Interstellar dust is still a dominant uncertainty in Astronomy, limiting precision in e.g., cosmological distance estimates and models of how light is re-processed within a galaxy. When a foreground galaxy serendipitously overlaps a more distant one, the latter backlights the dusty structures in the nearer foreground galaxy. Such an overlapping or occulting galaxy pair can be used to measure the distribution of dust in the closest galaxy with great accuracy. The STARSMOG program uses Hubble to map the distribution of dust in foreground galaxies in fine (<100 pc) detail. Integral Field Unit (IFU) observations will map the effective extinction curve, disentangling the role of fine-scale geometry and grain composition on the path of light through a galaxy. The overlapping galaxy technique promises to deliver a clear understanding of the dust in galaxies: geometry, a probability function of dimming as a function of galaxy mass and radius, and its dependence on wavelength.

Zoom recording: https://uky.zoom.us/rec/share/ApA_YxbNmZhyvRh6jOJV2-1oZh-8L1zw9O_kKivxWqPvTl1eiVTbv07if7cFx0bO.v9GsO7V4klwdB90p

Interstellar dust is still a dominant uncertainty in Astronomy, limiting precision in e.g., cosmological distance estimates and models of how light is re-processed within a galaxy. When a foreground galaxy serendipitously overlaps a more distant one, the latter backlights the dusty structures in the nearer foreground galaxy. Such an overlapping or occulting galaxy pair can be used to measure the distribution of dust in the closest galaxy with great accuracy. The STARSMOG program uses Hubble to map the distribution of dust in foreground galaxies in fine (<100 pc) detail. Integral Field Unit (IFU) observations will map the effective extinction curve, disentangling the role of fine-scale geometry and grain composition on the path of light through a galaxy. The overlapping galaxy technique promises to deliver a clear understanding of the dust in galaxies: geometry, a probability function of dimming as a function of galaxy mass and radius, and its dependence on wavelength.

Zoom recording: https://uky.zoom.us/rec/share/ApA_YxbNmZhyvRh6jOJV2-1oZh-8L1zw9O_kKivxWqPvTl1eiVTbv07if7cFx0bO.v9GsO7V4klwdB90p

The 7 Ms Chandra X-ray Observatory exposure on the Chandra

Deep Field-South (CDF-S) has provided the most sensitive

extragalactic X-ray survey by a wide margin. About 1050

X-ray sources have been detected, primarily distant active

galactic nuclei (AGNs) and starburst/normal galaxies. The

unmatched deep multiwavelength coverage for these sources

allows superb follow-up investigations, revealing the

details of supermassive black hole growth over most of

cosmic time. I will briefly describe the sources in the

7 Ms CDF-S and highlight some exciting science results.

The latter will include (1) evidence for black-hole vs.

bulge co-evolution in the distant universe; (2) constraints

on supermassive black hole growth in the first galaxies as

revealed by direct detection and stacking; and (3) the

discovery of representatives of a new population of faint,

fast X-ray transient sources. Finally, I will discuss some

future prospects for X-ray surveys of AGNs in the distant

universe, including the ongoing 5 Ms XMM-SERVS survey of

the LSST Deep Drilling Fields and new X-ray missions.

The 7 Ms Chandra X-ray Observatory exposure on the Chandra

Deep Field-South (CDF-S) has provided the most sensitive

extragalactic X-ray survey by a wide margin. About 1050

X-ray sources have been detected, primarily distant active

galactic nuclei (AGNs) and starburst/normal galaxies. The

unmatched deep multiwavelength coverage for these sources

allows superb follow-up investigations, revealing the

details of supermassive black hole growth over most of

cosmic time. I will briefly describe the sources in the

7 Ms CDF-S and highlight some exciting science results.

The latter will include (1) evidence for black-hole vs.

bulge co-evolution in the distant universe; (2) constraints

on supermassive black hole growth in the first galaxies as

revealed by direct detection and stacking; and (3) the

discovery of representatives of a new population of faint,

fast X-ray transient sources. Finally, I will discuss some

future prospects for X-ray surveys of AGNs in the distant

universe, including the ongoing 5 Ms XMM-SERVS survey of

the LSST Deep Drilling Fields and new X-ray missions.

