We present the first elemental abundance measurements of the K dwarf (K6) exoplanet-host star WASP-107 using high-resolution (R~45,000), near-infrared (H- and K-band) spectra from the IGRINS Spectral Archive. We use the previously determined physical parameters of the star from literature and infer the abundances of 13 elements, i.e., C, O, Na, Mg

Recently, mid-infrared (MIR) interferometry and single-dish high angular resolution imaging has revealed the presence of dust in the polar regions of nearby active galactic nuclei (AGN), on scales from parsecs to hundreds of parsecs. However, the nature, extent, and connection to the postulated outflows and inflows in the AGN environs is poorly

Cross-correlations of galaxy positions and galaxy shears with maps of gravitational lensing of the cosmic microwave background (CMB) are sensitive to the distribution of large-scale structure in the Universe. Such cross-correlations are also expected to be immune to some of the systematic effects that complicate correlation measurements internal to

Joint analyses of cross-correlations between measurements of galaxy positions, galaxy lensing, and lensing of the cosmic microwave background (CMB) offer powerful constraints on the large-scale structure of the Universe. In a forthcoming analysis, we will present cosmological constraints from the analysis of such cross-correlations measured using

We present cosmological constraints from the analysis of two-point correlation functions between galaxy positions and galaxy lensing measured in Dark Energy Survey (DES) Year 3 data and measurements of cosmic microwave background (CMB) lensing from the South Pole Telescope (SPT) and Planck. When jointly analyzing the DES-only two-point functions

We present JWST/MIRI MRS spectroscopy of three Seyfert AGN in which we compare their nuclear Polycyclic Aromatic Hydrocarbons (PAHs) emission with that of star-forming regions. This study, for the first time, investigates local luminous Seyferts (L bol > 10 44.46 erg/s) over a wide wavelength range (4.9-28.1 μm) using sub-arcsecond angular