THE LUMINOSITY, MASS, AND AGE DISTRIBUTIONS OF COMPACT STAR CLUSTERS IN M83 BASED ON<i>HUBBLE SPACE TELESCOPE</i>/WIDE FIELD CAMERA 3 OBSERVATIONS

Chandar, Rupali; Whitmore, Bradley C.; Kim, Hwi; Kaleida, Catherine; Mutchler, Max; Calzetti, Daniela; Saha, Abhijit; O’Connell, R. W.; Balick, Bruce; Bond, Howard E.; Carollo, M.; Disney, M. J.; Dopita, Michael A.; Frogel, J. A.; Hall, Donald N. B.; Holtzman, Jon A.; Kimble, Randy A.; McCarthy, Patrick J.; Paresce, Francesco; Silk, Joseph; Trauger, John T.; Walker, A. R.; Windhorst, Rogier A.; Young, Erick T.

doi:10.1088/0004-637x/719/1/966

Cited by 127 publications

(213 citation statements)

References 36 publications

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“…The bottom panel of Figure 4 shows the U−B versus V−I two-color distribution of our training set. The stars (open circles) are red supergiants, and fall away from the cluster tracks but are well matched to stellar tracks (see for example, Figure 7 in Chandar et al 2010b). Note that many of the stars are too faint to have U band measurements and so are not shown in this figure. The colors of the clusters clearly follow the model predictions.…”

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confidence: 85%

“…In order to separate star clusters from individual stars and blends of two or more stars, we follow the general approach described in Whitmore et al (2010) and Chandar et al (2010b), where we construct "training sets" of stars and clusters and use their measured properties to guide the criteria used to automatically select clusters. Figure 4 shows the separation of isolated stars from young, intermediate-age, and old globular clusters that were selected by hand.…”

Section: Cluster Selectionmentioning

confidence: 99%

“…We also apply size-dependent aperture corrections to each cluster, based on their measured CI value. As in Chandar et al (2010b), we determine a relationship between the aperture correction and CI value for clusters, using measurements of artificial clusters added to the M51 image. While this approach is better in principle, it does not work well for clusters with poorly determined values of CI, either because they have low S/N or because they are in very crowded regions.…”

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confidence: 99%

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The Age, Mass, and Size Distributions of Star Clusters in M51

Chandar

Whitmore

DiNino

et al. 2016

ApJ

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We present a new catalog of 3816 compact star clusters in the grand design spiral galaxy M51 based on observations taken with the Hubble Space Telescope. The age distribution of the clusters declines starting at very young ages, and can be represented by a power law,, with g = - 0.65 0.15. No significant changes in the shape of the age distribution at different masses is observed. The mass function of the clusters younger than t » 400 Myr can also be described by a power law, µ b dN dM M , with b » - 2.1 0.2. We compare these distributions with the predictions from various cluster disruption models, and find that they are consistent with models where clusters disrupt approximately independent of their initial mass, but not with models where lower mass clusters are disrupted earlier than their higher mass counterparts. We find that the half-light radii of clusters more massive than »´ M M 3 10 4and with ages between 100 and 400 Myr are larger by a factor of ≈3-4 than their counterparts that are younger than 10 7 years old, suggesting that the clusters physically expand during their early life.

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confidence: 85%

Section: Cluster Selectionmentioning

confidence: 99%

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confidence: 99%

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The Age, Mass, and Size Distributions of Star Clusters in M51

Chandar

Whitmore

DiNino

et al. 2016

ApJ

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“…Taking T L (U) as a proxy for the cluster formation efficiency, these data thus suggested an increase in the cluster formation efficiency with Σ SFR . It is worth noting here that the Σ SFR values were derived by normalizing Mora et al (2009) and references therein; (a) Schlegel et al (1998); (1) Bresolin et al (2009); (2) Chandar et al (2010b); (3) Walsh & Roy (1997); Larsen et al (2007); (4) Mora et al (2007) ; (5) and Zaritsky et al (1994) at r = 3 Kpc. Chandar et al (2010b) for the galaxies NGC 5236 and NGC 7793, where they found similar values to Larsen & Richtler (2000).…”

Section: Dataset Overviewmentioning

confidence: 99%

“…Harris et al find a large number of young and massive clusters, consistent with a burst of star formation that began around 10 Myr ago, but note that the apparent absence of older clusters might also be due to rapid disruption. Chandar et al (2010c) used the new Wide Field Camera 3 (WFC3) on HST to analyze the cluster system of NGC 5236. They find that luminosity functions and age distributions are consistent with previous work on galaxies of different morphological types (e.g.…”

