I Congreso de Postgrado fcfm: ingeniería, ciencias e innovación

31 Santiago, 10 al 12 de agosto, 2022 A S T RONOM Í A 01 PROBING THE MILKY WAY’S GAS RESERVOIRS WITH QUASARS Felipe Corro-Guerra¹*, Trystyn Berg¹ , ², Sebastian López¹ ¹Unive sidad de Chile, Casilla 36-D, Santi go, Chile. ²ESO fellow, Alonso de Córdova 3107, Santiago, Chile. *Email: fcorro@das.uchile.cl ABSTRACT Assessing the physical conditions of gas reservoirs of galaxies is important to study the history of their star formation. The advantage of studying the MW is that we can see 2-D variations in the gas properties -- chemical composition, density, and temperature -- in contrast to other galaxies that can only be studied in 1-D. Our goal is to quantify the Milky Way (MW)’s gas reservoirs’ properties in order to compare to observed galaxies across different cosmic times. To this end, we have used ~200 quasars (QSO) spectra sightlines across the sky, from the Cosmic Origin Spectrograph aboard Hubble Space Telescope to study the amounts of Fe in the gas reservoirs of the MW. We aim to understand the differences between the physical conditions of the gas both surrounding and within the MW. Since the QSO we observe are outside the MW with their spectra we probe the gas in the halo and disk of the MW. We compare our results to the literature which probes the gas only in the disk of the Galaxy to conclude about the scales in which the abundances change across the sky. We calculated the abundances of Fe in every sightline and plotted them in the sky, see Figure 1. In this talk I will summarize my methods, and results from my comparison with the literature. Figure 1: Distribution of abundance of Fe across the sky (colored circles; lighter colors represent higher abundance). In contrast the stars in the figure denote the abundance of Fe in the disk of the MW.