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The James Webb Space Telescope (JWST) will enable the detection of opticalemission lines in galaxies spanning a broad range of luminosities out toredshifts z>10. Measurements of key galaxy properties, such as star formationrate and metallicity, through these observations will provide unique insightinto, e.g., the role of feedback from stars and active galactic nuclei (AGNs)in regulating galaxy evolution, the co-evolution of AGNs and host galaxies, thephysical origin of the 'main sequence' of star-forming galaxies and thecontribution by star-forming galaxies to cosmic reionization. We present anoriginal framework to simulate and analyse observations performed with the NearInfrared Spectrograph (NIRSpec) on board JWST. We use the BEAGLE tool (BayEsianAnalysis of GaLaxy sEds) to build a semi-empirical catalogue of galaxy spectrabased on photometric spectral energy distributions (SEDs) of dropout galaxiesin the Hubble Ultra Deep Field (HUDF). We demonstrate that the resultingcatalogue of galaxy spectra satisfies different types of observationalconstraints on high redshift galaxies, and use it as input to simulateNIRSpec/prism (R~100) observations. We show that a single 'deep' (~100 ks)NIRSpec/prism pointing in the HUDF will enable S/N>3 detections of multipleoptical emission lines in ~30 (~60) galaxies at z>6 (z~4-6) down to m_F160W<30AB mag. Such observations will allow measurements of galaxy star formationrates, ionization parameters and gas-phase metallicities within factors of 1.5,mass-to-light ratios within a factor of 2, galaxy ages within a factor of 3 andV-band attenuation optical depths with a precision of 0.3.

Simulating and interpreting deep observations in the Hubble Ultra Deep Field with the JWST/NIRSpec low-resolution 'prism'