Cosmological simulations serve as invaluable tools for understanding the Universe. However, the technical complexity and substantial computational resources required to generate such simulations often limit their accessibility within the broader research community. Notable exceptions exist, but most are not suited for simultaneously studying the physics of galaxy formation and cosmic reionization during the first billion years of cosmic history. This is especially relevant now that a fleet of advanced observatories (e.g. James Webb Space Telescope, Nancy Grace Roman Space Telescope, SPHEREx, ELT, SKA) will soon provide an holistic picture of this defining epoch. To bridge this gap, we publicly release all simulation outputs and post-processing products generated within the thesan simulation project at www.thesan-project.com. This project focuses on the z ≥ 5.5 Universe, combining a radiation-hydrodynamics solver (arepo-rt), a well-tested galaxy formation model (IllustrisTNG) and cosmic dust physics to provide a comprehensive view of the Epoch of Reionization. The thesan suite includes 16 distinct simulations, each varying in volume, resolution, and underlying physical models. This paper outlines the unique features of these new simulations, the production and detailed format of the wide range of derived data products, and the process for data retrieval. Finally, as a case study, we compare our simulation data with a number of recent observations from the James Webb Space Telescope, affirming the accuracy and applicability of thesan. The examples also serve as prototypes for how to utilise the released dataset to perform comparisons between predictions and observations.

The interacting dark energy (IDE) model is a promising alternative cosmological model which has the potential to solve the fine-tuning and coincidence problems by considering the interaction between dark matter and dark energy. Previous studies have shown that the energy exchange between the dark sector components in this model can significantly affect the dark matter halo properties. In this study, by utilizing a large set of cosmological N-body simulations, we analyze the redshift evolution of the halo concentration–mass (c–M) relation in the IDE model, and show that the c–M relation is a sensitive proxy of the interaction strength parameter ξ₂, especially at lower redshifts. Furthermore, we construct parameterized formulae to quantify the dependence of the c–M relation on ξ₂ at redshifts ranging from z = 0 to z = 0.6. Our parameterized formulae provide a useful theoretical tool in constraining ξ₂ with the observational c–M relation. As a first attempt, we use the data from X-ray, gravitational lensing, and galaxy rotational curve observations and obtain a tight constraint on ξ₂, i.e. ξ₂ = 0.071 ± 0.034. Our work demonstrates that the halo c–M relation, which reflects the halo assembly history, is a powerful probe to constrain the IDE model.

Owing to design and operation limitations, most multi-zone variable air volume (VAV) systems in existing buildings still follow traditional techniques for ventilation. In recent ventilation research, most studies focused on comparing a traditional strategy with a superior one, and the comparison studies among traditional strategies are relatively rare. In this paper, four traditional outdoor airflow control strategies that are commonly used in existing VAV systems are introduced and discussed. The results illustrate that the phenomenon of uneven distribution for outdoor airflow among conditioned spaces often occurs, irrespective of the strategies with which the system operates. Compared to constant outdoor airflow fraction strategies, variable outdoor airflow fraction strategies can meet system outdoor airflow requirements while the occupancy number varies. On this basis, performance with respect to IAQ and energy-savings of variable outdoor airflow fraction strategies is compared. The results indicate that the two strategies have the same control effect on the IAQ. Furthermore, the multiple spaces equation-based strategy (MSE-V) shows energy reductions of 6.76% and 9.88% in the heating and cooling seasons, respectively, compared to the maximum outdoor airflow fraction-based strategy (MaxY-V) when the system operates under the same operation conditions.

In fuzzy dark matter scenarios, the quantum wave nature of ultralight axion-like particles generates stochastic density fluctuations inside dark matter haloes. These fluctuations, known as granules, perturb the orbits of subhaloes and other orbiting bodies. While previous studies have simulated these effects using N-body techniques or modelled them statistically using diffusion approximations, we propose an alternative framework based on representing the perturbations as a Fourier series with random coefficients, which can be applied to individual orbits, not just populations. We extend the model to finite-size subhaloes, identifying a critical length scale below which subhaloes behave as point-mass particles. In contrast, larger subhaloes exhibit suppressed perturbations from granules due to their extended mass profiles. Using FDM-Simulator, we validate our finite-size model by isolating granule accelerations and confirming their statistical effects on subhalo dynamics.