Rotation in young massive star clusters

Mapelli, Michela

doi:10.1093/mnras/stx304

Cited by 73 publications

(73 citation statements)

References 84 publications

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“…These investigations find evidence for a correlation between the rotation and mass of GCs, consistent with a scenario in which a forming globular cluster inherits angular momentum from its collapsing parent molecular cloud. Simulations of massive cluster formation agree with this picture, finding rotation in newborn clusters (e.g., Lee & Hennebelle 2016;Mapelli 2017). Direct dynamical evidence for rotation exists for a handful of young massive clusters (YMCs).…”

Section: Rotation Of the Sscmentioning

confidence: 61%

Ionized Gas Motions and the Structure of Feedback near a Forming Globular Cluster in NGC 5253

Cohen

Turner

Consiglio

et al. 2018

ApJ

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We observed Brackett α 4.05µm emission towards the supernebula in NGC 5253 with NIRSPEC on Keck II in adaptive optics mode, NIRSPAO, to probe feedback from its exciting embedded super star cluster (SSC). NIRSPEC's Slit-Viewing Camera was simultaneously used to image the K-band continuum at ∼0. ′′ 1 resolution. We register the IR continuum with HST imaging, and find that the visible clusters are offset from the K-band peak, which coincides with the Br α peak of the supernebula and its associated molecular cloud. The spectra of the supernebula exhibit Br α emission with a strong, narrow core. The linewidths are 65-76 km s −1 , FWHM, comparable to those around individual ultra-compact Hii regions within our Galaxy. A weak, broad (FWHM≃150-175 km s −1 ) component is detected on the base of the line, which could trace a population of sources with high-velocity winds. The core velocity of Br α emission shifts by +13 km s −1 from NE to SW across the supernebula, possibly indicating a bipolar outflow from an embedded object, or linked to a foreground redshifted gas filament. The results can be explained if the supernebula comprises thousands of ionized wind regions around individual massive stars, stalled in their expansion due to critical radiative cooling and unable to merge to drive a coherent cluster wind. Based on the absence of an outflow with large mass loss, we conclude that feedback is currently ineffective at dispersing gas, and the SSC retains enriched material out of which it may continue to form stars.

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Section: Rotation Of the Sscmentioning

confidence: 61%

Ionized Gas Motions and the Structure of Feedback near a Forming Globular Cluster in NGC 5253

Cohen

Turner

Consiglio

et al. 2018

ApJ

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“…gion G10.6-0.4 (e.g., Keto et al 1987;Liu et al 2012b), the L ∼10 5 L OB cluster-forming region G33.92+0.11 (e.g., Liu et al 2012aLiu et al , 2015, and the L ∼10 4 L OB cluster-forming region NGC6334 V (e.g., Juárez et al 2017). Is it plausible to form dense clusters of low-mass young stellar objects (YSOs) with a similar mechanism (c.f., Corsaro et al 2017;Mapelli 2017)?…”

