PBL is useful in the context of combining weak +strong lensing to reconstruct masses of galaxy clusters. In order to measure the weak lensing signal it is necessary to average over several tens of arc-seconds. On the other hand the separation multiple images incase of strong lensing can be a few arc-seconds. This means that the strong lensing information can give us information about the mass distribution on the scale of a few arc-seconds. PBL solves the problem of combining these two scales without making any prior assumptions about the mass distribution.

PBL codes

If you want to implement PBL to your lensing data here are the current codes in C++ that we use to do the weak lensing mass reconstruction. codes Strong lensing will be included very soon into this package.