Logging data are measurements of physical properties of the formation surrounding a borehole, acquired in situ after completion of coring (wireline logging) or during drilling (Logging-While-Drilling, LWD). The range of data (resistivity, gamma radiation, velocity, density, borehole images,…) in any hole depends on the scientific objectives and...

Based on a clumpy-cloud model for CIV absorbers we propose a universal column density profile for CIV clouds that is consistent with the observed column density distribution (e.g. D'Odorico et al. 2010). Using this model, we simulate pencil-beam (QSOs) and wide-beam (gravitational arcs) spectra. In this talk, I will show how, by employing...

Observations of diffuse gas in this circum-galactic medium (CGM) provide the most direct means to understand the baryon cycle, and how the growth of galaxies is profoundly influenced by the interplay of gas accretion from/outflows into their surroundings. However, traditional observations of the CGM are limited by the use of single background...

A key requirement to determining the structure, mass, and dynamics of the CGM is understanding its distribution along the disk axis. We use HST/COS observations of a set of novel UV-bright QSOs along the plane of the Milky Way from the Plane Quasar Survey to test the latest hydrodynamical, cosmological simulations that suggest extended, ionized...

The outcome of the evolutionary history of galaxies is recorded in the interstellar abundances of chemical elements. Observations of the interstellar medium (ISM) in galaxies of various types, differing in terms of mass, size, metallicity, and their respective evolutionary stages, may provide a key to understanding the processes taking place in...

Using the extreme sensitivity and 140 hour exposure times in the MUSE eXtreme Deep Field (MXDF) in the Hubble Ultra Deep Field, we are able to probe the inner CGM of strongly star-forming galaxies in non-resonant emission lines out to redshift of ~1. Of particular interest, is the [OII]_3727 doublet, for which we are able to measure the...

Cosmological hydrodynamical simulations are reaching enough resolution to explore the kpc-scale CGM via mock spectra. In this talk I will show spatially resolved absorption line "spectroscopy" of TNG50 halos using point-like and extended sources that mimic QSO and gravitational arc spectra, respectively. Our goal is to (1) study the effect...

We probe the structures embedded in the foreground Milky Way ISM and CGM using pairs of OB stars in the Large and Small Magellanic clouds. The UV spectra of the massive hot OB stars (130 in the LMC and 120 in the SMC) from various instruments (i.e., COS, FUSE, and STIS) have been archived as part of the Hubble director's discretionary program...

Low-mass galaxy groups are the most common environments for galaxies in the Universe, providing a crucial link between cosmology and galaxy evolution. Due to the low mass and sparse population of these groups, there is no strict division between the intra-group medium (IGrM) and the circumgalactic medium (CGM). These groups contain highly...

The circumgalactic medium (CGM) is a multiphase and ionized plasma that surrounds and is gravitationally bound to galaxies. There is much that still needs to be understood about the spatial distribution, thermodynamics, and kinematics of circumgalactic gas. We can probe these properties by looking at the column densities of ions that trace...