Great Balls of FIRE I: The formation of star clusters across cosmic time in a Milky Way-mass galaxy

Grudić, Michael Y.; Hafen, Zachary; Rodriguez, Carl L.; Guszejnov, Dávid; Lamberts, Astrid; Wetzel, Andrew; Boylan-Kolchin, Michael; Faucher-Giguère, Claude-André

doi:10.48550/arxiv.2203.05732

Cited by 7 publications

(8 citation statements)

References 124 publications

(226 reference statements)

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“…To fully model clusters, one possibility for cosmological or galactic simulations is to include the cluster evolution separately using a theoretical or empirical model (Pfeffer et al 2018) or by separately evolving a sample of clusters (Grudić et al 2022). An alternative approach is to model the full population of stars with Nbody dynamics (Fujii et al 2021;Rieder et al 2022;Liow et al 2022), even if the gas resolution is low, thus achieving the same resolution in the stars as individual cluster simulations.…”

Section: Introductionmentioning

confidence: 99%

The formation of clusters and OB associations in different density spiral arm environments

Dobbs

Bending

Pettitt

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present simulations of the formation and evolution of clusters in spiral arms. The simulations follow two different spiral arm regions, and the total gas mass is varied to produce a range of different mass clusters. We find that including photoionizing feedback produces the observed cluster mass radius relation, increasing the radii of clusters compared to without feedback. Supernovae have little impact on cluster properties. We find that in our high density, high gas mass simulations, star formation is less affected by feedback, as star formation occurs rapidly before feedback has much impact. In our lowest gas density simulation, the resulting clusters are completely different (e.g. the number of clusters and their masses) to the case with no feedback. The star formation rate is also significantly suppressed. The fraction of stars in clusters in this model decreases with time flattening at about 20 per cent. In our lowest gas simulation model, we see the formation of a star forming group with properties similar to an OB association, in particular similar to Orion Ia. We suggest that low densities, and stronger initial dynamics are conducive to forming associations rather than clusters. In all models cluster formation is complex with clusters merging and splitting. The most massive clusters which form have tended to undergo more mergers.

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Section: Introductionmentioning

confidence: 99%

The formation of clusters and OB associations in different density spiral arm environments

Dobbs

Bending

Pettitt

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…Star clus-ters form and evolve within their host galaxies across cosmic times (e.g Adamo et al 2020a). State-of-art cosmological simulations follow cluster formation and evolution during galaxy assembly like the Milky Way and M31 (e.g., Grudić et al 2022;Reina-Campos et al 2022, among the latest). These simulations agrees that the peak formation of massive star clusters (masses > 10 5 M ) is around redshift 3 (Reina-Campos et al 2019) in these Milky-Way like progenitors.…”

Section: Introductionmentioning

confidence: 99%

Star formation at the smallest scales; A JWST study of the clump populations in SMACS0723

Claeyssens¹,

Adamo²,

Richard³

et al. 2022

Preprint

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We present the clump populations detected in 18 lensed galaxies at redshifts 1 to 8 within the lensing cluster field SMACS0723. The recent JWST Early Release Observations of this poorly known region of the sky have revealed numerous point-like sources within and surrounding their host galaxies, undetected in the shallower HST images. We use JWST multiband photometry and the lensing model of this galaxy cluster to estimate the intrinsic sizes and magnitudes of the stellar clumps. We derive optical restframe effective radii from <10 to 100s pc and masses ranging from ∼ 10 5 to 10 8 M , overlapping with massive star clusters in the local universe. The ages range from 1 to 100s Myr. We compare the crossing time to the age of the clumps and determine that between 30 and 50 % of the detected clumps are consistent with being gravitationally bound. The lack of Gyr old clumps suggest that the dissolution time scales are shorter than 1 Gyr. We see a significant increase in the luminosity (mass) surface density of the clumps with redshift. Clumps in galaxies at the reionisation era have stellar densities higher than massive clusters in the local universe. We zoom-in into single galaxies at redshift < 6 and find for two galaxies, the Sparkler and the Firework, that their star clusters/clumps show distinctive color distributions and location within and surrounding their host galaxy that are compatible with recent (100-500 Myr) merger events. Our study, conducted on a small sample of galaxies, shows the potential of JWST observations for understanding the conditions under which star clusters form in rapidly evolving galaxies.

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“…Additionally, compressive tides and/or shock compression due to galaxy mergers are likely to have played an important role in GC formation (Renaud et al 2015;Kim et al 2018b;Lahén et al 2019). Improving upon tagging methods, Grudić et al (2022b) applied a cluster formation model derived from their GMC simulations (Grudić et al 2021) to a Milky Way-like galaxy, and showed that the clus-ter mass-size relation observed in nearby star-forming galaxies can be explained if denser GMCs form clusters with high efficiency. However, the detailed formation processes have not yet been rigorously investigated.…”

Section: Introductionmentioning

confidence: 99%

Impact of Radiation Feedback on the Formation of Globular Cluster Candidates during Cloud–Cloud Collisions

Han

Kimm

Katz

et al. 2022

ApJ

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To understand the impact of radiation feedback during the formation of a globular cluster (GC), we simulate a head-on collision of two turbulent giant molecular clouds (GMCs). A series of idealized radiation-hydrodynamic simulations is performed, with and without stellar radiation or Type II supernovae. We find that a gravitationally bound, compact star cluster of mass M GC ∼ 105 M ⊙ forms within ≈3 Myr when two GMCs with mass M GMC = 3.6 × 105 M ⊙ collide. The GC candidate does not form during a single collapsing event but emerges due to the mergers of local dense gas clumps and gas accretion. The momentum transfer due to the absorption of the ionizing radiation is the dominant feedback process that suppresses the gas collapse, and photoionization becomes efficient once a sufficient number of stars form. The cluster mass is larger by a factor of ∼2 when the radiation feedback is neglected, and the difference is slightly more pronounced (16%) when extreme Lyα feedback is considered in the fiducial run. In the simulations with radiation feedback, supernovae explode after the star-forming clouds are dispersed, and their metal ejecta are not instantaneously recycled to form stars.

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Great Balls of FIRE I: The formation of star clusters across cosmic time in a Milky Way-mass galaxy

Cited by 7 publications

References 124 publications

The formation of clusters and OB associations in different density spiral arm environments

The formation of clusters and OB associations in different density spiral arm environments

Star formation at the smallest scales; A JWST study of the clump populations in SMACS0723

Impact of Radiation Feedback on the Formation of Globular Cluster Candidates during Cloud–Cloud Collisions

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