Spectroscopy with the JWST Advanced Deep Extragalactic Survey (JADES) -- the NIRSpec/NIRCam GTO galaxy evolution project

TL;DR

The JADES project uses JWST's NIRCam and NIRSpec instruments to study galaxy evolution from redshift 2 to beyond 10, providing detailed photometric and spectroscopic data to understand early universe galaxy properties.

Contribution

This paper presents an overview of the JADES survey, combining deep imaging and spectroscopy to advance understanding of high-redshift galaxy formation and evolution.

Findings

Multi-filter NIRCam imaging enables unprecedented photometric redshifts.

NIRSpec spectroscopy measures secure redshifts and galaxy properties.

Coupled data will explore star formation, metallicity, and reionization contributions.

Abstract

I present an overview of the JWST Advanced Deep Extragalactic Survey (JADES), a joint program of the JWST/NIRCam and NIRSpec Guaranteed Time Observations (GTO) teams involving 950 hours of observation. We will target two well-studied fields with excellent supporting data (e.g., from HST-CANDELS): GOODS-North and South, including the Ultra Deep Field. The science goal of JADES is to chart galaxy evolution at z > 2, and potentially out to z > 10, using the rest-frame optical and near-IR though observations from $\approx$ 1 - 5 $\mu$m. Multi-colour NIRCam imaging with 9 filters will enable photometric redshifts and the application of the Lyman break technique out to unprecedented distances. NIRSpec spectroscopy (with spectral resolving powers of R = 100, 1000 & 2700) will measure secure spectroscopic redshifts of the photometrically-selected population, as well as stellar continuum slopes in the UV rest-frame, and hence study the role of dust, stellar population age, and other effects. Measuring emission lines can constrain the dust extinction, star formation rates, metallicity, chemical abundances, ionization and excitation mechanism in high redshift galaxies. Coupling NIRCam and NIRSpec observations will determine stellar populations (age, star formation histories, abundances) of galaxies and provide the information to correct their broad-band spectral energy distribution for likely line contamination. Potentially we can search for signatures of Population III stars such as HeII. We can address the contribution of star-forming galaxies at z > 7 to reionization by determining the faint end slope of the luminosity function and investigating the escape fraction of ionizing photons by comparing the UV stellar continuum with the Balmer-line fluxes.