Section: Introductionmentioning

confidence: 99%

Extreme fragmentation and complex kinematics at the center of the L1287 cloud

Juárez

Liu

Girart

et al. 2019

A&A

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Aims. The filamentary, ∼10 pc scale infrared dark cloud L1287 located at a ∼929 pc parallax distance, is actively forming a dense cluster of low-mass young stellar objects (YSOs) at its inner ∼0.1 pc region. To help understand the origin of this low-mass YSO cluster, the present work aims at resolving the gas structures and kinematics with high angular resolution. Methods. We have performed ∼1 angular resolution (∼930 AU) observations at ∼1.3 mm wavelengths using the Submillimeter Array (SMA), which simultaneously covered the dust continuum emission, and various molecular line tracers for dense gas, warm gas, shocks, and outflows. Results. From a ∼2 resolution 1.3 mm continuum image we identified six dense cores, namely SMA1-6. Their gas masses are in the range of ∼ 0.4 − 4 M . From a ∼1 resolution 1.3 mm continuum image, we find a high fragmentation level, with 14 compact millimeter sources within 0.1 pc: SMA3 contains at least nine internal condensations; SMA5 and SMA6 are also resolved with two internal condensations. Intriguingly, one condensation in SMA3, and one condensation in SMA5, appear associated with the known accretion outburst YSOs RNO 1C and RNO 1B. The dense gas tracer DCN (3-2) traces well the dust continuum emission and shows a clear velocity gradient along the NW-SE direction centered at SMA3. There is another velocity gradient with opposite direction around the most luminous young stellar object IRAS 00338+6312. Conclusions. The fragmentation within 0.1 pc in L1287 is very high compared to other regions at the same spatial scales. The incoherent motions of dense gas flows are sometimes interpreted by being influenced by (proto)stellar feedback (e.g., outflows), which is not yet ruled out in this particular target source. On the other hand, the velocities (with respect to the systemic velocity) traced by DCN are small, and the directions of the velocity gradients traced by DCN are approximately perpendicular to those of the dominant CO outflow(s). Therefore, we alternatively hypothesize that the velocity gradients revealed by DCN trace the convergence from the 0.1 pc scales infalling motion towards the rotational motions around the more compact (∼ 0.02 pc) sources. This global molecular gas converging flow may feed the formation of the dense low-mass YSO cluster. Finally, we also found that IRAS 00338+6312 is the most likely powering source of the dominant CO outflow. A compact blue-shifted outflow from RNO 1C is also identified.

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“…Second, from the theoretical point of view, it is of paramount importance to fill the gap between the highly complex end state predicted by numerical simulations of star formation in a clustered environment and the extremely simplified initial conditions that are usually adopted to study the subsequent long-term dynamical evolution of star clusters. In this respect, some recent hydrodynamical simulations of the formation of young massive star clusters have emphasised the importance of considering the kinematic dimension of protoclusters (e.g., see especially Hennebelle 2016 andMapelli 2017), also in view of the surprising morphological and kinematic richness that has emerged over the past few years in observational studies of young and intermediate age star clusters (e.g., see Hénault-Brunet et al 2012;Kuhn et al 2015;Vicente et al 2016).…”

Section: Introductionmentioning

confidence: 99%

The kinematic richness of star clusters – I. Isolated spherical models with primordial anisotropy

Breen

Varri

Heggie

2017

Monthly Notices of the Royal Astronomical Society

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We investigate the dynamical evolution of isolated equal-mass star cluster models by means of direct N-body simulations, primarily focusing on the effects of the presence of primordial anisotropy in the velocity space. We found evidence of the existence of a monotonic relationship between the moment of core collapse and the amount and flavour of anisotropy in the stellar system. Specifically, equilibria characterised by the same initial structural properties (Plummer density profile) and with different degrees of tangentially-biased (radially-biased) anisotropy, reach core collapse earlier (later) than isotropic models. We interpret this result in light of an accelerated (delayed) phase of the early evolution of collisional stellar systems ("anisotropic-response"), which we have characterised both in terms of the evolution of the velocity moments and of a fluid model of two-body relaxation. For the case of the most tangentially anisotropic model the initial phase of evolution involves a catastrophic collapse of the inner part of the system which continues until an isotropic velocity distribution is reached. This study represents a first step towards a comprehensive investigation of the role played by kinematic richness in the long-term dynamical evolution of collisional systems.

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Rotation in young massive star clusters

Cited by 73 publications

References 84 publications

Ionized Gas Motions and the Structure of Feedback near a Forming Globular Cluster in NGC 5253

Ionized Gas Motions and the Structure of Feedback near a Forming Globular Cluster in NGC 5253

Extreme fragmentation and complex kinematics at the center of the L1287 cloud

The kinematic richness of star clusters – I. Isolated spherical models with primordial anisotropy

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