# Optical IFU spectroscopy of a bipolar microquasar jet in NGC 300

## TL;DR

This study uses optical IFU spectroscopy to analyze a bipolar microquasar jet in NGC 300, providing detailed kinematic and physical properties, including jet power and age, which enhances understanding of such systems.

## Contribution

It presents the first detailed optical IFU analysis of a microquasar jet in NGC 300, enabling precise measurements of jet power and kinematics.

## Key findings

- Jet extent of approximately 40 parsecs.
- Shock velocity around 150 km/s.
- Jet power estimated at 6.3 x 10^{38} erg/s.

## Abstract

We recently reported the discovery of a candidate jet-driving microquasar (S10) in the nearby spiral galaxy NGC 300. However, in the absence of kinematic information, we could not reliably determine the jet power or the dynamical age of the jet cavity. Here, we present optical MUSE integral field unit (IFU) observations of S10, which reveal a bipolar line-emitting jet structure surrounding a continuum-emitting central source. The optical jet lobes of S10 have a total extent of $\sim$ 40 pc and a shock velocity of $\sim$ 150 km s$^{-1}$. Together with the jet kinematics, we exploit the MUSE coverage of the Balmer H$\beta$ line to estimate the density of the surrounding matter and therefore compute the jet power to be $P_{jet}\approx$ 6.3 $\times$ 10$^{38}$ erg s$^{-1}$. An optical analysis of a microquasar jet bubble and a consequent robust derivation of the jet power have been possible only in a handful of similar sources. This study therefore adds valuable insight into microquasar jets, and demonstrates the power of optical integral field spectroscopy in identifying and analysing these objects.