Welcome to the TangoSIDM project website! 


What is the Universe made of? The answer to this very simple question is not so simple. We appear to live in a universe composed of an unidentified form of matter called `dark matter’ (hereafter DM). Uncovering the nature of dark matter is one of the most pressing pursuits in modern physics and cosmology.
Astronomical observations are the key to understand the nature of DM and have been revealing the possibility that DM particles interact non-gravitationally with each other. It began with observations of the collision of nearby galaxy clusters. More recently, measurements of very large DM densities in lensed systems are indicating that DM-DM interactions can also induce gravothermal core collapse. This is an effect where frequent DM-DM interactions heat the central DM halo core, causing it to rapidly contract and raise in density.
While studies on galaxy clusters scales have set robust upper limits on the DM self-interaction cross section, σ/m, robust constraints of σ/m on dwarf galaxy scales are currently missing. The possibility of gravothermal core collapse indicates that σ/m could be larger than 10 cm2/g on dwarf galaxy scales, as recently estimated by Correa (2021). But more thorough studies with detailed modelling of self-interacting DM and galaxy formation in a cosmological context are needed to prove or rule out scenarios of large σ/m.
The goal of this project is to lead a theoretical program that will provide a much deeper understanding of what we can infer from observations of dwarf galaxies about the nature of dark matter.
We are currently making state-of-the-art cosmological hydro-dynamical simulations of a self-interacting DM universe, with the ambitious goal of producing detailed modelling of the nearby satellite galaxies that orbit around the Milky Way.

Cosmological Simulations of structure formation

Our simulation suite currently consists of:
- a set of dark matter only high-resolution boxes: of (25 Mpc)^3 cubic volume with 752^3 baryon particles and 752^3 DM particles, reaching a spatial resolution of 350 pc.
- a hydrodynamical suite of (25 Mpc)^3 cubic volume with 376^3 baryon particles and 376^3 DM particles, reaching a spatial resolution of 752 pc.

The simulations have been re-run starting from the same initial conditions, but assuming different self-interacting dark matter flavours. These include constant cross section of 0 (CDM case), 1 cm^2/g and 10 cm^2/g, as well as velocity dependent models (as shown in figure on the right).


Dark Matter Particle-Particle collisions in SWIFT

We have modelled the interaction between dark matter (DM) particles following a stochastic approach, where DM particles have a probability of interaction that depends on the cross section, σ/m, as well as on the distance and relative velocity between them. The search radius, which encloses a region where a DM particle has the probability of interacting with its neighbours, is not constant, instead it is adjusted according to the local density.

Meet the Team

Camila Correa (PI)
Veni Fellow at the University of Amsterdam

Matthieu Schaller
Lecturer at Leiden University, lead developer of the galaxy formation code SWIFT

Sylvia Ploeckinger
Postdoctoral fellow at Leiden University

Noemi Anau Montel
PhD Student at the University of Amsterdam

Weniger Christoph
A/Prof. at the University of Amsterdam

Shinichiro Ando
A/Prof. at the University of Amsterdam


This project is funded by NWO (Netherlands Organisation for Scientific Research). NWO Veni 192.020. The TangoSIDM simulation suite has been produced using the DECI resource Mahti (Finland/CSC), PRACE aisbl., project ID 17DECI0030-TangoSIDM, as well as the Dutch national e-infrastructure, Snellius, SURF Cooperative, project ID EINF-180-TangoSIDM.


Do you want to get involve?

Contact us! We are happy to share our simulations' data. We can discuss new projects anytime.