NGC 2363: Anatomy of a Two-Stage Starburst

Details NGC 2363: Anatomy of a Two-Stage Starburst NGC 2363: Anatomy of a Two-Stage Starburst

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6096d&link_type=abstract

HST Proposal ID #6096

Computer Science

Hst Proposal Id #6096 Stellar Populations

Scientific paper

This proposal aims at identifying the massive star content of NGC 2363, the archetype of a whole class of small but powerful young starbursts with blowout like-properties. NGC 2363 is a large and very luminous metal-poor giant H II region located at the soutwestern end of the magellanic galaxy NGC 2366. It presents an unusual combination of kinematical features, the most outstanding being low-intensity, broad spectral components {FWHM = 2400 kms} in the bright nebular lines H Alpha and O III. These features, detected over a spatial extent of 500 pc, betray very high velocity gas and mimic, at a smaller scale, galactic superwinds of large starburst galaxies. Ground-based imagery suggests that two clusters of massive stars, of different ages, ionize the gas and supply the kinetic energy to the nebula. Identifying the stellar content of NGC 2363 is an essential step in trying to unveal its powerhouse and to understand the intriguing origin of the very high-velocity nebular gas. We propose to obtain optical images and high quality UV spectra of the two ionizing clusters in NGC 2363. The images will be used to assess the starburst history by studying the morphology of the clusters, locating and counting individual Wolf-Rayet and Red Supergiant stars and to determine the spatial extent of the He^++ zone. The continuum slope and the profiles of the UV stellar lines will be analyzed using the most up-to-date population synthesis models to quantify the global characteristics of the upper IMF.

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