GA-NIFS: Multi-phase analysis of a star-forming galaxy at $z \sim 5.5$

TL;DR

This study uses advanced JWST/NIRSpec observations to analyze a z~5.5 star-forming galaxy, revealing it as a merger with complex outflows and detailed multiphase interstellar medium properties, challenging previous disk interpretations.

Contribution

First spatially resolved UV and optical emission analysis of a high-redshift galaxy, revealing its merger nature and detailed gas outflow characteristics.

Findings

HZ4 is a galaxy merger, not a rotating disk.

Detected extended outflows up to 4 kpc from the galaxy.

Ionized and neutral outflows are co-spatial with different mass loadings.

Abstract

In this study, we present a detailed multiphase analysis of HZ4, a main-sequence star-forming galaxy at z ~ 5.5, known for being a turbulent rotating disk and having a detection of a [CII] outflow in the ALMA observations. We exploit JWST/NIRSpec observations in the integral field spectroscopy mode with low- and high-spectral resolution that allow us for the first time to spatially resolve the rest-frame UV and optical emission of the galaxy to investigate the galaxy properties. In particular, the high-resolution dataset allows us to study the kinematics of the ionized gas phase, and the conditions of the interstellar medium, such as the excitation mechanism, dust attenuation, and metallicity. The lower-spectral resolution observations allow us to study the continuum emission and infer the stellar populations' ages and properties. Our findings suggest that HZ4 is a galaxy merger rather than a rotating disk as previously inferred from lower resolution [CII] data. The merger is associated with an extended broad, blueshifted emission, potentially indicative of an outflow originating from a region of intense star formation and extending up to 4 kpc. In light of these new observations we reanalyzed the ALMA data to compare the multiphase gas properties. If we interpret the broad components seen in [CII] and [OIII]$\lambda$5007\.A as outflows, the neutral and ionized components are co-spatial, the mass loading factor of the ionized phase is significantly lower than that of the neutral phase, aligning with trends observed in multi-phase systems at lower redshifts. Nonetheless, additional observations and larger statistical samples are essential to determine the role of mergers and outflows in the early Universe and to clarify the origin of the broad emission components observed in this system.