The Low End of the Initial Mass Function in Young Large Magellanic Cloud Clusters. I. The Case of R136

Sirianni, M.; Nota, A.; Leitherer, Claus; Marchi, Guido De; Clampin, Mark

doi:10.1086/308628

Cited by 101 publications

(132 citation statements)

References 26 publications

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“…To plot the isochrones we assumed a distance modulus of (m − M) 0 = 18.9, the Galactic extinction law, a reddening of E(B − V ) = 0.08, and A F 555W = 0.19. An inspection by eye of Figure 5 shows that, as found in several other SMC stellar fields (i.e., Sirianni et al 2002;McCumber et al 2005;Nota et al 2006;Sabbi et al 2007;Chiosi & Vallenari 2007;Carlson et al 2007;Noël et al 2007;Sabbi et al 2009) (Keller et al 2000). This is also confirmed by the few red supergiant stars brighter than m F814W > 13.1 and redder than m F555W − m F814W > 1.24.…”

Section: Color-magnitude Diagramssupporting

confidence: 78%

“…As for other young star clusters (de Grijs et al 2002;Sirianni et al 2002;Stolte et al 2002;Gouliermis et al 2004;Sabbi et al 2008) the steepening of the PDMF with distance from the center is caused by a lack of massive stars rather than an excess of low-mass stars in the outskirts. The paucity of massive stars in the halo of a star cluster is normally interpreted as a signature of mass segregation.…”

Section: Present-day Luminosity and Mass Functionsmentioning

confidence: 74%

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Is the Young Star Cluster NGC 376 Dissolving in the Field of the Small Magellanic Cloud?

Sabbi

Nota

Tosi

et al. 2011

ApJ

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We use deep images acquired with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope in the filters F555W and F814W to characterize the properties of NGC 376, a young star cluster located in the wing of the Small Magellanic Cloud. Using isochrone fitting we derive for NGC 376 an age of 28 ± 7 Myr, in good agreement with previous studies. The high spatial resolution ACS data allow us to determine the center of gravity of the cluster and to construct extended surface brightness and radial density profiles. Neither of these profiles can be fitted with a theoretical model, suggesting that the cluster is not in virial equilibrium. Considering the young age of the cluster, we speculate that the distortion of the radial profiles may be the result of the rapid gas dispersal that follows the initial phase of star formation (SF). The cluster shows clear evidence of dynamical mass segregation. From the properties of the radial profiles and the present-day mass function we conclude that NGC 376 appears to have already lost nearly 90% of its initial stellar mass, probably as a consequence of the sudden gas dispersal that follows the early phase of SF.

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Section: Color-magnitude Diagramssupporting

confidence: 78%

Section: Present-day Luminosity and Mass Functionsmentioning

confidence: 74%

Is the Young Star Cluster NGC 376 Dissolving in the Field of the Small Magellanic Cloud?

Sabbi

Nota

Tosi

et al. 2011

ApJ

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“…Unfortunately the IMF can be determined directly by photometry of individual stars only in very nearby galaxies. In the main star formation region of the Large Magellanic Cloud, 30 Doradus, the IMF of the central cluster R 136 is close to the classical Salpeter one from 3 to >100 M , with some flattening below 2 M (Sirianni et al 2000). Similar, although less precise, results exist for other young clusters or associations of the Magellanic Clouds (Parker et al 1992;Oey & Massey 1995;Holtzman et al 1997), suggesting that the IMF is similar in all these objects.…”

Section: Introductionmentioning

confidence: 53%

H$_\gamma$ and H$_\delta$ absorption lines and the Initial Mass Function in extragalactic star forming regions

Sinanian

Kunth

Lequeux

et al. 2002

A&A

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Abstract. High-dispersion, long-slit spectroscopic observations of 13 extragalactic star-forming regions were obtained for two Blue Compact Dwarf galaxies (IZw18, IZw36) and for bright star-formation regions in the spiral galaxies M 101 and M 51 and in the irregular starburst galaxies Mrk 171 and NGC 4449. The H γ and/or H δ absorption lines have been observed in 11 star forming regions and will be used to constrain the Initial Mass Function and age of the young stellar populations. In this paper we present the results of the observations and the measurements of the absorption and emission lines. The astrophysical discussion is deferred to a forthcoming paper.

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“…Two supernova remnant (SNR) candidates have also been identified (Lazendic et al 2003). Using deep broadband I and V WFPC2 images from the HST, Sirianni et al (2000) derived the IMF for the central cluster R136 in 30 Doradus down to 1.35 M , suggesting there are relatively fewer lower-mass stars than in the Galactic IMF (though this may also arise from not fully correcting for extinction from the source). IR and radio observations show molecular gas and warm dust concentrated in an arc to the north and west of the central cluster (Rubio et al 1998).…”

Section: Doradusmentioning

confidence: 99%

L-band (3.5 $\mathsf{\mu}$m) IR-excess in massive star formation

Maercker¹,

Burton²

2005

A&A

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Abstract. L-band data of 30 Doradus at 3.5 µm taken with SPIREX (South Pole Infrared Explorer) is presented. The photometry was combined with 2MASS JHK data at 1.25−2.2 µm. Colour−colour and colour−magnitude diagrams are constructed and used to determine the sources with infrared excess. These are interpreted as circumstellar disks, and enable the fraction of sources with disks (the cluster disk fraction or CDF) to be determined. We find that ∼42% of the sources detected at L-band in 30 Doradus have an IR-excess.

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The Low End of the Initial Mass Function in Young Large Magellanic Cloud Clusters. I. The Case of R136

Cited by 101 publications

References 26 publications

Is the Young Star Cluster NGC 376 Dissolving in the Field of the Small Magellanic Cloud?

Is the Young Star Cluster NGC 376 Dissolving in the Field of the Small Magellanic Cloud?

H$_\gamma$ and H$_\delta$ absorption lines and the Initial Mass Function in extragalactic star forming regions

L-band (3.5 $\mathsf{\mu}$m) IR-excess in massive star formation

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