The intricate web of magnetic fields threading the Galaxy plays a fundamental role in a plethora of astrophysical phenomena, from the enigmatic origins of ultra-high-energy cosmic rays to the process of star formation. Despite their significance, directly measuring the three-dimensional (3D) magnetic fields within the interstellar medium (ISM) remains a formidable challenge. Driven by an enriched comprehension of magnetohydrodynamic (MHD) turbulence, this project proposes innovative methodologies to trace and characterize the orientation and strength of 3D magnetic fields:

3D Galactic magnetic field:

1. Mapping the Galactic magnetic field orientation and strength in three dimensions. arXiv:2302.05047

2. Anisotropic turbulence in PPV space: probing three-dimensional magnetic fields. arXiv:2104.02842.

3. Anisotropies in compressible MHD turbulence: probing magnetic fields.  arXiv:2012.06039. 

3D magnetic fields in star-forming regions:

1. Probing three-dimensional magnetic fields: I -- polarized dust emission. arXiv:2203.09745.

2. Probing three-dimensional magnetic fields: II -- interpretable convolutional neural network. arXiv:2310.12555

3. Characterizing three-dimensional magnetic field, turbulence, and self-gravity in the star-forming region L1688. arXiv:2210.11023

4. Velocity gradients: magnetic field tomography towards the supernova remnant W44. arXiv: 2109.13670. 

Magnetic fields interwoven within the Intracluster Medium (ICM) exert a substantial influence on the evolution of galaxy clusters. Despite their fundamental role, the properties of these magnetic fields remain largely enigmatic, with their measurement presenting a significant challenge. This project aims to probe the magnetic fields in the ICM by examining their association with both thermal X-ray emission, and non-thermal radio emission. By applying advanced methodologies to these observations, we have achieved the first-ever measurement of magnetic field topology within radio halos.

Magnetic fields in the galaxy clusters:

1. Probing the magnetic field in galaxy clusters with the gradient technique.  arXiv:2007.06219. 

2. Synchrotron intensity gradient revealing magnetic fields in galaxy clusters, Nature Communications.

3. Probing three-dimensional magnetic fields: III -- synchrotron emission and machine learning. arXiv:2404.07806.

4. Tracing magnetic fields with the GT: spatial filtering and use of interferometers. arXiv:2208.06074. 

The magnetic field is a pivotal yet enigmatic force within the Central Molecular Zone (CMZ) and galaxies at large. To elucidate the complexities of magnetic fields in the CMZ and neighboring galaxies, this project leverages a multi-wavelength observational strategy. We combine neutral and ionized gas spectroscopic observations, radio polarization data, and far-infrared polarization measurements. Through this rich dataset, we generate detailed magnetic field maps, facilitating an in-depth analysis of how magnetic fields contribute to the dynamics of galactic nuclei and the orchestration of interstellar processes. 

Multi-scale and 3D magnetic fields in the Central Molecular Zone:

1. Multi-scale magnetic fields in the central molecular zone. arXiv:2105.03605. 

2. Decomposing magnetic fields in three dimensions over the central molecular zone. arXiv:2201.07970.

Magnetic fields in nearby galaxies:

1. Role of magnetic fields in fueling Seyfert nuclei. arXiv:2206.05423 

2. Multiphase magnetic fields in the galaxy NGC 3627. arXiv:2208.06090 

Magnetohydrodynamic (MHD) turbulence represents a cornerstone component within the Interstellar Medium (ISM) and Intracluster Medium (ICM), with its influence extending across a vast spectrum of scales—from hundreds of parsecs down to sub-astronomical units. This project is dedicated to an in-depth examination of MHD turbulence and its related astrophysical manifestations through the lens of cutting-edge simulations.

Cosmic ray transport:

1. Superdiffusion of CRs in compressible magnetized turbulence.  arxiv:2111.15066. 

Turbulent dynamo:

1. Turbulent magnetic field amplification by the interaction of shock wave and inhomogeneous medium. arXiv:2207.06941. 

Turbulence damping due to neutral-ion decoupling:

1. Damping of turbulence in a partially ionized medium. arXiv:2306.10005. 

Deciphering the regulatory mechanisms of star formation necessitates a comprehensive analysis of the interplay among turbulence, magnetic fields, stellar feedback, and gravitational forces within molecular clouds. This project endeavors to dissect the characteristics of turbulence and magnetic field structures within star-forming regions. By integrating state-of-the-art numerical simulations with high-resolution spectroscopic observations, we aim to illuminate the intricate dynamics at play in these stellar nurseries.

Turbulence in star formation:

1. The velocity statistics of turbulent clouds in the presence of outflow feedback. arXiv:2203.01508.

2. Velocity gradient in the presence of self-gravity: identifying inflows. arXiv:2002.06754.

Magnetic fields in star formation:

1. Magnetic field morphology with velocity gradient technique in Interstellar Clouds.  Nature Astronomy 

2. Revealing gravitational collapse in the Serpens G3-G6 molecular cloud. arXiv:2102.06225.

3. Tracing multi-scale magnetic field structure in GMC. arXiv:1904.04391.

Observations of the Cosmic Microwave Background (CMB) polarization yield invaluable insights into the primordial inhomogeneities of the universe. However, these signals are muddied by the polarization of the Galactic foreground. This project aims to model the Galactic foreground with the aid of atomic neutral hydrogen data. Our goal is to enhance the clarity of CMB data, thereby sharpening our view of the universe's earliest epochs. 

Modeling of the Galactic foreground polarization:

1. Predictions of CMB foregrounds dust polarization using velocity gradient.  arXiv:1910.05637. 

2. Modeling of galactic foreground polarization with velocity gradients. arXiv:2007.02184. 

3. Improving the accuracy of magnetic field tracing by velocity gradients: PCA. arXiv:1802.08772.

4. Intensity gradients technique: synergy with velocity gradients and polarization. arXiv:1908.09488.

5. Nature of striation in 21 cm channel Maps: Velocity caustics. arXiv:2306.10005.