Carma CO(1-0) Observations Of Four Nearby Spirals: Implications For The Origin Of Feathers

Details Carma CO(1-0) Observations Of Four Nearby Spirals: Implications For The Origin Of Feathers Carma CO(1-0) Observations Of Four Nearby Spirals: Implications For The Origin Of Feathers

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21333501l&link_type=abstract

American Astronomical Society, AAS Meeting #213, #335.01; Bulletin of the American Astronomical Society, Vol. 41, p.396

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CARMA CO(1-0) Observations of Four Nearby Spirals: Implications for the Origin of Feathers
Feathers are prominent extinction features first termed by Lynds (1970), which emerge from a spiral arm dust lane and arch into the interarm. Previously, La Vigne et al. 2006 showed that feathers are common in a range of galaxy types, that in M51 feathers emerge from giant molecular associations (GMAs) with their spacing related to the local, molecular surface density, and that feathers can be associated with much of the star formation in a galaxy. To evaluate whether the conclusions based on M51 can be more generally applied, we observed CO(1-0) emission in four spiral galaxies: NGC 0628, NGC 3627, NGC 4637, and NGC 5055, at 2-3" resolution using the CARMA millimeter wave array. From these new high resolution maps, we find that the conclusions from M51 can be applied to our sample of galaxies, which vary from early to late type and in morphological type. As in M51, we find the feathers emerge from GMAs or massive giant molecular clouds (GMCs) in the spiral arm dust lane. Also similar to M51, the spacing of the feathers is related to the gas surface density; as the surface density decreases the spacing of the feathers increases. We will discuss the implications of these results for the theories of origin for feathers and present a multi-wavelength analysis of star formation tracers of feathers.
CARMA operations are supported by the NSF under a cooperative agreement, and by the partner universities.

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