Attendees: Fred, Yohan, Jeff, Amy, Nathalie, Sasha, Gemma, Allison, Roberto, Patricio, Nichol, Adam, Thomas, Leo, Alex, HongLi, Fabrice, Sylvain, Timea, Tapas, Quang, Ant
Not attending: Fabien
Minutes from our last telecon
Members and their main interests
Measurements: original images, PB-corrected
→ Final extraction to be done with getsf and GExt2D.
Question to Sasha: is it possible to spare time and not measure cores’ parameters on the W43-MM2MM3_1mm_cohe_sm_sk06.fits and W43-MM2MM3_3mm_cohe_sm_sk06.fits maps? Answer: Sure!
Here is the GitHub link : https://github.com/Yohan-Pouteau/FlufiCarp
Please only circulate this link between consortium members
Questions to Alex:
→ why is the PPMAP coverage smaller than the 1mm ALMA coverage? Some cores fall outside the Tdust map…
Answer: image cropped to avoid edge effect, filtering will solve this issue.
→ why such squared regions?
Answer: edge effects as well, not present anymore in the new image
→ A couple of cores lie over the cold (10K) artefact created when fitting a modified blackbody toward pixels whose the 3mm emission is largely contaminated by free-free emission. Is there a method to ignore the 3mm image when fitting the SED of these pixels?
Answer: Alex could substitute a model wo 3mm to the black rounded artefact on the image
Adam: To mitigate/remove the free-free emission, we could in the future use the H41alpha image or VLA emission.
Question to Fabrice/Nathalie:
→ Do you confirm the “hot core” nature of the red sources?
Jeff’s presentation from last week.
* Max recov. scale = ~0.6 x \lambda/Lmin See equation nº6.1 (p53) in https://www.iram.fr/IRAMFR/ARC/documents/cycle1/alma-technical-handbook.pdf
optical thickness to be treated (70 micron, 1mm?)
[This information cannot be used for the 1st mass estimates we’ll make but we can expect publishing more corrected core temperature and thus mass measurements in the future.]