Dr. Janna Levin
James McAteer, NMSU
Why is this picture correct? And what does that have to do with Pikachu?
The Aditya-L1 mission: ISRO’s first solar observatory in space
Durgesh Tripathi, Inter-University Centre for Astronomy and Astrophysics
Abstract: Aditya-L1 is the first space mission of ISRO dedicated to solar observation. With seven payloads on boards, Aditya-L1 will provide the remote sensing observations of the Sun from Hard-X rays to infrared as well as in situ measurements of solar wind and interplanetary magnetic field. It aims to provide coronal magnetic field measurement using Spectro-polarimetric observation in the infrared Fe XIII line. It will measure the spatially resolved solar spectral irradiance in the near ultraviolet, central to our understanding of the Sun climate relations. This talk will discuss the mission’s capabilities with a focus on the Solar Ultraviolet Imaging Telescope (SUIT). SUIT will image the sun in 2000-4000 A band using 11 different filters, which is designed to study the coupling and dynamics of the lower solar atmosphere and obtain crucial inputs on the solar spectral irradiance in the NUV range.
Small Statistics No More: a suite of galaxy simulations to interpret observations
Alyson Brooks, Rutgers University
The past decade has seen tremendous progress in simulating realistic dwarf galaxies. Despite the hype, not all dwarfs are simulated equally. Given their shallow potential wells, dwarfs are an excellent probe of star formation and feedback processes. In this talk, I’ll outline a campaign to simulate the largest suite of dwarf galaxies to date, in environments both near the Milky Way (the DC Justice League simulations) and further afield (the Marvel simulations). These high resolution simulations are probing dwarf galaxy formation from LMC-mass scales down into the regime of the ultra-faints for the first time. Our realistic dwarf galaxies can be used to interpret galaxy formation and to make predictions for upcoming surveys such as LSST at the Vera Rubin Observatory. Controlled tests with the simulated dwarfs may also reveal clues about how the first stellar populations formed.
Characteristics of Gaseous Counter-rotating Galaxies and their Role in Galaxy Evolution
Minje Beom, NMSU
A counter-rotating galaxy is a galaxy having one or more component with opposite angular momentum to the main stellar disk. Absent the presence of tidal tails and disturbed morphologies seen in ongoing galaxy mergers, a counter-rotating feature is the most direct evidence for past galaxy interaction. Not only counter-rotators are unique and interesting themself, but they are good targets from the perspective of their possible role in galaxy quenching. This study is analyzing characteristics of gaseous counter-rotators in the largest and unbiased galaxy sample based on the large MaNGA galaxy sample. We also include various photometric data from UV to Radio data and archival images for a comprehensive analysis. Based on these, we will present reliable statistics and common characteristics for various gaseous counter-rotators with different galaxy types and inclinations. Their characteristics will be also analyzed to describe how they are linked to their formation process. The kinematics of counter-rotators will be analyzed from the galaxy evolution point of view to compare to that of the other normal galaxies. In addition, we will search for any counter-rotating stellar component embedded in the major stellar disk to see any evidence for the formation origin or to estimate a stellar population formed in the centrally concentrated gas produced by their formation process.
Constraining Galaxy Formation and Baryonic Effects on LSS with
Observations of the Thermal and Kinetic Sunyaev-Zeldovich Effects
Nicolas Battaglia, Cornell University
A new window into the growth and evolution of large-scale
structure has opened up with the recent observations of the thermal
and kinetic Sunyaev-Zel’dovich (SZ) effects. I will review recent
observations of the SZ signals and highlight their expected rapid
growth over the next decade with upcoming cosmic microwave background
experiments, like Simons Observatory and CMB-S4. I will present
ongoing work to extract SZ signals in data from the Atacama Cosmology
Telescope and how they can be used to constrain the important baryonic
process that govern galaxy formation. Time permitting, I will conclude
by discussing the connections between these SZ observations and
mitigating the modeling uncertainties associated with “baryonic
effects” in future large-scale structure surveys like LSST.
The view of early massive galaxies in the run up to JWST
Christina Williams, University of Arizona
Our most powerful telescopes have glimpsed galaxies in their early growth phase only a few billion years after the Big Bang. Surprisingly, galaxy surveys show that the most massive galaxies in the Universe were formed the earliest in cosmic time, in an extreme but short-lived burst of star-formation. I will discuss my research into how these first massive galaxies form and evolve using the Atacama Large Millimeter Array (ALMA), and what we have learned about the unknown astrophysics that drives their extreme lives. Some of the most interesting and unexplored phases of galaxy evolution remain hidden from our telescopes as a result of their limited sensitivity and wavelength coverage. After its launch, the James Webb Space Telescope (JWST) will unveil the hidden physics of early galaxy growth for the first time. I will conclude with some predictions for galaxy surveys planned for the first year of JWST, which will produce the deepest infrared imaging and spectroscopy ever taken, and can resolve many outstanding questions about the life cycle of massive galaxies.
Unveiling the physics of gaseous halos through X-ray spectroscopy
Aurora Simionescu, Netherlands Institute for Space Research
As bright X-ray emitters, the cores of clusters of galaxies have been studied for over 50 years, with many exciting applications ranging from plasma physics to precision cosmology. I will discuss three main directions in which the study of gaseous haloes can be pushed to new frontiers using X-ray astronomy.
The first is to expand our studies to the much fainter, outer regions of massive galaxy clusters, which can teach us how these objects grow by accreting matter from the surrounding large-scale structure. The second is to expand our studies to significantly higher spectral resolution, revealing the dynamics of the intra-cluster medium for the first time and giving a much clearer picture of its chemical composition. The third is to expand these studies to the much less massive (and also fainter) halos of galaxy groups and eventually the circumgalactic medium, where feedback from supermassive black holes plays an increasingly important role.
I will briefly summarise the current state-of the art and point our some recent progress in these three fields, as well as present the outstanding open questions and how future space missions and mission concepts will help address them.