GA-NIFS: JWST/NIRSpec IFS view of the z~3.5 galaxy GS5001 and its close environment at the core of a large-scale overdensity

Kavli Affiliate: Roberto Maiolino

| First 5 Authors: Isabella Lamperti, Santiago Arribas, Michele Perna, Bruno Rodríguez Del Pino, Chiara Circosta

| Summary:

We present JWST NIRSpec observations in IFS mode of the galaxy GS5001 at
redshift z=3.47, the brightest member of a candidate protocluster in the
GOODS-S field. The data cover a field of view (FoV) of 4”$times$4”
(~$30times30$~kpc$^2$) and were obtained as part of the GA-NIFS GTO program.
The observations include both high (R~2700) and low (R~100) spectral resolution
data, spanning the rest-frame wavelength ranges 3700-6780A and 1300-11850A,
respectively. We analyse the spatially resolved ionised gas kinematics and
interstellar medium properties, including obscuration, gas metallicity,
excitation, ionisation parameter, and electron density. In addition to the
central galaxy, the NIRSpec FoV covers three components in the south, with
velocities blue-shifted by -150 km/s with respect to the main galaxy, and
another source in the north redshifted by ~200 km/s. The emission line ratios
in the BPT diagram are consistent with star formation for all the sources in
the FoV. We measure electron densities of ~500 cm$^{-3}$ in the different
sources. The gas-phase metallicity in the main galaxy is 12+log(O/H) $=
8.45pm0.04$, and slightly lower in the companions (12+log(O/H)$ = 8.34-8.42$),
consistent with the mass-metallicity relation at $zsim3$. We find peculiar
line ratios (high log [NII]/H$alpha$, low log [OIII]/H$beta$) in the northern
part of the main galaxy (GS5001). These could be attributed to either higher
metallicity, or to shocks resulting from the interaction of the main galaxy
with the northern source. We identify a spatially resolved outflow in the main
galaxy, with an extension of about 3 kpc. We find maximum outflow velocities of
~400 km/s, an outflow mass of $(1.7pm0.4)times 10^8$ M$_{odot}$, a mass
outflow rate of $23pm5$ M$_{odot}$ yr$^{-1}$ and a mass loading factor of
0.23. These properties are compatible with star formation being the driver of
the outflow.

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