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X-WR-CALNAME;VALUE=TEXT:ITC Seminar - Hannah Ubler (MPE)
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SUMMARY:ITC Seminar - Hannah Ubler (MPE)
DESCRIPTION:<span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">Kinematics of z~1–2 star-forming galaxies with KMOS^3D: intrinsic</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">velocity dispersion</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">Abstract: Kinematics are a powerful tool to study galaxy evolution</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">because they are directly affected by transformative processes such as</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">accretion, gravitational instabilities, feedback, or outflows. The</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">incidence or strength of several of these processes changes with cosmic</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">time, allowing us to connect certain kinematic signatures with specific</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">physical processes. I will present recent results on the kinematics of</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">star-forming galaxies during the peak epoch of cosmic star formation</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">from the KMOS^3D survey, with a focus on the redshift evolution of the</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">intrinsic velocity dispersion. Combining observational evidence and</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">theoretical predictions, I will discuss the origin of the elevated</span></span></span></span><br style="color:#222222;Helvetica,sans-serif;background-color:#ffffff"><span><span style="color:#222222"><span style="Helvetica,sans-serif"><span style="background-color:#ffffff">velocity dispersions at high redshift.</span></span></span></span>
LOCATION:Phillips
STATUS:CONFIRMED
DTSTART:20191210T170000Z
DTEND:20191210T180000Z
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