The Department of Physics welcomes Dr. Carlos J. Vargas to present during their virtual colloquium.
Dr. Vargas earned his Ph.D. in 2018 from New Mexico State University, where he led and contributed to large observing programs in the radio and optical to study the link between gaseous galaxy halos and star formation. He has since been a postdoc at the University of Arizona in Professor Erika Hamden’s ultraviolet/optical instrumentation development group. His most current work focuses on NASA space mission design and development to study the circumgalactic medium and star formation.
Abstract: For over half a century, observational astrophysics has been eager to successfully detect and map the most massive baryonic component of galaxies: warm-hot phase coronal gas extending into the circumgalactic medium (CGM). Despite its importance to galaxy evolution, this phase of gas is entirely unmapped in the nearby universe. Morphological characteristics, such as the presence, size, and extent of filamentary or cloud-like structures, are impossible to determine through pencil-beam absorption line studies. The evolution of galaxies relies heavily gaseous halos, indicating an urgent need to map and measure these understudied regions. In the last decade, high-efficiency reflective coatings for UV optics have undergone a renaissance with transformative improvements in reflectivity per bounce and overall coating stability in the extreme UV (EUV). Detector technology sensitive to EUV wavelengths has seen steady development of MicroChannel Plate (MCP) detector technology. In parallel with these advances in UV technology, SmallSat missions with serious science objectives—which did not exist a decade ago—have emerged as a promising platform for high-impact science, an opportunity for more adventurous experiments and investigations. In this talk, I present Aspera (PI C. Vargas): an EUV SmallSat mission concept to detect and map warm-hot phase gas emission in nearby galaxies for the first time. The Aspera mission was designed to target the O VI emission line doublet from highly ionized oxygen, located at ll (lambda) =1032, 1038 Å rest frame. Aspera combines a simple spectroscopic optical design using recent advances in highly-reflective EUV-coated optics with an advanced UV MCP detector to optimize throughput and sensitivity. Aspera will build multiple days of exposure time on each individual target to ensure spectroscopic detection of O VI emission and produce 2D morphological maps and direct measurements of physical conditions such as kinematics. The Aspera concept is being developed for submission to the inaugural 2020 NASA Astrophysics Pioneers call on October 1, 2020.
This event was first published on September 10, 2020 and last updated on September 11, 2020.