We deconvolved the cold and
warm dust emission components spatially by making the best use of the multi-band photometric capability of the FIS.
Not exact matches
ALMA can map radio
emissions from the
warm dust and gravel in disks.
This might indicate that smaller (and
warmer)
dust grains are responsible for the 100 μm
emission than at the longer wavelengths, in agreement with the theoretical predictions of van Marle et al. (2011).
«However, there is an additional difficulty when searching for
warm dust in the immediate stellar environment: it generally contributes very little
emission compared to the star, and that is when nulling interferometry comes into play.»
If located within a few AUs of the central star, this
dust is
warmed to temperatures that produce near - infrared
emission and small grains produce scattered light.
The
warmer dust component is spatially correlated well with the [O III]
emission and hence likely to be associated with the highly - ionized gas locally heated by intense radiation from the two clusters.