A High Resolution View of Galactic Centers: Arp 220 and M31.
A High Resolution View of Galactic Centers: Arp 220 and M31.
Date
2017-08
Authors
Lockhart, Kelly E.
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Astronomy
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The centers of galaxy are small in size and yet incredibly complex. They play host
to supermassive black holes and nuclear star clusters (NSCs) and are subject to large gas
in
ows, nuclear starbursts, and active galactic nuclear (AGN) activity. They can also be
the launching site for large-scale galactic out
ows. However, though these systems are quite
important to galactic evolution, observations are quite di cult due to their small size.
Using high spatial resolution narrowband imaging with HST/WFC3 of Arp 220, a latestage
galaxy merger, I discover an ionized gas bubble feature (r = 600 pc) just o the
nucleus. The bubble is aligned with both the western nucleus and with the large-scale
galactic out
ow. Using energetics arguments, I link the bubble with a young, obscured
AGN or with an intense nuclear starburst. Given its alignment along the large-scale out
ow
axis, I argue that the bubble presents evidence for a link between the galactic center and
the large-scale out
ow.
I also present new observations of the NSC in M31, the closest large spiral galaxy to
our own. Using the OSIRIS near-infrared integral eld spectrograph (IFS) on Keck, I map
the kinematics of the old stellar population in the eccentric disk of the NSC. I compare the
observations to models to derive a precession speed of the disk of 0 5 km s1 pc1, and
hence con rm that winds from the old stellar population may be the source of gas needed
to form the young stellar population in the NSC.
Studies of galactic centers are dependent on high spatial resolution observations. In
particular, IFSs are ideal instruments for these studies as they provide two-dimensional
spectroscopy of the eld of view, enabling 2D kinematic studies. I report on work to
v
characterize and improve the data reduction pipeline of the OSIRIS IFS, and discuss
implications for future generations of IFS instrumentation.
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