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A. A. Goodman (Harvard-Smithsonian Center for Astrophysics), J. F. Alves (ESO-Garching), H. G. Arce (AMNH), T. Bethell (U. Wisconsin), M. A. Borkin (CfA), P. Caselli (Arcetri Obs.), J. Di Francesco (HIA), J. B. Foster (CfA), M. Halle (Brigham and Women's Hospital, Harvard U.), M. Heyer (U. Massachusetts), D. Johnstone (HIA), H. Kirk (U. Victoria), D. A. Kosslyn (CfA), D. Li (JPL), J. Li (CfA), M. Lombardi (ESO-Garching), J. Pineda, N. A. Ridge, S. L. Schnee (CfA), M. Tafalla (OAN, Spain), N. Whitehorn (U. Chicago/CfA)
The COMPLETE (COordinated Molecular Probe Line Extinction Thermal Emission) Survey of Star-Forming Regions has now mapped the full extent (as defined by the Spitzer c2d Legacy Survey) of the Perseus, Ophiuchus, and Serpens star-forming regions in: 1) 12CO and 13CO maps (featuring >200,000 spectra) from FCRAO with 40 arcsec resolution; 2) extinction, using the ``NICER" method on 2MASS data; and 3) thermal emission using a combination of IRAS (60 and 100 micron) and SCUBA (850 micron) data. The molecular line maps give kinematic information, while the combination of the extinction and thermal emission maps give the most accurate view of the clouds' dust column density and temperature distributions to date. The COMPLETEd ``wide-field" maps represent ``Phase 1" of the Survey, and ``Phase 2," which offers close-up views of nearly all of the embedded ``cores" within the COMPLETE fields is well underway. Our key results to date include: 1) a new methodology for calibrating dust emission maps with extinction maps (Schnee et al. 2005); 2) a new appreciation of the fundamental uncertainty in the line-of-sight variations in dust temperature introduced into column-density measurements using dust emission (Schnee et al. 2006) 3) evidence for important interactions of spherical winds from B-type stars with molecular clouds (see Ridge et al. 2006a); 4) an extinction ``threshold" for star formation in Ophiuchus (Johnstone et al. 2004); 5) demonstration that extinction mapping routinely yields log-normal density distributions, which disagree with molecular-line map based density distributions, because the line data is biased by excitation and optical depth effects (Goodman et al. 2006); 6) the discovery of ubiquitous ``cloudshine" coming from dark clouds (Foster & Goodman 2005); 7) measurement and identification of uncertainties in the clump mass function for Perseus (Pineda et al. 2006); and 8) testing and new use of 3D medical-imaging software for identification and analysis of spatial features (e.g. clumps, outflows) within molecular line maps (Borkin et al. 2005; Goodman et al. 2006). All of these data and results are online and available for public use through the COMPLETE web site at http://cfa-www.harvard.edu/COMPLETE, and the Phase 1 data are summarized in Ridge et al. 2006b.
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The author(s) of this abstract have provided an email address for comments about the abstract: agoodman@cfa.harvard.edu
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.