size, formed from the same material as the main galaxy, likely through internal dynamics or retrograde gas accretion.

Contribution

It provides detailed kinematic and stellar population analysis confirming the counter-rotating core as a disk, clarifying its formation mechanism in an early-type galaxy.

Findings

The core is a counter-rotating disk about 1 kpc in diameter.

Stellar populations in the core and main galaxy are very similar.

The core likely formed from internal processes or retrograde gas accretion.

Abstract

Context. Kinematically decoupled cores (KDCs) are often found in the centers of early-type galaxies. Aims. We aim to investigate the kinematics, structure, and stellar populations of the KDC residing in the early-type galaxy NGC 4494 to understand its formation. Methods. We used long-slit spectroscopic data obtained with the FORS2 instrument on the VLT to measure the stellar kinematics and stellar populations. We performed a spectroscopic decomposition to disentangle the properties of the KDC from those of the host galaxy and construct models of the observed rotation curve. Results. The rotation curve is characterized by two symmetric dips at |R|=6", where the rotation velocity drops to zero. Contrary to previous studies that explained the decoupled structure as a rapidly co-rotating disk, our analysis clearly shows that it is a counter-rotating component. A counter-rotating core is indeed needed to reproduce the observed dip in the velocity curve. The properties of the stellar populations of the decoupled core and the main galaxy are very similar: old stars (12-13 Gyr) with slightly super-solar metallicities (0<[Z/H]<0.15 dex) and alpha-enhanced (0 <[alpha/Fe]< 0.15 dex). Conclusions. Our results indicate that the counter-rotating component is a disk of about 1 kpc in diameter that is obscured by dust in the central 0.12 kpc. The properties of its stellar populations suggest that it formed from the same material as the main stellar body of the host galaxy. This could have happened via internal processes such as the precession of a pre-existing rotating core, or, alternatively, via gas accretion in retrograde orbits followed by star formation. In the latter scenario, the accretion event occurred almost simultaneously with the formation of the galaxy, using material that had the same composition as the gas from which the stars in the main body of the galaxy were formed.