We can use the principal moments of inertia of a shape to classify astronomically ineresting structures in 2D (J plots) and 3D (J3D).
This code is able to separate centrally concentrated structures (cores), elongated structures (filaments) and hollow circular structures (bubbles) from the main population of ‘slightly irregular blobs’ that make up most astronomical images.
This can be applied to any 2D greyscale pixelated image (single wavelength/tracer or column density).
Examples of the usage of J plots are given in the tests folder.
A full description of this algorithm, the proof of concept tests, and example astronomical applications are described in the paper. A PDF is included in the docs folder or can be found on arXiv at https://arxiv.org/abs/1803.01640
This code is able to separate centrally concentrated structures, elongated structures (filaments), hollow structures, and prolate/oblate spheroids.
This can be applied to any 3D greyscale data cube (single wavelength/tracer or column density in PPP or PPV).
It should be pretty simple to run this code and get the plots out, but if you want to do anything more complicated please contact the authors on s.jaffa@herts.ac.uk.
A full description of this algorithm, the proof of concept tests, and some example astronomical applications are described in the paper which is currently in preparation.
This code is written in Python 3 (so should also run in Python 2). It requires the following libraries:
The scripts included in the 'tests' folder give basic examples of how to use J plots and J3D on common types of astronomical data. The input and output files are included so you can test the code yourself, or modify these examples to analyse your own data.
If you wish to use the code as it is to analyse your own work, please cite the relevant papers in your publication. If you wish to edit the code, expand it with new features, point out bugs or suggest improvements please contact the authors either by email or through the GitHub issue tracking page. This code is shared under the GNU GPLv3 license. For further detail please see the LICENSE file.
If you use this code in your work, please cite the original J plots paper and/or cite the code directly via the Astrophysical Source Code Library. If you need help running the code or interpreting your results, we would be happy to collaborate!