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DTSTAMP:20260609T041029Z
SUMMARY:CASPER Seminar: Ron Wilhelm, Texas Tech University: "The Halo of the Milky Way"
DESCRIPTION;ENCODING=QUOTED-PRINTABLE: Our home galaxy, the Milky Way, is a disk-type galaxy surrounded by a nearly spherical distribution of ancient stars which constitute the Galactic halo.  Because these stars are some of the oldest stars in the Galaxy,  they are an excellent tracer population of the kinematics and chemical properties of  the Milky Way dating back to the time of formation.  In my talk I will contrast the orderly, monolithic collapse model for the formation of the Galaxy from the observations of the 1960's with current day studies which present a halo filled with stellar substructure from tidal streams of disrupts dwarf satellite galaxies.   These streams not only suggest a halo that formed from deposited stellar populations but can also be used to help constrain the distribution of dark matter in the Galaxy.=0D=0A=
	The great advances to our understanding of the halo has arisen from large scale surveys such as the Sloan Digital Sky Survey (SDSS).  I will discuss how photometry and spectroscopy obtained from SDSS can be used to determine the important stellar parameters of temperature, surface gravity, chemical abundance, radial velocity, and distance.  Using these stellar parameters we can explore the properties of the halo streams and the global properties of the halo.  I will present current comparisons of kinematics for stars in the Sagittarius stream to theoretical models which help to constrain the shape of the dark matter halo.  I will also show new results from a global analysis of the halo which suggest that the halo is composed of two distinct components, an inner halo and outer halo.  The kinematics of the outer halo component strongly suggest an accreted origin.  =0D=0A=
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Dr. Wilhelm graduated with a BS in Physics from Bowling Green State University in 1985 and also received his MS from Bowling Green under the guidance of Dr. John Laird in 1989. Dr. Wilhelm received the PhD. from Michigan State University under Dr. Timothy Beers in 1995.  He was a research associate at McDonald Observatory until 1999 and a tenure-track assistant professor at Southwestern University until 2001.  He is currently an associate professor at Texas Tech University.  Wilhelm’s research is primarily involved with the determination of stellar parameters of stars in the halo of our Galaxy.  He is a member in the Sloan Extension for Galactic Understanding and Exploration (SEGUE) and has contributed to the stellar parameter software pipeline.  Wilhelm is also involved with research concerning the high velocity clouds in the halo of the Galaxy and with the properties of hot stars in the Canis Major Over-density.  =0D=0A=
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LOCATION:BSB C.231
DTSTART;TZID=US_Central:20081010T140000
DTEND;TZID=US_Central:20081010T150000
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