Section: Dataset Overviewmentioning

confidence: 99%

The star cluster – field star connection in nearby spiral galaxies

Silva-Villa

Larsen

2011

A&A

109

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Context. Recent studies have started to cast doubt on the assumption that most stars are formed in clusters. Observational studies of field stars and star cluster systems in nearby galaxies can lead to better constraints on the fraction of stars forming in clusters. Ultimately this may lead to a better understanding of star formation in galaxies, and galaxy evolution in general. Aims. We aim to constrain the amount of star formation happening in long-lived clusters for four galaxies through the homogeneous, simultaneous study of field stars and star clusters. Methods. Using HST/ACS and HST/WFPC2 images of the galaxies NGC 45, NGC 1313, NGC 5236, and NGC 7793, we estimate star formation histories by means of the synthetic CMD method. Masses and ages of star clusters are estimated using simple stellar population model fitting. Comparing observed and modeled luminosity functions, we estimate cluster formation rates. By randomly sampling the stellar initial mass function (SIMF), we construct artificial star clusters and quantify how stochastic effects influence cluster detection, integrated colors, and age estimates. Results. Star formation rates appear to be constant over the past 10 7 −10 8 years within the fields covered by our observations. The number of clusters identified per galaxy varies, with a few detected massive clusters (M ≥ 10 5 M ) and a few older than 1 Gyr. Among our sample of galaxies, NGC 5236 and NGC 1313 show high star and cluster formation rates, while NGC 7793 and NGC 45 show lower values. We find that stochastic sampling of the SIMF has a strong impact on the estimation of ages, colors, and completeness for clusters with masses ≤10 3 −10 4 M , while the effect is less pronounced for high masses. Stochasticity also makes size measurements highly uncertain at young ages (τ 10 8 yr), making it difficult to distinguish between clusters and stars based on sizes. Conclusions. The ratio of star formation happening in clusters (Γ) compared to the global star formation appears to vary for different galaxies. We find similar values to previous studies (Γ ≈ 2%-10%), but we find no obvious relation between Γ and the star formation rate density (Σ SFR ) within the range probed here (Σ SFR ∼ 10 −3 −10 −2 M yr −1 kpc −2 ). The Γ values do, however, appear to correlate with the specific U-band luminosity (T L (U), the fraction of total light coming from clusters compared to the total U-band light of the galaxy).

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The Lifecycle of Clusters in Galaxies

Adamo

Bastian

2017

The Birth of Star Clusters

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We review many of the basic properties of star cluster systems, and focus in particular on how they relate to their host galaxy properties and ambient environment. The cluster mass and luminosity functions are well approximated by power-laws of the form Ndm ∝ M α dm, with α ∼ −2 over most of the observable range. However, there is now clear evidence that both become steeper at high masses/luminosities, with the value of the downward turn dependent on environment. The host galaxy properties also appear to affect the cluster formation efficiency (Γ -i.e., the fraction of stars that form in bound clusters), with higher starformation rate density galaxies having higher Γ values. Within individual galaxies, there is evidence for Γ to vary by a factor of 3 − 4, likely following the molecular gas surface density, in agreement with recent predictions. Finally, we discuss cluster disruption and its effect on the observed properties of a population, focussing on the age distribution of clusters. We briefly discuss the expectations of theoretical and numerical studies, and also the observed distributions in a number of galaxies. Most observational studies now find agreement with theoretical expectations, namely nearly a constant cluster age distribution for ages up to ∼ 100 Myr (i.e. little disruption), and a drastic steepening above this value caused by a combination of cluster disruption and incompleteness. Rapid cluster disruption for clusters with ages < 100 Myr is ruled out for most galaxies.

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THE LUMINOSITY, MASS, AND AGE DISTRIBUTIONS OF COMPACT STAR CLUSTERS IN M83 BASED ONHUBBLE SPACE TELESCOPE/WIDE FIELD CAMERA 3 OBSERVATIONS

Cited by 127 publications

References 36 publications

The Age, Mass, and Size Distributions of Star Clusters in M51

The Age, Mass, and Size Distributions of Star Clusters in M51

The star cluster – field star connection in nearby spiral galaxies

The Lifecycle of Clusters in Galaxies

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