The Clustering Behavior of Pre-Main-Sequence Stars in NGC 346 in the Small Magellanic Cloud

Schmeja, S.; Gouliermis, D. A.; Klessen, Ralf S.

doi:10.1088/0004-637x/694/1/367

Cited by 37 publications

(43 citation statements)

References 71 publications

(81 reference statements)

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“…This result agrees well with previous works, which also reveal hierarchically sub-grouped young stellar structures in individual star-forming regions (e.g. Schmeja et al 2009;Kirk & Myers 2011;Gouliermis et al 2014) or over the whole galaxies (e.g. Gouliermis et al 2010Gouliermis et al , 2015Gusev 2014).…”

Section: Group Identification and Dendrogramssupporting

confidence: 93%

The VMC Survey. XXII. Hierarchical Star Formation in the 30 Doradus-N158–N159–N160 Star-forming Complex

Sun

Grijs

Subramanian

et al. 2017

ApJ

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We study the hierarchical stellar structures in a ∼1.5 deg 2 area covering the 30 Doradus-N158-N159-N160 star-forming complex with the VISTA Survey of the Magellanic Clouds. Based on the young upper main-sequence stars, we find that the surface densities cover a wide range of values, from log(Σ·pc 2 ) −2.0 to log(Σ·pc 2 ) 0.0. Their distributions are highly non-uniform, showing groups that frequently have sub-groups inside. The sizes of the stellar groups do not exhibit characteristic values, and range continuously from several parsecs to more than 100 pc; the cumulative size distribution can be well described by a single power law, with the power-law index indicating a projected fractal dimension D 2 = 1.6 ± 0.3. We suggest that the phenomena revealed here support a scenario of hierarchical star formation. Comparisons with other star-forming regions and galaxies are also discussed.

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Section: Group Identification and Dendrogramssupporting

confidence: 93%

The VMC Survey. XXII. Hierarchical Star Formation in the 30 Doradus-N158–N159–N160 Star-forming Complex

Sun

Grijs

Subramanian

et al. 2017

ApJ

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“…Our results support the idea that stars in newly born clusters likely follow the fractal patterns of their parent molecular clouds, and that they eventually evolve towards more centrally concentrated structures (see Schmeja & Klessen 2006;Schmeja et al 2008Schmeja et al , 2009Sánchez et al 2007aSánchez et al , 2009). However, this seems to be only an overall trend.…”

Section: Discussionsupporting

confidence: 85%

The spatial distribution of stars in open clusters

Sánchez¹,

Alfaro²

2009

Proc. IAU

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Abstract. We study the internal spatial structure of 16 open clusters in the Milky Way spanning a wide range of ages. For this, we use the minimum-spanning-tree method (the Q parameter, which enables one to classify the stellar distribution as either radially or fractally clustered), King-profile fitting, and the correlation dimension (Dc ) for those clusters with fractal patterns. On average, clusters with fractal-like structure are younger than those exhibiting radial stellardensity profiles. There is a significant correlation between Q and the cluster age measured in crossing-time units. For fractal clusters, there is a significant correlation between fractal dimension and age. These results support the idea that stars in newly born clusters likely follow the fractal patterns of their parent molecular clouds, and eventually evolve towards more centrally concentrated structures. However, stellar clusters as old as ∼ 100 Myr can exist that have not totally destroyed their fractal structure. Finally, we have found the intriguing result that the lowest fractal dimensions obtained for the open clusters seem to be considerably smaller than the average value measured in Galactic molecular cloud complexes.

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“…In Testor et al (2005) a pure H 2 emission is detected in N88A at low spatial resolution, as well as along a north-south diffuse long filament at ∼6−8 to the east. In N66 (Henize 1956), which is a giant HII region in the SMC, Schmeja et al (2009) have reported that most of the H 2 emission peaks coincide with the bright component of the ionized gas and with compact embedded young clusters where candidate YSOs have been identified. Using SEST, Israel et al (2003) detected a CO molecular cloud of 1.5 × 1.5 in the region, reporting spectra and maps of the 12 CO lines J = 1−0 and J = 2−1.…”

Section: Introductionmentioning

confidence: 99%

VLT/NACO near-infrared imaging and spectroscopy of N88A in the SMC

Testor¹,

Lemaire

Heydari-Malayeri³

et al. 2010

A&A

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Aims. We present near-infrared imaging and spectroscopic high spatial resolution observations of the SMC region N88 containing the bright, excited, extincted and compact H II region N88A of the size of about 1 pc. Methods. To investigate its stellar content and reddening, N88 was observed using spectroscopy and imagery in the JHKs-and L -band at a spatial resolution of ∼0.1−0.3 , using the VLT UT4 equipped with the NAOS adaptive optics system. In an attempt to establish if the origin of the infra-red (IR) excess is due to bright nebulosity, circumstellar material and/or local dust, we used Ks vs. J − K color−magnitude (CM) and JHK color−color (CC) diagrams, as well as L imagery. Results. Our IR-data reveal in the N88 area an IR-excess fraction of ≥30 per cent of the detected stars as well as an unprecedently detailed morphology of N88A. It consists of an embedded cluster of ∼3.5 (∼1 pc) in diameter of at least thirteen resolved stars superposed with an unusual bright continuum centered on a very bright star. The four brightest stars in this cluster lie red-ward of H − K ≥ 0.45 mag and could be classified as young stellar object (YSO) candidates. Four other probable YSO candidates are also detected in N88 along a north-south bow-shaped thin H 2 filament at ∼7 east of the young central bright star. This star, which we assume to be the main exciting source, could also be complex. At 0.2 east of this star, a heavily embedded core is detected in the L -band. This core with L ∼ 14 mag and L − K ≥ 4.5 mag could be a massive class I protostar candidate. The 2.12 μm H 2 image of N88A resembles a shell of a diameter of ∼3 (∼0.9 pc) centered on the bright star. This shell consists of three bright components, of which the brightest one superposes the ionization front. The line ratios of H 2 2−1 S(1) and 1−0 S(0) relative to 1−0 S(1), as well as the presence of high v lines, are indicative of photodissociation regions, rather than shocks.

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The Clustering Behavior of Pre-Main-Sequence Stars in NGC 346 in the Small Magellanic Cloud

Cited by 37 publications

References 71 publications

The VMC Survey. XXII. Hierarchical Star Formation in the 30 Doradus-N158–N159–N160 Star-forming Complex

The VMC Survey. XXII. Hierarchical Star Formation in the 30 Doradus-N158–N159–N160 Star-forming Complex

The spatial distribution of stars in open clusters

VLT/NACO near-infrared imaging and spectroscopy of N88A in the SMC

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