Embedded Files
My research explores the relationship between planet formation and star cluster formation. I use ground- and space-based telescopes to study protoplanetary disks that reside in clustered star-forming regions, like the Orion Nebula Cluster. By characterizing these disk populations, we can examine how the initial conditions of planet formation are shaped by the stellar birth environment.
HST images of protoplanetary disks in the Orion Nebula Cluster. Image Credit: NASA, ESA, and L. Ricci
Current Projects
Current Projects
Irradiated Disk Chemistry with JWST
Irradiated Disk Chemistry with JWST
Clusters host disk populations that are externally irradiated by massive stars. This radiation may play a crucial role in shaping the chemistry of disks and, by extension, the composition of forming planets. I am the PI of a Cycle 3 JWST program and the American Co-PI of a Cycle 4 JWST program that, together, will use 130 hours of JWST MIRI/MRS time to survey the chemistry of 88 externally irradiated disks in the Orion Nebula Cluster and NGC 1977 Cluster. The goal of these programs is to constrain the impact of external UV radiation on the chemistry of giant, terrestrial, and habitable planet formation.
Clusters host disk populations that are externally irradiated by massive stars. This radiation may play a crucial role in shaping the chemistry of disks and, by extension, the composition of forming planets. I am the PI of a Cycle 3 JWST program and the American Co-PI of a Cycle 4 JWST program that, together, will use 130 hours of JWST MIRI/MRS time to survey the chemistry of 88 externally irradiated disks in the Orion Nebula Cluster and NGC 1977 Cluster. The goal of these programs is to constrain the impact of external UV radiation on the chemistry of giant, terrestrial, and habitable planet formation.
To aid the interpretation of the JWST data, I am also leading a Cycle 26 Chandra program and new Cycles 11 and 12 ALMA programs to measure the stellar X-ray luminosities and mm-dust morphologies of all JWST-targeted irradiated disks.
To aid the interpretation of the JWST data, I am also leading a Cycle 26 Chandra program and new Cycles 11 and 12 ALMA programs to measure the stellar X-ray luminosities and mm-dust morphologies of all JWST-targeted irradiated disks.
Radio Recombination Lines from Proplyds
Radio Recombination Lines from Proplyds
Proplyds are protoplanetary disks surrounded by cocoons of ionized gas with a cometary morphology. These disks are commonly found in nearby star-forming clusters, and their morphologies are produced by gas that has been photoevaporated off the disk and ionized by UV radiation from nearby massive stars. Recently, I led a paper that, for the first time, detected hydrogen and helium radio recombination lines from proplyds in the Orion Nebula Cluster (ONC). Our analysis indicates that radio recombination lines are powerful tracers of external photoevaporation.
Proplyds are protoplanetary disks surrounded by cocoons of ionized gas with a cometary morphology. These disks are commonly found in nearby star-forming clusters, and their morphologies are produced by gas that has been photoevaporated off the disk and ionized by UV radiation from nearby massive stars. Recently, I led a paper that, for the first time, detected hydrogen and helium radio recombination lines from proplyds in the Orion Nebula Cluster (ONC). Our analysis indicates that radio recombination lines are powerful tracers of external photoevaporation.
This work was featured as both NRAO and ALMA press releases.
To follow up on this exciting discovery, I designed the successful large VLA program "PEARRLS: The Proplyd EVLA/ALMA Radio Recombination Survey." PEARRLS will use 140 hours of approved VLA time and 40 hours of approved ALMA time to survey 21 hydrogen and helium radio recombination lines from 20 proplyd disks.
Identifying Photoevaporating Disks with the VLA
Identifying Photoevaporating Disks with the VLA
In young clusters, we expect UV radiation from massive stars to externally photoevaporate disks around low-mass stars. I am leading an effort to identify photoevaporating disk populations with the VLA. In a recent paper, I identified 10 photoevaporating disk candidates in NGC 1977 and measured their mass-loss rates. Currently, I am supervising a University of Virginia undergraduate student who is searching for photoevaporating disks in NGC 2024. Our findings confirm that external photoevaporation is operating in a range of cluster environments.
In young clusters, we expect UV radiation from massive stars to externally photoevaporate disks around low-mass stars. I am leading an effort to identify photoevaporating disk populations with the VLA. In a recent paper, I identified 10 photoevaporating disk candidates in NGC 1977 and measured their mass-loss rates. Currently, I am supervising a University of Virginia undergraduate student who is searching for photoevaporating disks in NGC 2024. Our findings confirm that external photoevaporation is operating in a range of cluster environments.
Disk Demographics in the Orion Nebula Cluster
Disk Demographics in the Orion Nebula Cluster
The Orion Nebula Cluster hosts hundreds of photoevaporating disks. In my dissertation, I analyzed deep, high angular resolution ALMA molecular line observations of disks in the Orion Nebula Cluster. My findings, as described here and here, indicate that disks in the Orion Nebula Cluster are smaller and more rich in gas-phase CO than disks in lower-density star-forming regions, likely due to external radiation from nearby massive stars. To build off my dissertation, I am leading as PI a Cycle 11 ALMA program and a Semester 2024B VLA program to measure the masses of Orion Nebula Cluster disks with combined ALMA Band 1 and VLA Q-band observations. Much of the data reduction is now being led by a University of Virginia undergraduate student that I am supervising.
The Orion Nebula Cluster hosts hundreds of photoevaporating disks. In my dissertation, I analyzed deep, high angular resolution ALMA molecular line observations of disks in the Orion Nebula Cluster. My findings, as described here and here, indicate that disks in the Orion Nebula Cluster are smaller and more rich in gas-phase CO than disks in lower-density star-forming regions, likely due to external radiation from nearby massive stars. To build off my dissertation, I am leading as PI a Cycle 11 ALMA program and a Semester 2024B VLA program to measure the masses of Orion Nebula Cluster disks with combined ALMA Band 1 and VLA Q-band observations. Much of the data reduction is now being led by a University of Virginia undergraduate student that I am supervising.
Previous Projects
Previous Projects
Molecular Cloud Turbulence Statistics
Molecular Cloud Turbulence Statistics
My undergraduate research involved analyzing synthetic observations of turbulent molecular clouds. I used common astrostatistics, such as principal component analysis, to constrain the impact of stellar feedback on molecular cloud turbulence. We identified several statistical diagnostics that can be used to pinpoint wind-driven stellar feedback in CO and CI observations of molecular clouds. My undergraduate research led to two first-author papers (Paper I and Paper II). It also contributed to the development of TurbuStat, a Python package for applying turbulence statistics to spectral line data cubes.
My undergraduate research involved analyzing synthetic observations of turbulent molecular clouds. I used common astrostatistics, such as principal component analysis, to constrain the impact of stellar feedback on molecular cloud turbulence. We identified several statistical diagnostics that can be used to pinpoint wind-driven stellar feedback in CO and CI observations of molecular clouds. My undergraduate research led to two first-author papers (Paper I and Paper II). It also contributed to the development of TurbuStat, a Python package for applying turbulence statistics to spectral line data cubes.
Page updated
Google Sites
Report abuse