After being asked by many people to use some of my codes for their projects, I realized how making source codes public may benefit the community and astronomy as a whole (and I myself used a lot of open-source codes too). Here I list some of the codes developed by myself and collaborators.
I mainly work with pen and paper (and python) and thus not a professional coder, so there may be (badly-written) parts that are difficult to understand. If you have questions, feel free to ask me. When using one of these codes, it would be great if you can cite the relevant papers.
Codes
A code to calculate (in a few minutes) the profile of a shocked region created from ejecta-CSM interaction (self-similar solution from Chevalier82 ApJ, 258, 790, and used for the paper Tsuna+19, ApJ, 884, 87).
CHIPS: library for simulating circumstellar matter and light curves for interaction-powered transients (see this paper). The code is actively developed and maintained by (former) members of the Shigeyama group at RESCEU, University of Tokyo.
A code to calculate the distribution of Galactic compact objects (BHs, NSs) with/without natal kick, by orbit calculation following the Galactic potential (used in Tsuna+18, MNRAS, 477, 791, and several other works later on). The dataset itself is available from this Zenodo link.
A code to model light curves of (bright) precursors from massive stars with compact object companions (based on Tsuna+2024, ApJ 966, 30)
A code to model long-rising (months-years) "merger precursors", powered by unstable mass transfer of a low-mass helium star to a NS companion (based on Tsuna+2024, Open Journal of Astrophysics 7, 82)
A code to model light curves of extremely luminous transients powered by collision of a newborn NS/BH and a main-sequence binary companion (based on Tsuna & Lu, 2025; ApJ Accepted)
Data
SN precursor light curve models calculated by CHIPS (by eruptions of red supergiants; Tsuna, Takei, Shigeyama 2023, ApJ, 945, 104; Important caveat: dust extinction by the progenitor mass-loss (e.g. in SN 2023ixf) is not considered in these models.)
Failed SN light curve models calculated by SNEC (red supergiants; Tsuna, Huang, Fuller, Piro 2024)
In prep (if you are interested please contact me):
A code for analytical (UVOIR) light curve model of interaction-powered supernovae with time-dependent radiative efficiency (Tsuna+19, ApJ, 884, 87).
A code for modelling multi-wavelength emission of wind outflow following BH formation (Tsuna+21, ApJL, 914, 64)