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8 ANGULAR RESOLUTION & u-v COVERAGE

Table 5 gives the maximum lengths ( [画像:$B^{\rm km}_{\rm max}$]) for each of the VLBA's 45 internal baselines as well as the baselines to HSA telescopes. A measure of the corresponding resolution ( $\theta _{\rm HPBW}$) in milliarcseconds (mas) is

where $\lambda^{\rm cm}$ is the receiver wavelength in cm (Wrobel 1995). A uniformly weighted image made from a long $u$-$v$ plane track will have a synthesized beam with a slightly narrower minor axis.

Values of $\theta _{\rm HPBW}$ for the longest VLBA baseline, at the center frequencies of the standard observing bands (Table 3), are shown in Table 6. The longest VLBA baseline at 3 mm is currently that between MK and NL, which is about 30% shorter than the longest baseline at lower frequencies.

Customized plots of the u-v plane coverage with the VLBA and/or other VLBI stations can be generated by NRAO program SCHED (Walker 2011).

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next up previous contents
Next: 9 BASELINE SENSITIVITY Up: VERY LONG BASELINE ARRAY Previous: 7.4 Output Rate Contents

Jon Romney 2012年01月05日