Modelling the molecular gas that is detected through CO observations of high-z galaxies constitutes a major challenge for ab initio simulations of galaxy formation. I will present recent numerical work aimed at studying the formation and evolution of the simplest and most abundant molecule, H2. Our model fully solves the out-of-equilibrium rate equations and accounts for the unresolved structure of molecular clouds. We apply our model to two types of cosmological simulations: a) the formation of a Milky Way-sized galaxy at z=2 and b) a small cosmological box in order to obtain some statistical results. The results are compared to those obtained from two different approximations commonly used in the literature and for numerical convergence. Our results indicate that independently of the model, robust results (H2 masses) can only be obtained for galaxies that are suffiiciently metal enriched in which H2 formation is fast. However, their morphology differ from model to model. Furthermore, the cosmological H2 mass function derived from the non-equilibrium model agrees well with recents observations that only sample the high-mass end. Extensions of our model towards including other molecules, such as CO, and species, in particular C and its derivatives, will also be discussed.

Abstract: I will review recent observations and theoretical estimates of the spatial extent of galaxies, defined as systems of stars and gas embedded in extended halos of dark matter and hot gas. Formed by the infall of smaller systems, their sizes are determined by gravitational assembly, gas dynamics, and chemical enrichment in heavy elements blown into extragalactic space by galactic winds. But the full extent of galaxies remains poorly determined. The “virial radius” and “splash-back radius” approximate the separation between collapsed structures and infalling matter. Other measurements include X-ray emission and ultraviolet absorption lines from metal-enriched gas in galactic halos. Astronomers have identified large reservoirs of baryonic matter in the circumgalactic medium (CGM) and intergalactic medium (IGM) that contain 50-70% of the cosmological baryons formed in the Big Bang. Investigations of physical processes at the “edge of galaxies” help define the importance of this gas in sustaining the star formation in galaxies.

The HI-MaNGA survey is an HI (21cm line) follow-up program for the SDSS-IV MaNGA survey.  I will describe the HI-MaNGA survey, its progress to date, and future plans.  I will then present new results where we combine HI-MaNGA and MaNGA data to investigate how the global HI content of star-forming galaxies relates to the mean properties of their ISM derived from optical emission lines, including integrated equivalent width, metallicity, ionization parameter, and the relative strength of low-ionization lines such as [SII] and [OI]. This analysis allows us to understand if and how the properties of the ISM vary between the most gas-rich galaxies to the most gas-poor, and how such variations may affect their evolution.  I will also discuss how gas content relates to the nuclear ionizing source (e.g., Seyfert, LINER, HII regions) and whether we find any evidence that AGN contribute to gas deficiency in the galaxy population.

Zoom Recording: https://uky.zoom.us/rec/share/xGrDewYs7rui5ao4A-_hr_N5r8_c6mkGkiksm--I61WP-hQ8VhJn9HM8fTadgDUG.M9oUhbMc-oa1r2Nr

Stellar parameter determination represents a critical step in the procedure of Simple Stellar Population Synthesis (SSPS), of which the aim is to produce realistic composite spectra for model stellar populations, such as galaxies and star clusters. As SDSS-IV nears completion, the MaStar stellar library, an unprecedented large and comprehensive collection of medium-resolution stellar spectra from ~10,000 unique stars, will be made available to the public in its entirety. In order to make proper use of such a library in SSPS, accurate stellar parameter estimates (Teff, log g, [Fe/H], and [\alpha/Fe]) associated with the spectra are a necessity. Here, I present a new approach to stellar parameter estimation that we in the MaStar team have developed in recent years, which combines the spirit of conventional methods with the goal of obtaining an efficient and versatile software pipeline for delivering stellar parameter estimates, as well as other important data such as extinction estimates. This method makes use of the continuum-normalized stellar spectra and the spectral continua themselves (often characterized by photometric measurements in previous efforts) to match the MaStar spectra to models derived from the ATLAS9-based BOSZ model set via reduced-\chi^2 fitting. Carefully combining these two approaches allows us to avoid many of the problems that afflict each approach separately, and obtain reliable estimates throughout parameter space, including notoriously difficult regimes, such as at higher temperatures (> 7000 K). Steps are also taken to account for extinction and flux calibration residuals present in the data. Since this project is ongoing, focus will be placed on recent progress, preliminary results, and plans for the near future.

The Galactic center excess has lingered as a possible, but ambiguous, signal of new physics for several years. It has previously been argued that certain details of the excess emission imply that it likely originates from a population of point sources, but this remains a topic of vigorous debate. In this talk, I will report on my recent work, relying on a new point source catalog (obtained by the Fermi-LAT collaboration), that sheds light on this controversial topic. After giving some background on the excess, I will discuss various metrics that have been used to try to understand its true nature. I will show that the large majority of bright sources that were previously suggested to be members of the excess are indeed contained in the new Fermi-LAT point source catalog -- and yet, despite masking out these sources (so that they cannot contribute to the excess), the excess remains just as bright in our new fit to the data. I will go on to discuss the implications of our findings for the two most popular interpretations of the excess.