Many branches of astronomy interpret observations through approximate, one-dimensional models of stars. Furthermore, many stars are observed to undergo resonant pulsations, and the frequencies at which they do so are similarly interpreted through the predicted pulsations of the one-dimensional models. The study of these resonant pulsations in stars is known as asteroseismology. Since the equations of stellar structure, evolution and pulsation were defined in their modern forms around the mid-20th century, many programs have been written to produce models and predict their pulsations frequencies and correspondingly many custom data formats have been defined, with varying levels of ease-of-use and interoperability. tomso's main purpose is to provide a compact interface for parsing data in these formats and simplify research that uses them.

PIPPIN (PDI pipeline for NACO data) is a pipeline developed to reduce the polarimetric observations made with the VLT/NACO instrument. It applies the Polarimetric Differential Imaging (PDI) technique to distinguish the polarised, scattered light from the (largely) un-polarised, stellar light. As a result, circumstellar dust can be uncovered. During its operation, NACO employed different instrument configurations (e.g. half-wave plate or de-rotator usage, Wollaston beam-splitter or wiregrid observations) which are appropriately handled by PIPPIN. As part of the PDI reduction, PIPPIN performs various levels of corrections for instrumental polarisation and crosstalk.

INSPECTA (formerly sdhdfProc) is a software package to read, manipulate and process radio astronomy data in Spectral-Domain Hierarchical Data Format (SDHDF). It is available as part of the 'sdhdf_tools' repository.

Working with a GUI, or adding interaction in plotting, will help a lot in data analysis. However, the common GUI of Python is OS-dependent, while manually adding interactive codes is too complex. A pseudo-GUI tool is introduced in this work. It will help to add buttons/checkers in the graph and assign callback functions to them. The remaining problem is that the documents in this package are in Chinese and will be in English in the next version. This program is published to the PyPI, and can be installed by 'pip install pltgui'.

Matching stars in astronomical images is an essential step in data reduction. This work includes some matching programs implemented by Python: simple matching, fast matching, and triangle matching. For two catalogs with m and n objects, the simple method has a time and space complexity of O(m*n) but is fast for fewer n or m. The time complexity of the fast method is O(mlogm+nlogn). The triangle method will work between rotated and scaled images. All methods are applied in pipelines and work well. This package is published to the PyPI with the name 'qmatch'.

JWST PSF photometry in complex and crowded fields. StarbugII is an open-source python photometry suite that provides accurate photometry on point-like sources embedded in complex diffuse emissions. The tool has a simple modular interface with a wide range of photometric routines including embedded source detection, aperture and PSF photometry, diffuse background emission estimation, catalogue matching and artificial star testing. The core is built around Photutils (ascl:1609.011). Contributions and collaborations welcomed.

Calibration solutions for the LOFAR radio telescope are stored in a 5-dimensional (time, frequency, station, polarisation and direction in the sky) HDF5 table. H5plot is a GUI application focussing on interactive visual inspection of these calibration solutions.

The R code compares two periodogram algorithms for detecting transiting exoplanets: the Box-fitting Least Squares (BLS) and the Transit Comb Filter (TCF). It calculates the False Alarm Probability (FAP) based on extreme value theory and signal-to-noise ratio (SNR) metrics to quantify periodogram peak significance. The comparison approach is aimed at optimizing the detection of small transiting planets in future transiting exoplanet surveys. The code can be extended for comparing any set of periodograms.

Plages Identification identifies solar plages from Ca II K photographic observations irrespective of noise level, brightness, and other image properties. The code provides an efficient, reliable method for identifying solar plages. The output of the algorithm is an image highlighting the plages and the calculated plage index. Plages Identification is also deployed as a webapp, allowing users to experiment with different hyperparameters and visualize their impact on the output image in real time.

The injection-recovery MATRIX (Multi-phAse Transits Recovery from Injected eXoplanets) Toolkit creates grids of scenarios with a set of periods, radii, and epochs of synthetic transiting exoplanet signals in a provided light curve. Typical injection-recovery executions consist of 2-dimensional scenarios, where only one epoch (random or hardcoded) was used for each period and radius, which may reduce accuracy. MATRIX performs multi-phase analyses needing only a few parameters in a configuration file and running one line of code.