Constraints on Upper Cutoffs in the Mass Functions of Young Star Clusters

Mok, Angus; Chandar, Rupali; Fall, S. Michael

doi:10.3847/1538-4357/aaf6ea

Cited by 47 publications

(72 citation statements)

References 41 publications

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“…Baumgardt & Kroupa 2007). In Mok et al (2019), we found that cluster catalogs in M83 and M51 created by different groups, despite having somewhat different methods and criteria, gave similar results for the shape of the mass function.…”

Section: Previous Catalogs and Mass Functionsmentioning

confidence: 65%

“…To date, published cutoff masses for cluster populations are largely consistent with this expected size-of-sample effect (e.g. Mok et al 2019). In this work, we assess whether or not the data show a physical, i.e.…”

Section: Introductionmentioning

confidence: 81%

“…We assume that this flattening is due to incompleteness, rather than to a physical effect, just as we have done previously for cluster catalogs (e.g. Chandar et al 2017;Mok et al 2019). We set the completeness limit M lim for each catalog at the mass where the distribution begins to flatten noticeably, represented by the dotted lines in Figure 4, and listed in the second column of Table 3.…”

Section: Mass Functionsmentioning

confidence: 99%

“…In this Section, we use the maximum-likelihood method described in Mok et al (2019) to determine the best-fit values and confidence intervals for the parameters β and M * when fitting a Schechter function to the cluster and GMC masses above the completeness limit of each catalog. This method has the advantage of not using binned data (which can hide weak features at the ends of the distribution) or cumulative distributions (where the data points are not independent of one another).…”

Section: Maximum-likelihood Fitsmentioning

confidence: 99%

“…In this work, we uniformly apply the robust maximum-likelihood fitting method developed in Mok et al (2019) to the GMC and cluster populations in 6 nearby galaxies (LMC, M83, M51, NGC 3627, Antennae, and NGC 3256), selected to have high-quality catalogs for both populations. The galaxies span a wide range in mass, morphology, and star formation rate (SFR).…”

Section: Introductionmentioning

confidence: 99%

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Mass Functions of Giant Molecular Clouds and Young Star Clusters in Six Nearby Galaxies

Mok

Chandar

Fall

2020

ApJ

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We compare the mass functions of young star clusters (ages ≤ 10 Myr) and giant molecular clouds (GMCs) in six galaxies that cover a large range in mass, metallicity, and star formation rate (LMC, M83, M51, NGC 3627, the Antennae, and NGC 3256). We perform maximum-likelihood fits of the Schechter function, ψ(M ) = dN/dM ∝ M β exp(−M/M * ), to both populations. We find that most of the GMC and cluster mass functions in our sample are consistent with a pure power-law distribution (M * → ∞). M51 is the only galaxy that shows some evidence for an upper cutoff (M * ) in both populations. Therefore, physical upper mass cutoffs in populations of both GMCs and clusters may be the exception rather than the rule. When we perform power-law fits, we find a range of indices β PL = −2.3 ± 0.3 for our GMC sample and β PL = −2.0 ± 0.3 for the cluster sample. This result, that β Clusters ≈ β GMC ≈ −2, is consistent with theoretical predictions for cluster formation and suggests that the star-formation efficiency is largely independent of mass in the GMCs.

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Section: Previous Catalogs and Mass Functionsmentioning

confidence: 65%

Section: Introductionmentioning

confidence: 81%

Section: Mass Functionsmentioning

confidence: 99%

Section: Maximum-likelihood Fitsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Mass Functions of Giant Molecular Clouds and Young Star Clusters in Six Nearby Galaxies

Mok

Chandar

Fall

2020

ApJ

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Star Clusters Near and Far

et al. 2020

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Star clusters are fundamental units of stellar feedback and unique tracers of their host galactic properties. In this review, we will first focus on their constituents, i.e. detailed insight into their stellar populations and their surrounding ionised, warm, neutral, and molecular gas. We, then, move beyond the Local Group to review star cluster populations at various evolutionary stages, and in diverse galactic environmental conditions accessible in the local Universe. At high redshift, where conditions for cluster formation and evolution are more extreme, we are only able to observe the integrated light of a handful of objects that we believe will become globular clusters. We therefore discuss how numerical and analytical methods, informed by the observed properties of cluster populations in the local Universe, are used to develop sophisticated simulations potentially capable of disentangling the genetic map of galaxy formation and assembly that is carried by globular cluster populations.

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Pre-supernova feedback sets the star cluster mass function to a power law and reduces the cluster formation efficiency

Andersson,

Mac Low,

Agertz

et al. 2024

A&A

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Context. The star cluster initial mass function is observed to have an inverse power law exponent around 2, yet there is no consensus on what determines this distribution, and why some variation is observed in different galaxies. Furthermore, the cluster formation efficiency (CFE) covers a range of values, particularly when considering different environments. These clusters are often used to empirically constrain star formation and as fundamental units for stellar feedback models. Detailed galaxy models must therefore accurately capture the basic properties of observed clusters to be considered predictive. Aims. We study how feedback mechanisms acting on different timescales and with different energy budgets affect the star cluster mass function and CFE. Methods. We use hydrodynamical simulations of a dwarf galaxy as a laboratory to study star cluster formation. We test different combinations of stellar feedback mechanisms, including stellar winds, ionizing radiation, and supernovae (SNe). Results. Each feedback mechanism affects the CFE and cluster mass function. Increasing the feedback budget by combining the different types of feedback decreases the CFE by reducing the number of massive clusters. Ionizing radiation is found to be especially influential. This effect depends on the timing of feedback initiation, as shown by comparing early and late feedback. Early feedback occurs from ionizing radiation and stellar winds with onset immediately after a massive star is formed. Late feedback occurs when energy injection only starts after the main-sequence lifetime of the most massive SN progenitor, a timing that is further influenced by the choice of the most massive SN progenitor. Late feedback alone results in a broad, flat mass function, approaching a log-normal shape in the complete absence of feedback. Early feedback, on the other hand, produces a power-law cluster mass function with lower CFE, albeit with a steeper slope than that usually observed.

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Constraints on Upper Cutoffs in the Mass Functions of Young Star Clusters

Cited by 47 publications

References 41 publications

Mass Functions of Giant Molecular Clouds and Young Star Clusters in Six Nearby Galaxies

Mass Functions of Giant Molecular Clouds and Young Star Clusters in Six Nearby Galaxies

Star Clusters Near and Far

Pre-supernova feedback sets the star cluster mass function to a power law and reduces the cluster formation efficiency

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