The Morphology of Dust Lanes in Barred Spirals

Details The Morphology of Dust Lanes in Barred Spirals The Morphology of Dust Lanes in Barred Spirals

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8374s&link_type=abstract

HST Proposal ID #8374

Physics

Hst Proposal Id #8374 Galaxy Structure And Dynamics

Scientific paper

We propose to use the HST archives to investigate gas inflow along bars in spiral galaxies, by studying in detail the structure of the dust lanes along these bars. In nearby galaxies, these dust lanes are typically about 1'' wide {50 pc at a distance of 10 Mpc} and so are unresolved or nearly unresolved on groundbased images. With the unprecedented resolution of HST, however, these features are well-resolved, providing the opportunity to study their structure in detail. These dust lanes trace the inflowing gas, which is difficult to detect directly along bars, and so provide information about clumping, shocks, and cloud formation in the inflowing gas. The HST archives contain a large number of WFPC2 images of nearby spiral galaxies. With these data, we will be able to determine if these lanes are continuous or clumpy and if they are separated into multiple streams. With the large sample of data available, we will be able to determine if the structure varies from galaxy to galaxy and if there are trends {i.e., are the lanes clumpier, weaker, and/or wider in weaker bars? In galaxies without strong circumnuclear star formation?}. These data will provide a valuable test of theoretical models of gas inflow along bars, addressing questions about the importance of self-gravity, viscosity, and shocks in driving gas inflow.

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