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Connection:
https://univ-grenoble-alpes-fr.zoom.us/j/98634272360?pwd=YkQ1ZVM5K2l4UUFPTkViYVNZRDFXZz09 Attendees: Fred, Sasha, Adam, Timea, HongLi, Mélanie, Fabrice, Nichol, Josh, Fabien, Nathalie, Leo, Yohan, Allison, Sylvain, Amy, Cara, Tapas, Mélisse Not attending: For memory: Minutes from our last telecon Activities of the Core Working Group Members and their main interests Agenda:
NH3, 3’’ → T(NH3) of the cores surrounding (+ ALMA 0.2’’ @ 1mm) Mean temperatures: 20K (SE or W51-E) 60K (W51-E) up to 120K (W51-IRS2) Effect of the dynamic assumptions for temperature on the CMF: slightly steeper Cores located on the extended free-free emission could correspond to chance alignment (no T measurements) or free-free peaks. To remember: apply for more NH3 measurements at the VLA deadline for C configuration (later than August).
getsf seems to provide better flux estimates for the weakest sources. → better for mass studies
Gemma: W51-E (more sensitive and larger area than the paper to be submitted by Josh+) Hongli G353.41 (CMF, fragmentation) Xing G327 Nichol+Jeff?: on the denoised images by MnGSeg
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Connection:
https://univ-grenoble-alpes-fr.zoom.us/j/98634272360?pwd=YkQ1ZVM5K2l4UUFPTkViYVNZRDFXZz09 Attendees: Fred, Fabien, Yohan, Sasha, Nathalie, Mélanie, Fabrice, Gemma, Adam, Leo, Sylvain, Amy, Allison, Patricio, Nichol, Timea Not attending: For memory: Minutes from our last telecon Activities of the Core Working Group Members and their main interests Agenda:
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
Gemma: W51-E Hongli G353.41 (CMF, fragmentation) Xing G327 Nichol+Jeff?: on the denoised images by MnGSeg
To be discussed in 2 weeks.
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