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

The Javalambre-Physics of the Accelerated Universe Astrophysical Survey (J-PAS) is a narrow band, very wide field cosmological and astrophysical survey to be carried out from the Javalambre Astrophysical Observatory in Spain with a purpose-built, dedicated 2.5m telescope and a 5 sq.deg. 1.2Gpix camera. With first light obtained in June 2020, J-PAS plans to observe >8000sq.deg. of Northern Sky and measure sigma_z~0.003(1+z) photo-z for up to 9E7 LRG and ELG galaxies plus several million QSOs, sampling an effective volume of ~ 14 Gpc^3 up to z~1.3 reaching Stage IV radial BAO experiment. J-PAS is expected to detect ~7E5 galaxy clusters and groups, setting constraints on Dark Energy which rival those obtained from its BAO measurements. 

Thanks to the superb characteristics of the site (seeing ~0.7 arcsec), J-PAS is expected to obtain a deep, sub-arcsec multi-band image of the Northern sky, which combined with its unique photo-z precision will have an immense legacy value for almost all astrophysical areas. The key to the J-PAS potential is its innovative approach: a contiguous system of 54+2 filters with 145A width, placed 100A apart over a multi-degree FoV is a powerful "redshift machine", with the survey speed of a 4000 multiplexing low resolution spectrograph. Its commissioning camera, the PathFinder, has collected data since 2018 with all J-PAS filters of a variety of targets and fields, in particular of the AEGIS field (miniJPAS) as a proof of concept for photo-z depth and others. 

Here I will present the status of J-PAS, the main results of miniJPAS and how it impacts the expectations for J-PAS.

Zoom recording: https://uky.zoom.us/rec/share/F9E1ic1VTD7A1b0uY0c6sWNlWtCvII8N1eESjj8WC4UNIHGTzMJzxRa_mj3iIdnL.ay0DT-aSZ6MRRBTU

The Javalambre-Physics of the Accelerated Universe Astrophysical Survey (J-PAS) is a narrow band, very wide field cosmological and astrophysical survey to be carried out from the Javalambre Astrophysical Observatory in Spain with a purpose-built, dedicated 2.5m telescope and a 5 sq.deg. 1.2Gpix camera. With first light obtained in June 2020, J-PAS plans to observe >8000sq.deg. of Northern Sky and measure sigma_z~0.003(1+z) photo-z for up to 9E7 LRG and ELG galaxies plus several million QSOs, sampling an effective volume of ~ 14 Gpc^3 up to z~1.3 reaching Stage IV radial BAO experiment. J-PAS is expected to detect ~7E5 galaxy clusters and groups, setting constraints on Dark Energy which rival those obtained from its BAO measurements. 

Thanks to the superb characteristics of the site (seeing ~0.7 arcsec), J-PAS is expected to obtain a deep, sub-arcsec multi-band image of the Northern sky, which combined with its unique photo-z precision will have an immense legacy value for almost all astrophysical areas. The key to the J-PAS potential is its innovative approach: a contiguous system of 54+2 filters with 145A width, placed 100A apart over a multi-degree FoV is a powerful "redshift machine", with the survey speed of a 4000 multiplexing low resolution spectrograph. Its commissioning camera, the PathFinder, has collected data since 2018 with all J-PAS filters of a variety of targets and fields, in particular of the AEGIS field (miniJPAS) as a proof of concept for photo-z depth and others. 

Here I will present the status of J-PAS, the main results of miniJPAS and how it impacts the expectations for J-PAS.

Zoom recording: https://uky.zoom.us/rec/share/F9E1ic1VTD7A1b0uY0c6sWNlWtCvII8N1eESjj8WC4UNIHGTzMJzxRa_mj3iIdnL.ay0DT-aSZ6MRRBTU