A pretty broad workshop covering key parts of ProTools. We go from directly measuring flux on multi-band data with ProFound to full SED fitting of the results with ProSpect.

An example of some basic analysis (similar to some of the Robotham and Bellstedt first ProGeny paper).

Here we generate all 44 SSPs used and discussed in the original ProGeny paper (Robotham & Bellstedt).

A summary of some of the useful Rfits methods.

Fitting PSFs (i.e. stars) with ProFit. Note there are now more automated routes to doing this available in ProFuse. In this vignette we fit a model Moffat profile fit to an empirical PSF. We then use this model PSF for our image convolution when fitting a galaxy, rather than the empirical estimate that comes packaged with ProFit.

A simple example of loading in FITS data and fitting some 2D profiles with ProFit. This vignette lets the user try a sophisticated decomposition of 10 example galaxies that have both SDSS and KiDS data. These examples were presented in the original ProFit MNRAS 2017 paper.

Useful hints on making good use of ProFound.

Older image stacking function in ProFound (now mostly prefer those in ProPane).

Working with lower level segmentation maps.

Combining ProFound source detection with creating low level inputs for ProFit (note ProFuse offers a much more automatic mechanism for combining the two).

Colour photometry with ProFound

Here we look at different modes of image tweaking and registration available in ProPane.

Various tests of stacking using the ProPane package. This include warping data to a common WCS, and investigating different schemes for stacking and combing the data to create the best quality output.

Here we look at using the Apache Arrow Dataset database system to operate on Medium Data (small enough to fit on your RAID, too big form RAM). We look at using CSV and Parquet backends.

Examples of 1/1.5/2/3 component fitting with ProFuse. This should be enough to get people going with different observations.

A simple example of how to generate and fit an SED. If you have observed data then it should be clear how to just execute the fitting part.

A simple Bulge-Disk fit using ProFuse. This is as presented in the associated paper.

Examples of how to run ProFit on multi images, be they offset images with the same filter, or multi band. The final example shows it working in a highly automated mode, extracting PSFs and fitting a smooth model across bands without sharp discontinuities.

Here we look at how to simultaneously fit multiple images of the same object. Each one can have a different PSF and segmentation map etc. This is a better route to multi-exposure fitting than just stacking.

Almost fully automated fitting. This is useful for beginners finding their feet, and particularly easy cases.

Example of complex multi-band stacking including dynamic masking.

Example of calculating a filter transform using ProSpect. In this case we use Sloan r and i to predict VST r.

Here we use ProSpect to generate the EBL with a model for the SFH and ZH.

A short journey into the use and impact of priors on LML and Bayes Factors.

Comparison of BC03 and EMILES SSPs

Some sanity checks of the BC03 library.

A short guide and basic introduction for beginners to ProSpect. This is likely to evolve with time.

PSF musings by Dan Taranu

A complex example combining the outputs of ProFound with the inputs of ProFit.

Main overview of the ProFound source finding package.

Examples and tests of the ProFound sky estimation routines.

A demo of using extracted isophotal ellipses to fit a basic 1D profile, and using these fit parameters to make reasonable estimates for a full 2D ProFit solution.

This is a demo of using ProFit in a fully automatic mode for processing VST data in the SAMI clusters.

Basic overview of the package that accompanies the GitHub version of the code. This covers basic installation issues that you might have.

This vignette concentrates on the model image generation capabilities of ProFit, ending with examples of producing images with dozens of galaxies distributed around a large frame.

Some info on speeding things up by making use of OpenCL and OpenMP support.

A detailed vignette on what we mean by, and how to construct, sigma maps.