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PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:0
UID:UW-Physics-Event-3507
DTSTART:20141017T170000Z
DTEND:20141017T180000Z
DTSTAMP:20260419T172241Z
LAST-MODIFIED:20141016T141426Z
LOCATION:4421 Sterling Hall
SUMMARY:The Structure of the Faintest Dwarf Galaxies\, Special Astrono
 my Talk\, Ken Freeman\, ANU College of Physical and Mathematical Scien
 ces
DESCRIPTION:The faintest dwarf galaxies are very baryon-depleted and h
 ave large<br>
\nM/L ratios.  Their gravitational fields are dominated 
 by their dark halos.<br>
\nIf the dark halos have cores of near-consta
 nt surface density\, and the<br>
\nbaryons have isotropic kinematics a
 nd are close to isothermal as observed\,<br>
\nthen the density distri
 bution of the baryons is expect to have a simple<br>
\nanalytic form w
 hich we can use to measure the central densities of their<br>
\ndark h
 alos. The observed density distributions of the faintest dwarf<br>
\ns
 pheroidal and dwarf irregular galaxies appear to follow this expected<
 br>
\ndistribution.<br>
\n<br>
\nThe core radii and central densities 
 of the dark halos of rotationally<br>
\ndominated late-type spirals sc
 ale with their absolute magnitudes: the<br>
\ndensities decrease with 
 luminosity and the core radii increase\, with<br>
\nthe central surfac
 e densities of the halos being almost independent of<br>
\nlumiosity. 
 I will talk about the consequences of these scaling laws and<br>
\nsom
 e other correlations for the epoch of formation of the dwarfs\, the<br
 >
\nsizes of their dark halos and  the existence of dark dwarfs.
URL:https://www.physics.wisc.edu/events/?id=3507
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