The DOI matches its Crossref record; 199 of the 199 references it cites were found in a registry or an index.
The E-MOSAICS project: simulating the formation and co-evolution of galaxies and their star cluster populations
Open accessAbstract
We introduce the MOdelling Star cluster population Assembly In Cosmological Simulations within EAGLE (E-MOSAICS) project. E-MOSAICS incorporates models describing the formation, evolution, and disruption of star clusters into the EAGLE galaxy formation simulations, enabling the examination of the co-evolution of star clusters and their host galaxies in a fully cosmological context. A fraction of the star formation rate of dense gas is assumed to yield a cluster population; this fraction and the population's initial properties are governed by the physical properties of the natal gas. The subsequent evolution and disruption of the entire cluster population are followed accounting for two-body relaxation, stellar evolution, and gravitational shocks induced by the local tidal field. This introductory paper presents a detailed description of the model and initial results from a suite of 10 simulations of ∼L⋆ galaxies with disc-like morphologies at z = 0. The simulations broadly reproduce key observed characteristics of young star clusters and globular clusters (GCs), without invoking separate formation mechanisms for each population. The simulated GCs are the surviving population of massive clusters formed at early epochs (z ≳ 1–2), when the characteristic pressures and surface densities of star-forming gas were significantly higher than observed in local galaxies. We examine the influence of the star formation and assembly histories of galaxies on their cluster populations, finding that (at similar present-day mass) earlier-forming galaxies foster a more massive and disruption-resilient cluster population, while galaxies with late mergers are capable of forming massive clusters even at late cosmic epochs. We find that the phenomenological treatment of interstellar gas in EAGLE precludes the accurate modelling of cluster disruption in low-density environments, but infer that simulations incorporating an explicitly modelled cold interstellar gas phase will overcome this shortcoming.
Overview
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Integrity signals
Registry
Cites
Statistics
Verification
Claims the paper makes
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Claims other papers make about this one
Each is checked against this paper’s own text: does it say what the citing paper says it does?
The cited source says what the claim attributes to it.
In the citing paper
“Because these simulations simultaneously reproduce young and old stellar cluster populations with a single, environmentally dependent cluster formation and disruption model, they enable linking the properties of the cluster population to the assembly history of the host galaxy.”
From Kraken reveals itself – the merger history of the Milky Way reconstructed with the E-MOSAICS simulations (2020) · cites this paper as Pfeffer et al. 2018
The cited source says what the claim attributes to it.
In the citing paper
“Because E-MOSAICS overpredicts the number of GCs at masses much smaller than M 10 5 M due to underdisruption (Pfe er et al. 2018; Kruijssen et al. 2019a), we only consider GCs with z = 0 masses of M > 5 10 4 M .”
From Kraken reveals itself – the merger history of the Milky Way reconstructed with the E-MOSAICS simulations (2020) · cites this paper as Pfeffer et al. 2018
Self-check
Percentages, sums and reported differences re-computed from the paper’s own numbers.
The self-check needs the paper’s full text.
Citations
Cites
Galactic Stellar and Substellar Initial Mass Function
Chabrier, G. (2003) · Publications of the Astronomical Society of the Pacific · doi:10.1086/376392 · Cited by 9,071
STAR FORMATION IN GALAXIES ALONG THE HUBBLE SEQUENCE
Kennicutt, R. C. (1998) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.36.1.189 · Cited by 6,578
The cosmological simulation code gadget-2
Springel, V. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.09655.x · Cited by 6,368
A Catalog of Parameters for Globular Clusters in the Milky Way
Harris, W. E. (1996) · The Astronomical Journal · doi:10.1086/118116 · Cited by 4,500
Galactic Dynamics: Second Edition
Binney, J., & Tremaine, S. (2008) · doi:10.1515/9781400828722 · Cited by 4,375 · cited 3×
“Typically√ 2σ (rc)/vc ≈ 1.2, which increases the time-scale tdf by a factor ∼2 over the standard definition (with B(1) and σ = vc/ √ 2, Binney & Tremaine 2008).”
