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CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
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SEQUENCE:0
UID:UW-Physics-Event-1589
DTSTART:20090908T203000Z
DURATION:PT1H0M0S
DTSTAMP:20260506T172137Z
LAST-MODIFIED:20090831T191026Z
LOCATION:3425 Sterling Hall
SUMMARY:NCG 205 and M32\, Understanding Andromeda's Tidally Distorted 
 Satellites\, Astronomy Colloquium\, Kirsten Howley\, Univeristy of Cal
 ifornia - Santa Cruz
DESCRIPTION:<br><br>
\nNGC 205 and M32 are close satellites of the And
 romeda (M31) galaxy\, and are our nearest examples of a dwarf elliptic
 al (dE) and compact	elliptical (cE) galaxy\, respectively. Photometric
  observations strongly suggest NGC 205 and M32 are currently undergoin
 g tidal distortion from their interaction with M31. In NGC 205\, this 
 conclusion is strengthened by the observation of an unusual velocity p
 rofile. Despite earlier attempts\, the orbit and progenitor properties
  of NGC 205 are not well known. We perform an optimized search for the
 se unknowns by combining a genetic algorithm with restricted N-body si
 mulations of the interaction. Using NGC 205's photometric and kinemati
 c observations as constraints\, we carry out an effective exploration 
 of the parameter space that defines the orbit and internal structure/d
 ynamics of the progenitor satellite. We find that orbits best matching
  the observables place NGC 205 on primarily radial orbits moving from 
 the Northwest to the Southeast with the satellite currently residing j
 ust behind M31. NGC 205's velocity appears near escape velocity\, sign
 ifying it is likely on its first M31 passage. We also present Keck DEI
 MOS observations of M32's stellar kinematics well beyond the r &lt\; 4
  arc sec region probed in previous studies. The task is made challengi
 ng by the fact that M32 is projected against the bright/complicated in
 ner regions of M31. Long-slit integrated light spectroscopy is used to
  measure the rotation curve of M32 out to a radius of about 1 arcmin. 
 Beyond this radius\, we present constraints based on multislit spectro
 scopy of resolved stars. The velocity distributions from the latter da
 ta set reveal a distinct M32 component. A by-product of our M32 study\
 , is the characterization of the kinematics of the underlying M31 disk
  and inner spheroid.<br><br>
\n
URL:https://www.physics.wisc.edu/events/?id=1589
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