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

Giant molecular clouds (GMCs) are the primary reservoir of cold molecular gas in the interstellar medium and sites of ongoing star formation. It has been known for decades that star formation efficiency (SFE) of GMCs is very low. While UV radiation feedback from massive stars are expected to play a crucial role in controlling the GMC lifetime and SFE, our theoretical understanding of how it actually works in turbulent, magnetized clouds remains incomplete. In this talk, I will report recent progress we made in modeling GMC destruction by UV radiation feedback. I will first briefly review the predictions made by 1D models about SFE, cloud lifetime, and importance of photoionization and radiation pressure in different star-forming environments. I will then present the results of radiation (magneto)hydrodynamic simulations of star-forming GMCs and discuss how turbulence and magnetic fields can change the picture. If time allows, I will also talk about ongoing efforts in modeling GMC evolution with all major forms of feedback processes (radiation/winds/SNe).

Giant molecular clouds (GMCs) are the primary reservoir of cold molecular gas in the interstellar medium and sites of ongoing star formation. It has been known for decades that star formation efficiency (SFE) of GMCs is very low. While UV radiation feedback from massive stars are expected to play a crucial role in controlling the GMC lifetime and SFE, our theoretical understanding of how it actually works in turbulent, magnetized clouds remains incomplete. In this talk, I will report recent progress we made in modeling GMC destruction by UV radiation feedback. I will first briefly review the predictions made by 1D models about SFE, cloud lifetime, and importance of photoionization and radiation pressure in different star-forming environments. I will then present the results of radiation (magneto)hydrodynamic simulations of star-forming GMCs and discuss how turbulence and magnetic fields can change the picture. If time allows, I will also talk about ongoing efforts in modeling GMC evolution with all major forms of feedback processes (radiation/winds/SNe).

In recent work, we have obtained improved measurements of the properties of the Milky Way and used the results to select a sample of Milky Way analog (MWA) galaxies from the Sloan Digital Sky Survey (SDSS) whose distributions of stellar mass and star formation rate match our Galaxy’s, incorporating all uncertainties. Relying on the Copernican assumption that the Milky Way should not be extraordinary, the colors and luminosities of the MWAs constrain the possible properties of our own Galaxy. This has enabled us to explore how our Galaxy fits in with the broader population; for instance, we can determine whether its properties are consistent with the power-law scaling relations exhibited by other spiral galaxies. The results have significant implications for the development of computational models of galaxy evolution in a cosmological context.  I will also describe follow-up work exploring the population of satellite galaxies in Milky Way-like dark matter halos.  It has been a long-standing puzzle why the Milky Way has considerably fewer satellite galaxies discovered to date than the typical number of satellite dark matter halos that would be found in a dark matter halo as massive as that which contains our Galaxy.  I will show that almost half of this ‘missing satellites’ problem can be explained by well-established ways in which our Galaxy’s dark matter halo is atypical.  Finally, if time allows I will also describe new work on the density profile of dark matter halos when mass within subhalos, which can often host individual galaxies, is not counted as part of the parent halo.  Widely-used profiles (such as Navarro Frenk and White) perform poorly at representing the smooth centrally-concentrated component of the halo, but there are simple functional forms which do better.

Zoom recording: https://uky.zoom.us/rec/play/58uXDQDw95A6o5P7owEDEwzb-X3PhCXv8WevwQSdhV…