A Lifetime of Influence: Abstracts, Talks, and Posters
 

Barbosa

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Bastian

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Blum

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Brott

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Caballero

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Chen

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Churchwell

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Corcoran

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Damineli et al

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Damineli

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Fullerton

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Gagne

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Georgiev

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Hamann

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Hillier

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Howarth

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Indebetouw

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Kobulnicky

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Koenigsberger

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Lang

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Leitherer

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Linder

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Naze

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Smith

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Soderberg

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Teodoro

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Townsley

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Vacca

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Walborn

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Whelan

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Williams

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Willis

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Wing

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Wolff

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van den Heuvel

  

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Massive Star Formation in LMC HII Complexes

C.-H. Rosie Chen
University of Virginia

You-Hua Chu
University of Illinois

Robert Gruendl
University of Illinois

Karl Gordon
Space Telescope Science Institute

Fabian Heitsch
University of Michigan

Remy Indebetouw
University of Virginia

We use the HII complexes N44 and N159 in the Large Magellanic Cloud (LMC) to perform a detailed study of star formation in a mild starburst, as they host regions of star formation at different evolutionary stages and are not as complicated and confusing as the 30 Doradus giant HII region. We have used Spitzer IRAC and MIPS observations and complementary ground-based uBVIJK observations to identify candidate massive young stellar objects (YSOs) in these two HII complexes. We further classify the YSOs into Types I, II, and III, according to their spectral energy distributions (SEDs). In our sample of YSO candidates in N44 and N159, more than half of them are resolved into multiple components or extended sources in high-resolution ground-based images. We have modeled the SEDs of YSOs that appear single or dominant within a group. We find good fits for Types I and I/II YSOs, but Types II and II/III YSOs show deviations between their observed SEDs and models that do not include PAH emission. We have also found that some Type III YSOs have central holes in their disk components. YSO counterparts are found in ultracompact HII regions and their stellar masses determined from SED model fits are compared with those estimated from the ionization requirements of the HII regions. The distribution of YSOs is compared with those of the underlying stellar population and interstellar gas conditions to illustrate a correlation between the current formation of O-type stars and previous formation of massive stars. Evidence of triggered star formation is also presented.