Milky Way Halo Group (MWH)
Our research group studies the atmospheres (or “halos”) of the Milky Way and other Local Group galaxies. The halo is a vital component of a galactic ecosystem, being closely connected to the star formation cycle. Gas flows from the halo into the disk play a key role in galaxy growth by providing fuel for star formation. Our group has a long track record of studying the halos of the Milky Way and other nearby galaxies, including the Large and Small Magellanic Clouds. We study key halo properties including chemical abundances, kinematics, and physical conditions using multi-wavelength spectroscopy at UV, optical, IR, and radio wavelengths together with radiative-transfer simulations. The lessons learned from these Local Group studies inform the larger subject of galaxy formation and evolution.
We are part of the Low Density Universe community at STScI. We welcome new collaborators at all career stages. We're interested in questions such as:
- How and where do baryons enter and exit the Milky Way?
- What are the physical and chemical properties of the Galactic halo?
- How did the Magellanic System form and evolve?
- How did the Fermi Bubbles at the Galactic Center form?
- How is interstellar gas distributed around the spiral arms?
We address these questions using a wide range of observational programs using the Hubble Space Telescope and ground based telescopes.
Website: The Milky Way Halo Research Group at STScI
Leads: Andrew Fox, Jason Tumlinson
Members: Francie Cashman, David French, Sapna Mishra, Ravi Sankrit, Debopam Som
Research Topics:
- Local Group Galaxies
- Galaxy Formation and Evolution
- Interstellar Medium
- Intergalactic/circumgalactic medium
- Chemical Abundances
- Milky Way
- Magellanic Clouds
- Galactic Center
- Galactic Structure
- High-velocity Clouds
- Spiral arms
- Photoionization simulations
Seminars/Journal Club: Low Density Universe, Galaxies Journal Club
Related Missions & Instruments: HST, GBT, VLT/UVES, Keck/HIRES, Gemini/NIFS, GTC/MEGARA, HWO, LVM