How does a MOND cosmology fare on Gpc scales? - Collisionless $N$-body simulations of $ν$HDM
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| Format: | Preprint |
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2026
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| author | Russell, Alfie Banik, Indranil Cray, Oscar Zhao, Hongsheng |
| author_facet | Russell, Alfie Banik, Indranil Cray, Oscar Zhao, Hongsheng |
| contents | We present the largest collisionless $N$-body cosmological simulations in a MOdified Newtonian Dynamics (MOND) cosmology to date. Our 4 simulations cover $Λ$CDM as a baseline, a MOND with hot dark matter model known as $ν$HDM, and 2 unphysical models we call $Λ$HDM and $ν$CDM to test the individual contributions of hot dark matter and MOND gravity, respectively. $ν$HDM reproduces the CMB power spectrum whilst also theoretically matching cluster dynamics and preserving MOND predictions for galactic rotation curves. We test its viability on cosmological scales using simulations with $256^{3}$ particles in a box of size $800/h$ comoving Mpc. We find generically that the MOND models massively overproduce large-scale structures by $z=0$, with a most massive cluster in $ν$HDM of $\approx 5 \times 10^{17} M_{\odot}/h$ and typical peculiar velocities of several thousand km/s. We also explore a local void solution to the Hubble tension in these models. Analogues to the observed "Local Hole'' do form in the MOND models, but values for the deceleration parameter $<-1.5$ in these regions prevent a satisfactory resolution to the Hubble tension. Whilst $Λ$CDM significantly underpredicts the observed bulk flow in Cosmicflows-4, the high peculiar velocities that arise in the MOND models create the opposite problem, ruling out $ν$HDM at $>5σ$ confidence. Observations clearly require a much milder enhancement to the rate of structure growth in $Λ$CDM than is provided by the $ν$HDM paradigm. Our results also suggest that replacing cold dark matter with hot dark matter is unlikely to provide a viable cosmological model, regardless of the gravity law. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2602_21975 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | How does a MOND cosmology fare on Gpc scales? - Collisionless $N$-body simulations of $ν$HDM Russell, Alfie Banik, Indranil Cray, Oscar Zhao, Hongsheng Cosmology and Nongalactic Astrophysics We present the largest collisionless $N$-body cosmological simulations in a MOdified Newtonian Dynamics (MOND) cosmology to date. Our 4 simulations cover $Λ$CDM as a baseline, a MOND with hot dark matter model known as $ν$HDM, and 2 unphysical models we call $Λ$HDM and $ν$CDM to test the individual contributions of hot dark matter and MOND gravity, respectively. $ν$HDM reproduces the CMB power spectrum whilst also theoretically matching cluster dynamics and preserving MOND predictions for galactic rotation curves. We test its viability on cosmological scales using simulations with $256^{3}$ particles in a box of size $800/h$ comoving Mpc. We find generically that the MOND models massively overproduce large-scale structures by $z=0$, with a most massive cluster in $ν$HDM of $\approx 5 \times 10^{17} M_{\odot}/h$ and typical peculiar velocities of several thousand km/s. We also explore a local void solution to the Hubble tension in these models. Analogues to the observed "Local Hole'' do form in the MOND models, but values for the deceleration parameter $<-1.5$ in these regions prevent a satisfactory resolution to the Hubble tension. Whilst $Λ$CDM significantly underpredicts the observed bulk flow in Cosmicflows-4, the high peculiar velocities that arise in the MOND models create the opposite problem, ruling out $ν$HDM at $>5σ$ confidence. Observations clearly require a much milder enhancement to the rate of structure growth in $Λ$CDM than is provided by the $ν$HDM paradigm. Our results also suggest that replacing cold dark matter with hot dark matter is unlikely to provide a viable cosmological model, regardless of the gravity law. |
| title | How does a MOND cosmology fare on Gpc scales? - Collisionless $N$-body simulations of $ν$HDM |
| topic | Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2602.21975 |