Attendees: Fred, Fabien, Antoine, Sasha, Adam, Nathalie, Amy, Tapas, Sylvain, Leo, Yohan, Thomas, Jeff, Pierre, Mélisse, Mélanie, Allison, HongLi, Fabrice
Minutes from our last telecon
Activities of the Core Working Group
Members and their main interests
Noise: white noise before simobserve + weather noise in simobserve
Integration time, distance, configuration were supposed to be representing ALMA-IMF images.
→ Dendrogram tests must still be correctly done
→ Comparison of getsf versus Gext2D: good correspondence except for lower-intensity sources
There is no more evolution of the CMF slope → index = 0.73-0.77 whatever the evolutionary stage of the region, flatter than the slope measure on the IRDC CMF by Patricio.
We now need to take into account free-free sources → removing cores using potential free-free emission (To Be improved), the index all regions gets steeper, and the evolved region close to = 1.4, the Salpeter index.
Inputs: Data and beam fits for each wavelength + beta and Tdust grids + color correction + “a priori dilution” (1 to 10, effect on Tmap)
Adding 70 micron and even worse 24 micron does not help modelize the SED of the big-grain submm component. Opacity at 70 micron was taken into account (empirical correction) by Ken for the Tdust image of W43-MM1.
None of these models include free-free emission...