Contents of: VI/111/./abstract/BMCBREEN_WRHIIGAL.abs

The following document lists the file abstract/BMCBREEN_WRHIIGAL.abs from catalogue VI/111.
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==> In this proposal, more time is being requested for LMETCALF.HARO_A
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In the guaranteed time of ISO the Blue Compact Dwarf Starburst Galaxy Haro 3 or
(Mkn 35) with a Wolf-Rayet (WR) feature was observed with ISOPHOT and ISOCAM.
The results of these observations will appear in the special ISO edition of A&A
and the results are summarised in the five figures attached to this proposal.
Based on these exciting results, and in an effort to investigate systematically
the properties of WR galaxies, we propose to observe a sample of eight galaxies
with ISOPHOT and with ISOCAM using the LW3, LW6, LW9 (and sometimes LW10)
filters and with PHT-S. The fact that WR galaxies are a roughly co-eval sample
makes comparison with other WR galaxies important and requires collection of a
sample of observations. The unique data obtained will be used to investigate
the causes of the massive bursts of star formation 3-6 million years ago. The
filters chosen provide maps of the galaxies in one, or in combinations of, the
Unidentified Infrared Bands (UIB --> "PAH") and dust or nebular line emission.
They enable a determination of the spatial relationship between the optical
star forming regions and the infrared emission from the young WR starburst
regions while allowing discrimination of the relative contribution to the far
infrared flux from dust, nebular emission and PAH molecules. The ratio of
filter intensities will yield valuable information on the effect on PAH density
of the intense radiation field. The PHT-S spectra allow a much more precise
discrimination of the contributions of many of the important spectral features,
complementing the spatially resolved CAM data.
The source list includes IRAS 15564+6359, which is a HII type galaxy with a
highly variable x-ray source recently observed by ROSAT. This is the first HII
type galaxy with an AGN type x-ray source. We propose observation of this
unique source to check for variability in the interval between the IRAS and ISO
observations.


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