Posters

The characterisation of early galaxy evolution and the role of environment is crucial for understanding cosmic reionisation, a pivotal period in cosmic history. This study uses MUSE integral field spectroscopy from an archival sample of 20 quasars from Meyer et al .(in preparation) to measure their possible impact on neighbouring Lyα emitters (LAEs), using the Lyα luminosity function (Lyα LF). At this stage of the project, we are optimising our source identification and extraction using the MUSELET software 1, to identify the most robust catalogue of intrinsically luminous yet observationally faint LAE candidates at these challenging redshifts, before comparing the Lyα LF in QSO environments with that measured in blank fields.

Studies of early galaxy formation are crucial for understanding the processes that have shaped the current Universe. Galaxies with intense star formation at z \( > \) 6 are key to events such as reionization, but their faintness limits detailed studies. At lower redshifts (z \( \sim \) 1), analogous galaxies allow for better characterization. Extreme Emission Line Galaxies (EELGs) stand out due to their high equivalent widths (\( \sim \)1000 \( \AA \)), high specific star formation rates, low metallicities, and low masses. We aim to characterize the physical properties of a sample of 123 EELGs at 0.7 \( < \) z \( < \) 3, photometrically selected from the Extended Groth Strip catalog, obtaining results consistent with previous studies [1]. These results will serve as preparatory science for future MOSAIC instrument observations.

The study of metallicity offers key insights into mechanical and chemical feedback processes shaping galaxies evolution. My project focuses on a detailed understanding of interstellar medium (ISM) metallicity in simulated galaxies to allow direct comparison with observations, where metallicity is inferred from spectra of star-forming regions. Using recent hydrodynamical simulations with dustyGadget, I investigate how parameters such as stellar age, gas density, and spatial distribution influence the HII regions generated by stellar particles. This poster presents the resulting trends and their implications for linking simulations to observed metallicity measurements.

he luminosity function (LF) of active galactic nuclei (AGN) is a key demographic to understand the evolution of their population across cosmic time. Before the advent of JWST it was extremely challenging to build large (\( N>10 \)) samples of spectroscopically-confirmed AGN at high redshift (\( z>5 \)) [1]. The new JWST treasury program COSMOS-3D (C3D) addresses this limitation by providing wide-field slitless spectroscopy (WFSS) in the wavelength range \( {\sim}3.9\mbox{–}5.0\,\mu\mathrm{m} \) over a \( 0.33\,\mathrm{deg}^2 \) area, enabling the confident identification of the largest sample of line emitters at high redshift to date. \par NIRCam WFSS and images [2] are utilised to identify broad, i.e. FWHM \( {>}1000\,\mathrm{km}\mathrm{s}^{-1} \), H\( \alpha \) lines within \( 4.9 < z < 6.6 \) among photometrically pre-selected candidates within the complete C3D dataset. Based on the identifications we are building a BL AGN catalogue with measured line properties (flux, FWHM of narrow and broad components) and derived quantities (e.g., line luminosities, black hole masses) which serves as the foundation for constructing the AGN LF. \par Several BL H\( \alpha \)-emitter candidates show asymmetric emission lines with double-peak features. NIRSpec Integral Field Unit follow-up observations will reveal whether these signatures originate from interacting galaxies or represent dual AGN within a single host [3].