Stellar Populations in the Disk-Halo Interface of NGC 55

Details Stellar Populations in the Disk-Halo Interface of NGC 55 Stellar Populations in the Disk-Halo Interface of NGC 55

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8697f&link_type=abstract

HST Proposal ID #8697

Physics

Hst Proposal Id #8697 Stellar Populations

Scientific paper

The disk-halo interface is where the global effects of stellar feedback on the ISM are expected to be most pronounced. Our deep ground-based emission-line images of the nearby, edge- on SBm galaxy NGC 55 provide a particularly spectacular example of this phenomenon. In addition to numerous supergiant ionized filaments and shells, our images also reveal the surprising discovery of several candidate HII regions located at significant heights {1-2 kpc} above the disk plane. We have obtained high-resolution ground-based broad-band images for the brightest of these candidate HII regions, revealing several underlying blue continuum sources, supporting the idea that such regions might be the site of in situ star formation in the disk-halo interface. If recent star formation has occurred in these clumps, it would have extremely important implications for understanding the disk-halo connection in galaxies. Further, if this is not an isolated event, there should be a faint background thick disk/halo. We propose to obtain WFPC2 UVI images of these candidate HII regions to resolve the embedded stars that appear to be present, together with parallel STIS observations to investigate a possible background thick-disk/halo stellar population, about which there is little information in very late-type disk systems, and which will place our targetted WFPC2 HII region data in context.

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