Research

I study how magnetic fields influence nearby high-latitude molecular clouds (HLCs) with Dr. Archana Soam. These clouds form from magnetically-guided gas flows created by supernova shells and expanding bubbles. Most HLCs are diffuse and non-star-forming, but MBM 12 (Lynds 1457/1458) is a rare case of a star-forming high-latitude cloud. Its proximity (∼100 pc) and active star formation make MBM 12 an ideal testbed. My research goal is to map MBM 12’s magnetic field and understand its role in the cloud’s structure and star formation.

Scientific Goals

This project aims to characterize the magnetic field structure of the high-latitude molecular cloud MBM 12 by combining large-scale dust polarization data from Planck with optical starlight polarization measurements. By probing the magnetic field across different density regimes, the study seeks to understand how magnetic fields influence cloud structure, dust grain alignment, and the earliest stages of star formation.

  • Map the three-dimensional magnetic field
    Combine Planck 353 GHz dust polarization data (~10’ resolution) with R-band starlight polarization of background stars to reconstruct the magnetic field geometry across MBM 12. Planck traces the large-scale plane-of-sky magnetic field in diffuse regions, while optical polarization measurements toward individual background stars provide line-of-sight sampling through the cloud. Together, these datasets will allow the magnetic field structure to be traced from the diffuse outskirts into the denser interior of the cloud.

  • Analyze magnetic field–structure alignment
    Quantify the relative orientation between the magnetic field and the filamentary structures within MBM 12. Studies of nearby molecular clouds have shown that the magnetic field often aligns with low-density striations but becomes perpendicular to dense filaments above column densities of approximately 1.6 × 10^21 cm^-2. We will test whether MBM 12 exhibits a similar transition and examine how the field geometry varies across different density regimes.

  • Quantify dust grain alignment efficiency
    Investigate how the polarization fraction varies with column density to evaluate the efficiency of dust grain alignment in the cloud. Previous comparisons between optical polarization and Planck dust polarization at high Galactic latitudes show strong consistency, suggesting similar dust properties across environments. We will examine whether MBM 12 follows the same behavior and whether grain alignment efficiency changes toward denser regions.

  • Explore the connection to star formation
    Assess whether the magnetic field geometry has influenced the formation of dense cores and young stellar objects within MBM 12. Earlier multiband polarimetric studies suggest that the cloud is threaded by a relatively ordered magnetic field. By combining new optical polarimetry with large-scale Planck data, this work will refine the magnetic field morphology and investigate its relationship with the distribution of young stars and dense structures in the cloud.

Observational Techniques

I work with data from ground-based and space-borne observatories, including McDonald Observatory, Akari, and Planck. My technical interests include using AI/ML techniques to reconstruct 3D magnetic field morphology from observation.