The level one science goals of this WG are the imaging Proto-planetary
disks and Normal Stars.  The special requirements are high frequency
operation - at least 22 GHz, and a sensitivity of 10K in a beam of a
few mas at the highest frequencies.

As was noted in Groningen, the biggest drawback in many of the
concepts is a low upper frequency limit. Certainly it is possible to
recover the resolution if the upper frequency limit is reduced by
increasing baselines. However, this adversely affects the science: 1)
at frequencies below 20 GHz it is not clear if emission from dust or
photo-evaporation dominates from proto-planetary systems, and 2) the
ability to image water masers is a key aspect of studying stellar
photospheres. So we maintain a firm requirement for at least an upper
limit that includes water maser emission - namely 22 GHz. 33 GHz would
be fantastic for thermal science, since the SNR improves dramatically
with high frequencies for thermal spectra.

USA:       No problems - the high frequency capability is fantastic.
Hopefully A/T will be pushed at the highest frequencies such that
remains relatively constant across the frequency range. 

           Compliance 5

Canada:    No problems apparent - upper frequency limit is fine, and
           could be pushed higher. No discussion of configurations is
           given in the White Paper, but baselines of around a 
           few 1000 km with
           sufficient brightness temperature sensitivity are not
           precluded by the large diameter reflectors.

           Compliance 5

India:     Low upper frequency limit. Less than 10 GHz precludes the bulk
           of our Level 1 science. If upper frequency capability is
           increased to 20 GHz (is that possible? The white paper
           mentions the wide frequency range of the reflectors - but
           the quoted efficiency at 10 GHz is already poor), then the
           configuration is the limiting factor - the white paper
           doesn't discuss configurations.

           Compliance 1

Ozlens:    Low upper frequency limit. Not clear if the Luneberg lens
           concept can attain attain a sufficiently broad frequency range that
           would include 20 GHz or higher.

           Compliance 1

Ozcyl:     Low upper frequency limit. 

           Compliance 1


Europe:    Low upper frequency limit. 

           Compliance 1

China:     Low upper frequency limit. Even if this could be increased,the 
           maximum baseline is too short to attain a few mas.
           
           Compliance: 1



SR amended for consistency with other working groups:
Ozcyl/India to 2 (could get hi frequency)