The structure of star clusters. I. an empirical density law

King, Ivan R.

doi:10.1086/108756

Cited by 1,871 publications

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“…Bonatto & Bica 2007a, and references therein). Structural parameters are derived by fitting Kinglike profiles to the clusters RDPs (King 1962). This procedure was applied in previous works (e.g., , 2011bLima et al 2014, and references therein).…”

Section: Methods Of Analysismentioning

confidence: 99%

Tracing the Galactic spiral structure with embedded clusters

Camargo

Bonatto

Bica

2015

Monthly Notices of the Royal Astronomical Society

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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.

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Section: Methods Of Analysismentioning

confidence: 99%

Tracing the Galactic spiral structure with embedded clusters

Camargo

Bonatto

Bica

2015

Monthly Notices of the Royal Astronomical Society

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“…Assuming a King profile, the GC mass satisfies the relation (King 1962) . colour map of the t df at varying M GC and r GC .…”

Section: Dynamical Friction and Tidal Disruptionmentioning

confidence: 99%

The MEGaN project – I. Missing formation of massive nuclear clusters and tidal disruption events by star clusters–massive black hole interactions

Sedda

Capuzzo-Dolcetta

2017

Monthly Notices of the Royal Astronomical Society

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We investigated the evolution of a massive galactic nucleus hosting a super-massive black hole (SMBH) with mass M SMBH = 10 8 M ⊙ surrounded by a population of 42 heavy star clusters (GCs). Using direct N -body modelling, we show here that the assembly of an NSC through GCs orbital decay and merger is efficiently inhibited by the tidal forces exerted from the SMBH. The GCs mass loss induced by tidal forces causes a significant modification of their mass function, leading to a population of low-mass (< 10 4 ) clusters. Nonetheless, the GCs debris accumulated around the SMBH give rise to well-defined kinematical and morphological properties, leading to the formation of a disk-like structure. Interestingly, the disk is similar to the one observed in the M31 galaxy nucleus, which has properties similar to our numerical model. The simulation produced a huge amount of data, which we used to investigate whether the GC debris deposited around the SMBH can enhance the rate of tidal disruption events (TDEs) in our galaxy inner density distribution. Our results suggest that the GCs disruption shapes the SMBH neighbourhoods leading to a TDE rate of ∼ 2 × 10 −4 yr −1 , a value slightly larger than what expected in previous theoretical modelling of galaxies with similar density profiles and central SMBHs. The simulation presented here is the first of its kind, representing a massive galactic nucleus and its star cluster population on scales ∼ 100 pc.

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“…King-profile fitting used the modified function σ(R) = σ bg + σ 0 /(1 + (R/R c ) 2 ), as introduced in King (1962). Figure 3 shows RDPs around the new center coordinates for the target clusters using the clean subsample.…”

Section: Radial Density Profilementioning

confidence: 99%

Membership probability via control-field colour–magnitude decontamination

Corradi¹,

Maia²,

Santos³

2009

Proc. IAU

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Abstract. The fundamental physical parameters of open clusters are important tools to understand the formation and evolution of the Galactic disk and to test star-formation and evolution models. However, only a small fraction of the known open clusters in the Milky Way have precise determinations of distance, reddening, age, metallicity, radial velocity and proper motion. One of the major problems in determining these parameters lies in the difficulty to separate cluster members from field stars and to assign membership. We propose a decontamination method by employing 2mass data in the regions around the clusters NGC 1981, NGC 2516, NGC 6494 and M11. We present decontaminated colour-magnitude diagrams of these objects showing the membership probabilities and structural parameters as derived from King-profile fitting.

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The structure of star clusters. I. an empirical density law

Cited by 1,871 publications

References 0 publications

Tracing the Galactic spiral structure with embedded clusters

Tracing the Galactic spiral structure with embedded clusters

The MEGaN project – I. Missing formation of massive nuclear clusters and tidal disruption events by star clusters–massive black hole interactions

Membership probability via control-field colour–magnitude decontamination

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