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Event Details

Description: Join us at the Metro location for the third presentation of the Women & Diversity in STEM series "Contributions to the Galactic Stellar Halo from In-Situ, Kicked-Out Disk, and Accreted Stars," presented by Kevin Woo.
More Info: Where did stars in the Milky Way's halo form? The LCDM model predicts that the Milky Way's halo was built in a "bottom-up" fashion, and this view is now generally accepted due to overwhelming evidence of the relics of past mergers. It is still uncertain, however, what fraction of the halo is made up of such accreted debris. Close to the time of accretion, a group of stars formed in a particular satellite of the Milky Way will show coherence spatially, kinematic ally, and chemically. In the inner halo where dynamical timescales are short, spatial coherence will become blurred quickly, although kinematical and chemical coherence remain. Kinematics alone may still lead to ambiguity, as a merger event can cause stars formed in the Milky Way to redistribute into rings in the halo ("kicked-out" dick starts) and these rings can be difficult to distinguish from accreted satellite stars. Thus, to get a more complete profile of a star's formation history, both kinematical and chemical information are needed.
I will report chemical abundances for a sample of M giants in the inner halo of the Milky Way. Abundances are derived for a-elements and neutron capture elements. By analyzing the multi-dimensional abundance space, the formation site of the halo giants-in-situ, kicked-out disk, or accreted- can be assessed. Additionally, I will report results from a study to understand the origin of a diffuse cloud of stars known as Triangulum-Andromeda.
Please register online, light refreshments will be served.
Date: 03/26/2019
Time: 5:00pm
Location: ESC Metropolitan Location
325 Hudson St., 5th Floor
New York, NY 10013-1005
Cost: free
Contact Name: Kevin Woo
Contact Phone: 646-230-1262
Contact E-mail: kevin.woo@esc.edu






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