Task mfboot models a planet as a simple disk with constant brightness temperature. It has built-in ephemerides of the planets, and so knows their apparent size and orientation. It also has a model of the brightness temperature variation with frequency. Hence mfboot can generate a nominal visibility function of a planet. This model for Mars is not sophisticated, but should be accurate to better than 10% if appropriately used.
Task mfboot can also be used when bootstrapping from a point source. Although mfboot contains models for sources such as 1934-638, these models are not relevant for 3mm observers. If using a point source, generally the user would need to give mfboot the flux density of the source.
It is implicitly assumed in the bootstrapping approach described here that the flux density calibrator is observed near simultaneously and at the same elevation as the secondary calibrator. This is required because the antenna gain changes with both elevation and with thermal changes. The most reliable approach to tying the secondary and the flux density calibrators flux scales together is through observations with the same elevation and thermal environment.
Task mfboot will apply the bandpass and antenna gain solutions to the observed data before it does a comparison with the models. While it is not generally important that the flux density calibrator data is phase calibrated, it is important that it has the antenna amplitude calibration, derived from the secondary, is applied. This is critical in tying the flux density scales of secondary and flux density calibrator.
We will discuss the various input parameters for mfboot:
When using scalar mode with significantly resolved planets, where there is little flux on long spacings, you might consider using the clip parameter so as to exclude data that would simply contribute noise bias.
clip=0.4, which will ignore data where the visibility function model is less than 40% of the model zero spacing value.
In the general case, to use mfboot with the calibration scheme recommended above is straightforward enough: you simply run mfboot on the dataset, having selected the flux density calibrator. For example:
|vis=vela.fixed.uv||Input multi-source, dual-band dataset.|
|select=source(uranus)||Select flux density calibrator.|