Cloud-scale Radio Surveys of Star Formation and Feedback in Triangulum Galaxy M 33: VLA Observations

TL;DR

This study uses high-resolution radio observations of galaxy M 33 to analyze star formation, cosmic rays, and magnetic fields, revealing how star formation influences interstellar medium properties and cosmic ray behavior.

Contribution

It provides a detailed multi-band radio continuum survey of M 33, separating thermal and nonthermal emissions, and investigates their relation to star formation and ISM components at high resolution.

Findings

Radio sources <200 pc account for 36-46% of total RC emission.

Nonthermal spectral index flattens with increasing star formation rate.

Magnetic field strength correlates with star formation rate, indicating efficient small-scale dynamo action.

Abstract

Studying the interplay between massive star formation and the interstellar medium (ISM) is paramount to understand the evolution of galaxies. Radio continuum (RC) emission serves as an extinction-free tracer of both massive star formation and the energetic components of the interstellar medium. We present a multi-band radio continuum survey of the local group galaxy M 33 down to ~30 pc linear resolution observed with the Karl G. Jansky Very Large Array (VLA). We calibrate the star-formation rate surface density and investigate the impact of diffuse emission on this calibration using a structural decomposition. Separating the thermal and nonthermal emission components, the correlation between different phases of the interstellar medium and the impact of massive star formation are also investigated. Radio sources with sizes <~ 200 pc constitute about 36% (46%) of the total RC emission at 1.5 GHz (6.3 GHz) in the inner 18' x 18' (or 4kpc x 4kpc) disk of M 33. The nonthermal spectral index becomes flatter with increasing star-formation rate surface density, indicating the escape of cosmic ray electrons {from their birth places}. The magnetic field strength also increases with star-formation rate following a bi-modal relation, indicating that the small-scale turbulent dynamo acts more efficiently at higher luminosities and star-formation rates. Although the correlations are tighter in star-forming regions, the nonthermal emission is correlated also with the more quiescent molecular gas in the ISM. An almost linear molecular star-formation law exists in M 33 when excluding diffuse structures. Massive star formation amplifies the magnetic field and increases the number of high-energy cosmic ray electrons, which can help the onset of winds and outflows.