Computer Science
Scientific paper
Jul 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003hst..prop.9824w&link_type=abstract
HST Proposal ID #9824
Computer Science
Hst Proposal Id #9824 Galaxies
Scientific paper
We propose a NIC3 H-band {F160W} SNAPshot survey of 48 nearby mid- to late-type galaxies covering all inclinations. In Cycle 9 and 10, we imaged 100 galaxies in the mid-UV {F300W/F255W} and I-band {F814W} with WFPC2, and obtained UBVR CCD surface photometry from the ground. Early-mid-type galaxies show the usual small radial color-gradients, where disks become somewhat bluer at larger radii. But, remarkably, the majority of {lower luminosity, smaller and rounder} late-type galaxies shows the opposite trend and becomes redder outwards in all filters. While young UV/blue-bright stellar populations dominate their inner morphology, most late-type galaxies must have a significant halo or thick disk of older stars. Combining our proposed NIC3 H-band with existing WFPC2 images will span the wavelength range 0.29-1.6 micron at resolutions of 0.04-0.16" {FWHM}. This Panchromatic Nearby Galaxy Atlas will be applicable to a wide range of problems, and will be made public immediately. Our NIC3/F160W science goals are to: {1} Establish the nature of the old outer stellar population. All target galaxies have z<0.005, allowing us to resolve any luminous, cool supergiant population. NIC3 is essential to make a pixel-to-pixel color-magnitude study of the nature, distribution and uniformity of the outer stellar populations, which will constrain dwarf galaxy formation theories. {2} Determine galaxy structure at 5-20 pc resolution, tracing the old stellar population and mass distribution compared to the star-forming regions seen in the mid-UV. A range of inclinations is needed to distinguish between old thick disks or halos in late-type galaxies. {3} Make a multi-wavelength pixel-to-pixel decomposition to help delineate the effects of dust, age, and metallicity. Since we must cover a range of inclinations, NIC3 H-band is essential to map the effects from dust, and see how these may affect the studies of {1} and {2}.
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