I Simposio de Postgrado 2023. Ingeniería, ciencias e innovación

I SIMPOSIO 2023 METALS IN GALAXY HALOS AT COSMIC NOON 1 Departamento de Astronomía, Universidad de Chile. 2 Centre de Recherche Astrophysique de Lyon. 3 Franco-Chilean Laboratory for Astronomy. *Email: dzamora@das.uchile.cl Diego Zamora 1* , Pasquier Noterdaeme 2, 3 , Sebastián Lopez 1 Figure 1: Comparison of equivalent width distribution. ABSTRACT Galaxies are capable of enriching the gas found in their surroundings and between them with elements forged inside stars. This occurs through large ejections of material outward. This study focuses on the evolution of this enrichment, particularly during the phase of the universe when star formation was at its peak, roughly 11 Gyr back in time. Since the intergalactic medium is highly diffuse and therefore difficult to observe directly, it is studied as intervening objects that absorb radiation at specific wavelengths from background sources. By using distant galaxies magnified by gravitational lenses as a light source and integral field spectroscopy data, we can study different absorbers, characterized by the presence of triply ionized carbon. Through VLT/MUSE spectra in the fields of five gravitational arcs and utilizing an automatic search algorithm, we detected 176 absorber candidates in 130 spectra. After estimating the completeness of the sample, we obtained the equivalent width distribution.This quantity ultimately holds dependencywith the most basic properties of these objects, size and number density. We compared the result with findings from studies using quasars as background sources. Despite the low completeness levels for weak absorbers, some similarity is observed, unlike our strong absorbers, whi ch show significant differences. These differences stem from both statistical arguments and notable dissimilarities between the methods used. Thefigure shows the comparisonof equivalentwidthdistribution. The y-axis is equivalent width distribution, hence number of absorbers per unit equivalent width per unit comoving path length and the x-axis is equivalent width, a measure of strength of the absorption. Astronomía The figure shows the comparison of equivalent width distribution. The y-axis is equiv distribution, hence number of absorbers per unit equivalent width per unit comoving and the x-axis is equivalent width, a measure of strength of the absorption.