A possible sequential star formation in the giant molecular cloud G174+2.5

Camargo, Denilso; Bonatto, Charles Jose; Bica, E.

doi:10.1111/j.1365-2966.2011.19150.x

Cited by 34 publications

(66 citation statements)

References 69 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…14 in Camargo et al (2013). Black circles are clusters in the present work and brown circles ECs from our previous studies (Camargo et al 2010(Camargo et al , 2011(Camargo et al , 2012(Camargo et al , 2013(Camargo et al , 2015a.…”

Section: Discussionmentioning

confidence: 52%

“…It has been used in several works (e.g. Camargo et al 2009Camargo et al , 2010Camargo et al , 2011Camargo et al , 2012Camargo et al , 2013, 2011a, and references therein). The cluster structure is analysed by means of the stellar radial density profile (RDP) built with stars selected after applying the respective colour magnitude (CM) filter to the observed photometry.…”

Section: Methods Of Analysismentioning

confidence: 99%

“…We have contributed significantly to increase the number of ECs with derived parameters (Camargo et al 2009(Camargo et al , 2010(Camargo et al , 2011(Camargo et al , 2012(Camargo et al , 2013(Camargo et al , 2015a eters, in Camargo et al (2015a) we discovered 437 ECs and stellar groups increasing the Galactic EC sample. Majaess (2013) has also made a significant contribution on young clusters (see also, Bica et al 2003a,b;Lada & Lada 2003;Mercer et al 2005;Froebrich, Scholz & Raftery 2007;Borissova et al 2011;Solin, Haikala & Ukkonen 2014).…”

Section: Introductionmentioning

confidence: 93%

See 2 more Smart Citations

Tracing the Galactic spiral structure with embedded clusters

Camargo

Bonatto

Bica

2015

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

In the present work we investigate the properties of 18 embedded clusters (ECs). The sample includes 11 previously known clusters and we report the discovery of 7 ECs on WISE images, thus complementing our recent list of 437 new clusters. The main goal is to use such clusters to shed new light on the Galactic structure by tracing the spiral arms with cluster distances. Our results favour a four-armed spiral pattern tracing three arms, Sagitarius-Carina, Perseus, and the Outer arm. The SagitariusCarina spiral arm is probed in the borderline of the third and fourth quadrants at a distance from the Galactic centre of d 1 ∼ 6.4 kpc adopting R ⊙ = 7.2 kpc, or d 2 ∼ 7.2 kpc for R ⊙ = 8.0 kpc. Most ECs in our sample are located in the Perseus arm that is traced in the second and third quadrants and appear to be at Galactocentric distances in the range d 1 = 9 − 10.5 kpc or d 2 = 9.8 − 11.3 kpc. Dolidze 25, Bochum 2, and Camargo 445 are located in the Outer arm that extends along the second and third Galactic quadrants with a distance from the Galactic centre in the range of d 1 = 12.5 − 14.5 kpc or d 2 = 13.5 − 15.5 kpc. We find further evidence that in the Galaxy ECs are predominantly located within the thin disc and along spiral arms. They are excellent tools for tracing these Galactic features and therefore new searches for ECs can contribute to a better understanding of the Galactic structure. We also report an EC aggregate located in the Perseus arm.

show abstract

Section: Discussionmentioning

confidence: 52%

Section: Methods Of Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 93%

See 1 more Smart Citation

Tracing the Galactic spiral structure with embedded clusters

Camargo

Bonatto

Bica

2015

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

“…For instance, Camargo et al (2011) summarises the concepts first discussed by Lada & Lada (2003) suggesting that the structure of embedded clusters is related to the structure of their original molecular cloud. Fractal structures are observed in clouds that have multiple peaks in their density profile (Cartwright & Whitworth 2004;Schmeja et al 2008;Sánchez et al 2010, LWC11).…”

Section: Comparing Clouds and Clustersmentioning

confidence: 99%

Probing the anomalous extinction of four young star clusters: the use of colour-excess, main-sequence fitting and fractal analysis

