Welcome to FANG!
What drives the evolution of galaxies? One of the most important
factors is energetic feedback from massive stars. The hottest, most
massive stars produce vast quantities of UV ionizing
radiation, and end their short lives as supernova explosions. These
shocks generate hot gas in galaxies and synthesize the chemical
elements in the universe. The stars themselves are also responsible
for photoionizing discrete nebulae, diffuse interstellar medium, and
the early cosmos itself. All of these effects originating from the
massive star population are fundamental drivers of galaxy evolution.
In addition, the relationships between stellar and gaseous galactic
components on all scales form the basis for interpreting observations of
galaxies and phenomena in the distant universe.
Sally Oey's research group, Feedback Activity in Nearby Galaxies
(FANG), focuses on this massive star feedback
to the interstellar and intergalactic medium, on local, global, and
cosmic scales.
- Massive stars and clusters
- Radiative feedback: HII regions, Lyman continuum-emitting galaxies
- Kinematic feedback: Supernova-driven superbubbles and
galactic superwinds
- Chemical feedback: Enrichment processes and galactic chemical evolution
CURRENT PROGRAMS
The escape of ionizing radiation from galaxies and super
star clusters is a fundamental problem that is poorly understood.
What conditions allow ionizing radiation to penetrate the dense
gas in star-forming clouds and the interstellar medium? We are
currently studying extreme, local starbursts to clarify these
processes. Some are resolved objects like Mrk 71 and Haro 11, while others are
intense, high-ionization objects like the "Green Pea" galaxies.
Our group is at the forefront of establishing a new paradigm for
massive-star feedback, where superwinds from compact young star
clusters are suppressed by catastrophic cooling and high interstellar
pressure.
Hubble image of starburst galaxy Haro 11 in [O II] (WFC3/FQ378N), [O III]
(ACS/F505N), and U (ACS/F336W).
From a paper by undergraduate
Ryan Keenan et al. (2017).
Field massive stars are a key probe of massive star-forming
processes. How many are runaways ejected from clusters, and how many
form in relative isolation? Our Runaways and Isolated O-Type Star
Spectroscopic Survey of the SMC (RIOTS4) has been generating a wealth
of data for a spatially complete sample in this nearby galaxy. We are
quantifying the properties of this luminous,
but enigmatic, stellar population, obtaining mass, radial velocity,
proper motion, spin, binarity, and other properties. We are
establishing the origins of field stars due to
dynamical ejections from clusters, acceleration by supernova kicks,
and in-situ formation in the field.
Residual proper motions of RIOTS4 field OB stars in the Small Magellanic Cloud.
Figure made by undergraduate Johnny Dorigo Jones, in
Oey et al. (2018).
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