Attendees: Fred, Fabien, Yohan, Sasha, Nathalie, Mélanie, Fabrice, Gemma, Adam, Leo, Sylvain, Amy, Allison, Patricio, Nichol, Timea
Minutes from our last telecon
Activities of the Core Working Group
Members and their main interests
Automatic removal of (0% in young, 10% in intermediate, ¼ in evolved regions) cores potentially contaminated by free-free emission using 3mm/1mm ratio maps and the recombination line images of Roberto
⇒ Evolutionary stage of regions to be refined (see Fig. 20 of Adam’s paper): G353 and G08 → Intermediate, G12 → Evolved, G337 → Young
⇒ The CMF becomes slightly steeper for evolved regions when removing cores lying in the free-free (H41alpha footprint for now) areas.
Young: G327, G328, G337, G338, W43-MM1, W43-MM2 (no Halpha)
Intermediate: W43-MM3, G351, G353, G008, W51-E (most cores on thermal dust emission)
Evolved: W51-IRS2, G010, G012, G333
The major uncertainty is now coming from the dust temperature, here assumed to be constant over the whole core sample.
→ Test to be done on W51 using NH3 temperature (Adam + Fabien)
Optical thickness to be investigated, using e.g. the approximated formula of our Nature Astronomy paper.
weak 3mm sources (TBD by Fabien)
Few sources (2-3) could be free-free in MM3
Hongli G353.41 (CMF, fragmentation)
Nichol+Jeff?: on the denoised images by MnGSeg
To be discussed in 2 weeks.