swiftsimio: A Python library for reading SWIFT data

Borrow, Josh; Borrisov, Alexei

doi:10.21105/joss.02430

Cited by 40 publications

(15 citation statements)

References 5 publications

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“…The research in this paper made use of the SWIFT open-source simulation code (http://www.swiftsim.com, Schaller et al 2018) version 0.9.0. This work made use of the python libraries numpy (Harris et al 2020), matplotlib (Hunter 2007), and swiftsimio (Borrow & Borrisov 2020), and of NASA's Astrophysics Data System Bibliographic Services. 2015) on galaxy stellar mass in our model, at resolution.…”

Section: Discussionmentioning

confidence: 99%

The importance of black hole repositioning for galaxy formation simulations

Bahé,

Schaye,

Schaller

et al. 2021

Preprint

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Active galactic nucleus (AGN) feedback from accreting supermassive black holes (SMBHs) is an essential ingredient of galaxy formation simulations. The orbital evolution of SMBHs is affected by dynamical friction that cannot be predicted self-consistently by contemporary simulations of galaxy formation in representative volumes. Instead, such simulations typically use a simple "repositioning" of SMBHs, but the effects of this approach on SMBH and galaxy properties have not yet been investigated systematically. Based on a suite of smoothed particle hydrodynamics simulations with the code and a Bondi-Hoyle-Lyttleton subgrid gas accretion model, we investigate the impact of repositioning on SMBH growth and on other baryonic components through AGN feedback. Across at least a factor ∼1000 in mass resolution, SMBH repositioning (or an equivalent approach) is a necessary prerequisite for AGN feedback; without it, black hole growth is negligible. Limiting the effective repositioning speed to 10 km s −1 delays the onset of AGN feedback and severely limits its impact on stellar mass growth in the centre of massive galaxies. Repositioning has three direct physical consequences. It promotes SMBH mergers and thus accelerates their initial growth. In addition, it raises the peak density of the ambient gas and reduces the SMBH velocity relative to it, giving a combined boost to the accretion rate that can reach many orders of magnitude. Our results suggest that a more sophisticated and/or better calibrated treatment of SMBH repositioning is a critical step towards more predictive galaxy formation simulations.

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Section: Discussionmentioning

confidence: 99%

The importance of black hole repositioning for galaxy formation simulations

Bahé,

Schaye,

Schaller

et al. 2021

Preprint

Self Cite

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“…(http://www.swiftsim.com, Schaller et al 2018) version 0.9.0. All galaxy images in this work (Figures 2,7) were created using - (Benitez-Llambay 2015) and the data analysis was carried out with the help of (Borrow & Borrisov 2020), (Harris et al 2020), and (Hunter 2007).…”

Section: Data Availabilitymentioning

confidence: 99%

The importance of the way in which supernova energy is distributed around young stellar populations in simulations of galaxies

Chaikin,

Schaye,

Schaller

et al. 2022

Preprint

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Supernova (SN) feedback plays a crucial role in simulations of galaxy formation. Because blastwaves from individual SNe occur on scales that remain unresolved in modern cosmological simulations, SN feedback must be implemented as a subgrid model. Differences in the manner in which SN energy is coupled to the local interstellar medium and in which excessive radiative losses are prevented have resulted in a zoo of models used by different groups. However, the importance of the selection of resolution elements around young stellar particles for SN feedback has largely been overlooked. In this work, we examine various selection methods using the smoothed particle hydrodynamics code . We run a suite of isolated disk galaxy simulations of a Milky Way-mass galaxy and small cosmological volumes, all with the thermal stochastic SN feedback model used in the simulations. We complement the original mass-weighted neighbour selection with a novel algorithm guaranteeing that the SN energy distribution is as close to isotropic as possible. Additionally, we consider algorithms where the energy is injected into the closest, least dense, or most dense neighbour. We show that different neighbour-selection strategies cause significant variations in star formation rates, gas densities, wind mass loading factors, and morphology. The isotropic method results in more efficient feedback and better numerical convergence than the conventional mass-weighted selection. We conclude that the manner in which the feedback energy is distributed among the resolution elements surrounding a feedback event is as important as changing the amount of energy by factors of a few.

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“…We acknowledge various public python packages that have greatly benefited this work: scipy (van der Walt et al 2011), numpy (van der Walt et al 2011, matplotlib (Hunter 2007). This work has also benefited from the python analysis pipeline SwiftsimIO (Borrow & Borrisov 2020), and the Swift color map collection 3 .…”

Section: Data Availabilitymentioning

confidence: 99%

TangoSIDM: Tantalizing models of Self-Interacting Dark Matter

Correa,

Schaller,

Ploeckinger

et al. 2022

Preprint

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We introduce the TangoSIDM project, a suite of cosmological simulations of structure formation in a Λ-Self-Interacting Dark Matter (SIDM) universe. TangoSIDM explores the impact of large dark matter (DM) scattering cross sections over dwarf galaxy scales. Motivated by DM interactions that follow a Yukawa potential, the cross section per unit mass, 𝜎/𝑚 𝜒 , assumes a velocity dependent form that avoids violations of current constraints on large scales. We demonstrate that our implementation accurately models not only core formation in haloes, but also gravothermal core collapse. For central haloes in cosmological volumes, frequent DM particle collisions isotropise the particles orbit, making them largely spherical. We show that the velocity-dependent 𝜎/𝑚 𝜒 models produce a large diversity in the circular velocities of satellites haloes, with the spread in velocities increasing as the cross sections reach 20, 60 and 100 cm 2 /g in 10 9 M haloes. The large variation in the haloes internal structure is driven by DM particles interactions, causing in some haloes the formation of extended cores, whereas in others gravothermal core collapse. We conclude that the SIDM models from the Tango project offer a promising explanation for the diversity in the density and velocity profiles of observed dwarf galaxies.

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swiftsimio: A Python library for reading SWIFT data

Cited by 40 publications

References 5 publications

The importance of black hole repositioning for galaxy formation simulations

The importance of black hole repositioning for galaxy formation simulations

The importance of the way in which supernova energy is distributed around young stellar populations in simulations of galaxies

TangoSIDM: Tantalizing models of Self-Interacting Dark Matter

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