Fernandes

Gregorio-Hetem

Hetem

2012

A&A

View full text Add to dashboard Cite

Aims. We studied four young star clusters to characterise their anomalous extinction or variable reddening and asses whether they could be due to contamination by either dense clouds or circumstellar effects. Methods. We evaluated the extinction law (R V ) by adopting two methods: (i) the use of theoretical expressions based on the colourexcess of stars with known spectral type; and (ii) the analysis of two-colour diagrams, where the slope of the observed colour distribution was compared to the normal distribution. An algorithm to reproduce the zero-age main-sequence (ZAMS) reddened colours was developed to derive the average visual extinction (A V ) that provides the closest fit to the observational data. The structure of the clouds was evaluated by means of a statistical fractal analysis, designed to compare their geometric structure with the spatial distribution of the cluster members. Results. The cluster NGC 6530 is the only object of our sample affected by anomalous extinction. On average, the other clusters suffer normal extinction, but several of their members, mainly in NGC 2264, seem to have high R V , probably because of circumstellar effects. The ZAMS fitting provides A V values that are in good agreement with those found in the literature. The fractal analysis shows that NGC 6530 has a centrally concentrated distribution of stars that differs from the substructures found in the density distribution of the cloud projected in the A V map, suggesting that the original cloud was changed by the cluster formation. However, the fractal dimension and statistical parameters of Berkeley 86, NGC 2244, and NGC 2264 indicate that there is a good cloud-cluster correlation, when compared to other works based on an artificial distribution of points.

show abstract

“…Kumar & Schmeja 2007;Caballero 2008;Allison et al 2009b;Küpper et al 2011;Camargo, Bonatto & Bica 2011;Gagné et al 2015), the distribution of cores in the Galaxy (Planck Collaboration et al 2011), the evolution of stellar distributions in the Magellanic Clouds and other external galaxies (Gieles, Bastian & Ercolano 2008;Bastian et al 2009;Gouliermis et al 2010;Bastian et al 2011;Haschke, Grebel & Duffau 2012;Gouliermis et al 2015), and even the distribution of field objects near radio galaxies (Keshelava & Verkhodanov 2015).…”

Section: Introductionmentioning

confidence: 99%

$\mathcal {Q}^{+}$: characterizing the structure of young star clusters

Jaffa¹,

Whitworth²,

Lomax³

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Many young star clusters appear to be fractal, i.e. they appear to be concentrated in a nested hierarchy of clusters within clusters. We present a new algorithm for statistically analysing the distribution of stars to quantify the level of sub-structure. We suggest that, even at the simplest level, the internal structure of a fractal cluster requires the specification of three parameters. (i) The 3D fractal dimension, D, measures the extent to which the clusters on one level of the nested hierarchy fill the volume of their parent cluster. (ii) The number of levels, L, reflects the finite ratio between the linear size of the large root-cluster at the top of the hierarchy, and the smallest leafclusters at the bottom of the hierarchy. (iii) The volume-density scaling exponent,measures the factor by which the excess density, δn, in a structure of scale L, exceeds that of the background formed by larger structures; it is similar, but not exactly equivalent, to the exponent in Larson's scaling relation between density and size for molecular clouds. We describe an algorithm which can be used to constrain the values of (D, L, C) and apply this method to artificial and observed clusters. We show that this algorithm is able to reliably describe the three dimensional structure of an artificial star cluster from the two dimensional projection, and quantify the varied structures observed in real and simulated clusters.

show abstract

A possible sequential star formation in the giant molecular cloud G174+2.5

Cited by 34 publications

References 69 publications

Tracing the Galactic spiral structure with embedded clusters

Tracing the Galactic spiral structure with embedded clusters

Probing the anomalous extinction of four young star clusters: the use of colour-excess, main-sequence fitting and fractal analysis

$\mathcal {Q}^{+}$: characterizing the structure of young star clusters

Contact Info

Product

Resources

About