Over the past decades, the discovery of a large number of young massive clusters (YMCs) in the local Universe and giant clumps in high-z galaxies suggests that clustered star formation is the dominant star formation mode across cosmic time. Mass and energy feedback from these enormous clusters is inevitably responsible for shaping their host galaxies. In this talk, I will discuss the tight relationship between giant molecular clouds on small scales and galaxies on large scales and provide the first attempts to bring star formation and galaxy formation community together. On the one hand, the properties of YMCs and GMCs populations can be used to calibrate and help improve the current cosmological simulations. On the other hand, galaxy formation simulations provide the perfect initial conditions for the modeling GMCs in realistic environments. Finally, bringing together the collective wisdom from both galaxy and star formation, I will highlight some of my recent works on solving the mystery of the origin of globular cluster populations in the Universe.

Zoom Recording: https://uky.zoom.us/rec/share/gU3PD8lWcY7ckp8yX1hzar4ehA2fRStP3in6YZPpUFYvsIVbmRrsxNpoHvP3qCOw.8tPxhtnTxMA4vByE

Over the past decades, the discovery of a large number of young massive clusters (YMCs) in the local Universe and giant clumps in high-z galaxies suggests that clustered star formation is the dominant star formation mode across cosmic time. Mass and energy feedback from these enormous clusters is inevitably responsible for shaping their host galaxies. In this talk, I will discuss the tight relationship between giant molecular clouds on small scales and galaxies on large scales and provide the first attempts to bring star formation and galaxy formation community together. On the one hand, the properties of YMCs and GMCs populations can be used to calibrate and help improve the current cosmological simulations. On the other hand, galaxy formation simulations provide the perfect initial conditions for the modeling GMCs in realistic environments. Finally, bringing together the collective wisdom from both galaxy and star formation, I will highlight some of my recent works on solving the mystery of the origin of globular cluster populations in the Universe.

Zoom Recording: https://uky.zoom.us/rec/share/gU3PD8lWcY7ckp8yX1hzar4ehA2fRStP3in6YZPpUFYvsIVbmRrsxNpoHvP3qCOw.8tPxhtnTxMA4vByE

Magnetic fields in the intracluster medium (ICM) affect the structure and the evolution of galaxy

clusters. However, their properties are largely unknown, and measuring magnetic fields in galaxy

clusters is challenging, especially on large-scales outside of individual radio sources. Here we

probe the plane-of-the-sky orientation of magnetic fields in clusters using the intensity gradients.

The technique is a branch of the Gradient Technique (GT) that employs emission intensity maps

from turbulent gas. We utilize the Chandra X-ray images of the Perseus, M 87, Coma, and

A2597 galaxy clusters, and the VLA radio observations of the synchrotron emission from

Perseus. We find that the fields predominantly follow the sloshing arms in Perseus, which is in

agreement with numerical simulations. The GT-predicted magnetic field shows signatures of

magnetic draping around rising bubbles driven by supermassive black hole (SMBH) feedback in

the centers of cool-core clusters, as well as draping around substructures merging with the Coma

cluster.

Zoom Recording: https://uky.zoom.us/rec/share/mkGB72TcxVuohGMJ5EVwN282koaKcMinbki7FuSKX3UvAwcl4j22df-zG5VZJnS_.gnvslk37Wx91DbZZ

Magnetic fields in the intracluster medium (ICM) affect the structure and the evolution of galaxy

clusters. However, their properties are largely unknown, and measuring magnetic fields in galaxy

clusters is challenging, especially on large-scales outside of individual radio sources. Here we

probe the plane-of-the-sky orientation of magnetic fields in clusters using the intensity gradients.

The technique is a branch of the Gradient Technique (GT) that employs emission intensity maps

from turbulent gas. We utilize the Chandra X-ray images of the Perseus, M 87, Coma, and

A2597 galaxy clusters, and the VLA radio observations of the synchrotron emission from

Perseus. We find that the fields predominantly follow the sloshing arms in Perseus, which is in

agreement with numerical simulations. The GT-predicted magnetic field shows signatures of

magnetic draping around rising bubbles driven by supermassive black hole (SMBH) feedback in

the centers of cool-core clusters, as well as draping around substructures merging with the Coma

cluster.

Zoom Recording: https://uky.zoom.us/rec/share/mkGB72TcxVuohGMJ5EVwN282koaKcMinbki7FuSKX3UvAwcl4j22df-zG5VZJnS_.gnvslk37Wx91DbZZ