Star Formation in NGC4449: MAMA-Detector UV Imagery and Fabry-Perot Balmer-Line Imagery

Details Star Formation in NGC4449: MAMA-Detector UV Imagery and Fabry-Perot Balmer-Line Imagery Star Formation in NGC4449: MAMA-Detector UV Imagery and Fabry-Perot Balmer-Line Imagery

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...182.3108s&link_type=abstract

American Astronomical Society, 182nd AAS Meeting, #31.08; Bulletin of the American Astronomical Society, Vol. 25, p.841

Astronomy and Astrophysics

Astronomy

Scientific paper

NGC 4449 is a Magellanic irregular galaxy with vacuum ultraviolet (VUV) luminosity comparable to late-type spirals and greater than that of the LMC by ~ 2.5 mag, indicating substantial star formation in the last 10(8) yr. Using VUV and Balmer-line images, we investigate the star formation history of 22 large OB complexes during this recent time interval. A group of VUV and Hα sources in the north of the galaxy, associated with a particular Hi feature, is producing stars actively at the present time. By contrast, VUV sources along the northeast-southwest surface brightness ridgeline (the ``bar'') appear to be less active at the present, though star formation has clearly occurred in the last 10(7) yr, and morphology suggestive of multigeneration star formation is seen. Over the entire galaxy, star formation rates are consistent on time scales of 10(6) , 10(8) , and 10(9) yr, confirming the results of previous investigators. Red and blue continuum images show dust features in the neighborhood of the ridgeline with a filamentary morphology coherent over ~ 100 pc. Imagery in Hα confirms the ionized-gas morphology found by previous investigators, including many compact knots, as well as radial filaments, loops, and ``froth'' filling the visible system. A partial oval of bright Hii regions is found along the ridgeline, as are the most luminous VUV sources.

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