A luminosity function for star clusters in the Large Magellanic Cloud

Elson, Rebecca A. W.; Fall, S. Michael

doi:10.1086/131591

Cited by 54 publications

(52 citation statements)

References 8 publications

(16 reference statements)

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“…Starting from the work by Elson & Fall (1985) on LMC SCs, empirical data from a large sample of spiral and irregular galaxies have shown that the Star Cluster Luminosity Function (SCLF) usually follows a power law, with a sharp turnover at faint magnitudes. In this section we analyse the LF profile of the SC candidate system in NGC 3370.…”

Section: Luminosity Functionsmentioning

confidence: 99%

The star cluster population of the spiral galaxy NGC 3370

Cantiello¹,

Brocato²,

Blakeslee

2009

A&A

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Aims. We study the photometric and structural properties of the star cluster system in the late type Sc spiral NGC 3370. Methods. BVI observations from the Advanced Camera for Surveys on board of HST are used to analyse in detail the colours, magnitudes and spatial properties of cluster candidates. The final catalogue of sources used for the study is composed by 277 objects. Results. The colour distributions of cluster candidates appear multi-modal. Although firm age constraints need the use of more agesensitive indicators, the comparison of cluster candidate colours with the colours of Galactic and Magellanic Clouds star clusters, suggests an age difference between the various sub-peaks, with a red old sub-system, a rich population of intermediate age (∼1 Gyr), and a blue tail of very young (below ∼100 Myr) clusters. The luminosity functions appear normal for this type of galaxy, as for the distribution of cluster effective radii (R eff ). Our analysis suggests the presence of a peak in the R eff distribution at ∼3.0 pc, with blue (likely young) cluster candidates showing smaller radii respect to red (likely old) objects. Finally, inspecting the properties of candidate globular clusters, we find a colour distribution matching with Galactic Globulars, with a median [Fe/H] ∼ −1.5 dex, though a non negligible tail towards lower metallicities is also present.

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Section: Luminosity Functionsmentioning

confidence: 99%

The star cluster population of the spiral galaxy NGC 3370

Cantiello¹,

Brocato²,

Blakeslee

2009

A&A

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“…This distribution can not be well fitted using any standard power-law luminosity function (see, e.g. Elson & Fall 1985, for the LMC star-clusters LF).…”

Section: Star-forming Regionsmentioning

confidence: 99%

Mapping the star formation history of Mrk 86

Paz¹,

Zamorano²,

Gallego³

et al. 2000

Astron. Astrophys. Suppl. Ser.

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Abstract. We have obtained optical (BV R, [O iii]λ5007Åand Hα), near infrared (JHK) imaging and long-slit optical spectroscopy for the Blue Compact Dwarf galaxy Mrk 86 (NGC 2537). In this paper, the first of two, we present optical-near-infrared colors and emission-line fluxes for the currently star-forming regions, intermediate aged starburst and underlying stellar population. We also describe the evolutionary synthesis models used in Paper II.The R and Hα luminosity distributions of the galaxy star-forming regions show maxima at M R = −9.5 m and L Hα = 10 37.3 erg s −1 . The underlying stellar population shows an exponential surface brigthness profile with central value, µ E,0 = 21.5 mag arcsec −2 , and scale, α = 0.88 kpc, both measured in the R-band image. In the galaxy outer regions, dominated by this component, no significant color gradients are observed.Finally, a complete set of evolutionary synthesis models have been developed, covering a wide range in metallicity, 1/50 Z < Z < 2 Z , and burst strength, 1 − 10 −4 . These models include nebular continuum and recombination and forbidden-line emission.

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“…However, power-law luminosity functions are generally associated with young stellar clusters, which have masses and sizes of GCs. And these younger populations generally reside in the LMC and in many starbursting and merging galaxies (e.g., Elson & Fall 1985;Meurer et al 1995;Whitmore et al 1997). And clearly, UGC 5981 does not have many young stellar cluster candidates, which are generally believed to have (V − I) < 0.5 color.…”

Section: Luminosity Function Of Globular Clustersmentioning

confidence: 99%

Hubble Space Telescope Imaging of Globular Clusters in Two Face-on Low Surface Brightness Galaxies Ugc 5981 and Ugc 6614

Kim

2011

Journal of The Korean Astronomical Society

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We present a study searching for globular cluster systems (GCSs) of two face-on low surface brightness galaxies (LSBGs), UGC 5981 and UGC 6614. Based on HST WFPC2 images of F555W and F814W filters, we detect 12 and 18 GC candidates for UGC 5981 and UGC 6614, respectively. Although these two LSBGs have very different bulge properties, they have very similar specific frequencies (S N ) of 0.1. However, S N ∼ 0.1 is quite small even for their late morphological types, albeit within errors. This suggests that LSBGs have had star formation histories lacking dominant initial starburst events while accumulating their stellar masses through sporadic star formation activities.

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A luminosity function for star clusters in the Large Magellanic Cloud

Cited by 54 publications

References 8 publications

The star cluster population of the spiral galaxy NGC 3370

The star cluster population of the spiral galaxy NGC 3370

Mapping the star formation history of Mrk 86

Hubble Space Telescope Imaging of Globular Clusters in Two Face-on Low Surface Brightness Galaxies Ugc 5981 and Ugc 6614

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