Research Interests:
I observe the infrared and radio emission from
star formation in local galaxies, and particularly in galaxies
with active star formation called "starbursts." Within starbursts,
I been observing the emission from "supernebulae" surrounding
young, super star clusters in the process of forming. These clusters
are so young that they are still hidden within clouds of gas and dust.
With the Keck
Telescope, which is jointly operated by the University of
California, Caltech, and NASA on Mauna Kea, Hawaii,
I observe young super star clusters
in the infrared. Infrared emission is relatively impervious to extinction
by interstellar dust and allows us an unobstructed view into
the heart of the gas clouds surrounding young clusters.
The Keck telescope image from the Keck Observatory webpage as
modified by J.T. Click for larger image
I also use radio telescopes such as the National Science Foundation's
Very Large Array
of the National Radio Astronomy
Observatory to make high resolution images of radio continuum emission
from young stars.
Radio continuum emission is emitted by hot nebulae surrounding
the most massive young stars, stars that are less than a few million years
old.
Like infrared emission but even more so, radio continuum
emission, is unaffected by the dust extinction. Radio images are often the
most reliable way to image these young clusters.
On the surface of one of the 25 meter VLA dishes
Cold gas provides the fuel for star formation. To understand the star formation
process, one must know the distribution of the cold gas fuel and its relation
to the young stars and nebulae.
I observe spectral lines to trace
gas such as the 21 cm line of atomic hydrogen, and the 2.6 and
1.3 mm lines of carbon monoxide (CO).
My students and I often use
the
Owens Valley Millimeter Array,
and the
Caltech Submillimeter Observatory to study gas in galaxies.
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Last modified 5-JAN-2004
