Narrow-Band Images of Star Forming Knots in HII Galaxies

Astronomy and Astrophysics – Astronomy

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Scientific paper

HII galaxies are low-luminosity, metal poor and compact objects with intense star formation activity. Initially it was hypothesized that HII galaxies are young galaxies, forming their first generation of stars. However, Optical-NIR photometry have revealed the existence of an evolved underlying population of old stars, suggesting an intermittent star formation history with short intense star-forming episodes followed by long quiescent phases.
HII galaxies in general are simple systems compared to other galaxies, more massive galaxies, and many of them have more than one starburst component, turning these objects in excellent laboratories to study the star-formation mechanism, supernova winds and chemical evolution. Due to their intense emission lines, HII galaxies have been common targets of spectroscopic works. These have biased the results to the location of the brightest regions where slits have been positioned.
Using narrowband Hβ and true continuum images obtained with the NTT telescope on La Silla, we have studied a selected HII galaxies, producing continuum free Hβ emission lines images. The images revealed a myriad of blobby structures due to the presence of multiple star forming knots, filaments or possible expanding shells, probably superbubbles.
>From these we could map the distribution of luminosity and EW over the whole extension of the galaxies. Our integrated Hβ flux, over similar apertures, is in good agreement with the slit spectroscopy. However, the EW (Hβ) distribution is non-uniform and varies significantly over the different star forming knots. Thus, integrated values appear only as an average of the star forming regions, hampering the fine determination of individual star cluster ages.

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