October 2014
The Origin of an Ultracompact
Dwarf Galaxy and Its Black Hole
Figure 4.
Upper panels show
near-infrared continuum
and Paschen α images
of target P35 and its
associated HII region.
The position-velocity
plot (c) around the
wavelength of Brackett
γ is extracted from the
GNIRS longslit spectrum
(whose location is
marked with horizontal
lines in the upper
panels). Low surface
brightness features
marked with arrows in
(b) are evident in the
position-velocity plot.
Figure 5.
The black hole mass
is derived from
dynamical modeling,
where the stellar CO
bandhead provides
the kinematic
information. This
figure shows the
goodness-of-fit
measurement
considering variations
in black hole mass
and stellar mass-tolight ratio, calculated
at the discrete green
points. Contours
mark the 1, 2, and 3σ
confidence levels.
26
eter (NIFS), both on the Gemini North telescope, provide spectroscopy with a resolution of around 50 kilometers per second.
Sample stars located near the Arches cluster
are similar to the cluster population (in terms
of age, mass, and spectral characteristics),
suggesting that they were originally cluster
memb \