mass profiles, HI masses

In the morning, Sheldon showed us that the weak lensing signal from massive clusters is consistent with the NFW profile, and that cluster richness is closely related to mass.

In the afternoon, Navarro showed us that CDM profiles really are (plausibly) shallower than r−1.5 at their centers, with a number of arguments. He also showed us that triaxiality of galaxy halos affects rotation curves significantly; plausibly enough to place currently discrepant measurements in agreement with models.

Katarina Kovac (Groningen) came by and showed us a very nice measurement of the HI mass function. She went from raw data (1400 pointings, each producing a 3 million pixel data cube) to mass function; nice work! She has much better sensitivity than HIPASS and finds a "flat faint end slope".

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