BackgroundInfluentialGalactic Stellar and Substellar Initial Mass FunctionPreprint
Chabrier, G. (2003) · Cited by 4,012
The cosmological simulation code GADGET-2
Petkova, M., & Springel, V. (2005) · Cited by 3,918
Star Formation in Galaxies Along the Hubble Sequence
Kennicutt, R. C., & Words, K. (1998) · Cited by 3,712
The EAGLE project: simulating the evolution and assembly of galaxies and their environments
Schaye, J., Crain, R. A., Bower, R. G., Furlong, M., Schaller, M., Theuns, T., Dalla Vecchia, C., Frenk, C. S., McCarthy, I. G., Helly, J. C., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu2058 · Cited by 3,601
Self-citationThe evolution of large-scale structure in a universe dominated by cold dark matter
Davis, M., Efstathiou, G., Frenk, C. S., & White, S. D. M. (1985) · The Astrophysical Journal · doi:10.1086/163168 · Cited by 3,397
Research works printed but not linked: 12
- Baumgardt, 1998, A&A, 330, 480
- Forbes, 2000, A&A, 358, 471
- Georgiev, 2010, MNRAS, 406, 1967
- Griffen, 2010, MNRAS, 405, 375
- Kaviraj, 2017, MNRAS, 467, 4739
- Lamers, 2017, A&A, A85
- Longmore, 2014, Protostars Planets VI, 914, 291
- Portinari, 1998, A&A, 334, 505
- Rahmati, 2015, MNRAS, 2034
- Sormani, 2017, MNRAS, 407
- Turner, 2017, MNRAS, 690
- Wendland, 1995, Adv. Comput. Math, 01
Cited by
Sorted by citations
Multiple Stellar Populations in Globular Clusters
Bastian, N., & Lardo, C. (2018) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081817-051839 · Cited by 737
Self-citationStar Clusters Across Cosmic Time
Krumholz, M. R., McKee, C. F., & Bland‐Hawthorn, J. (2019) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-091918-104430 · Cited by 716
Neumayer, N., Seth, A., & Böker, T. (2020) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-020-00125-0 · Cited by 450
The formation and assembly history of the Milky Way revealed by its globular cluster population
Kruijssen, J. M. D., Pfeffer, J. L., Reina-Campos, M., Crain, R. A., & Bastian, N. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1609 · Cited by 369
Self-citationKruijssen, J. M. D., Pfeffer, J. L., Chevance, M., Bonaca, A., Trujillo-Gomez, S., Bastian, N., Reina-Campos, M., Crain, R. A., & Hughes, M. E. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2452 · Cited by 252
“Most recently, these efforts have been aided by the E-MOSAICS project, which is a suite of selfconsistent, hydrodynamical cosmological simulations with a complete model for the formation and evolution of the GC population (Pfeffer et al. 2018; Kruijssen et al. 2019a).”
BackgroundMethodInfluentialSelf-citation
Metadata
- Authors
- Pfeffer, J., Kruijssen, J. M. D., Crain, R. A., & Bastian, N.
- Affiliations
- Liverpool John Moores University (GB)
- Heidelberg University (DE)
- Corresponding author
- Pfeffer, Joel
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2017-12-05
- Volume
- 475
- Issue
- 4
- Pages
- 4309-4346
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W2773772132
- Cited by
- 243
- References
- 199
- Citations by year
- 2026: 18 · 2025: 14 · 2024: 27 · 2023: 23 · 2022: 39 · 2021: 32 · 2020: 30 · 2019: 40 · 2018: 19 · 2017: 1
- FWCI
- 13.46
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- Liverpool John Moores University (acceptedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Funders
- European Research Council (ERC-CoG-646928-Multi-Pop)
- DFG (KR4801/1-1, PI Kruijssen)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- star cluster populations, globular clusters, star cluster disruption, galaxy co-evolution, EAGLE simulation, cosmological hydrodynamics, two-body relaxation, tidal field, stellar evolution, galaxy assembly history, star formation rate, disk galaxies
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
Are you an author, or do you see a problem with this page? Request a review
