Young Cluster(年輕集群)到底是什麼？
Young Cluster 年輕集群 - This is the predicted cutoff from dynamical models in which old globular clusters and young clusters observed today formed by similar processes with similar initial mass functions. [1] At the time of its discovery, it was the first multi-planet system in a young cluster. [2] The distribution of size as a function of age observed for star clusters in the Large Magellanic Cloud (LMC) is very puzzling: young clusters are all compact, while the oldest systems show both small and large sizes. [3] The low surface brightness of the streams (typically >30 mag/arcsec$^2$), however, will make them difficult to detect, unless the streams originate from very young clusters. [4] However, the clustering strength of the most massive GMCs, supposedly the progenitors of the young clusters for a star formation efficiency of a few percent, is comparable (alpha = -0. [5] Our study not only reinforces the notion that some young clusters like NGC 1866 harbor multiple populations, but gives also hints that the first population, the older, may inherit the angular momentum from the parent cloud while stars of the second one, the younger, do not. [6] Extended main-sequence turn-offs (eMSTO) are a commonly observed property of young clusters. [7] All of the 655 cluster candidates have a well defined main-sequence except for two candidates if we consider that the main sequence of very young clusters is somewhat broad due to differential extinction. [8] We derive parameters such as age, distance modulus and extinction for a sample of 269 open clusters, selecting only low reddening objects and discarding very young clusters, for which techniques other than isochrone-fitting are more suitable for estimating ages. [9] Here we provide an overview of optical photometric observations of the young clusters, identification of variable nature from their light curves, characterization of their circumstellar disk. [10] These observations shed light on the frequency of the ejection events in young clusters. [11] Young clusters and associations hold clues to the origin and properties of multiple star systems. [12] This finding is important for understanding the physics of the MP phenomenon, as these young clusters can provide much stronger constraints (e. [13] We suggest that variable stars, binary interactions, and stellar rotation affect the eMSTO morphology of these very young clusters. [14] The Scutum complex in the inner disk of the Galaxy hosts a number of young clusters and associations of red supergiant stars that are heavily obscured by dust extinction. [15] We have undertaken a similar analysis for 61 B-type similar targets, towards the young cluster, NGC 346 in the Small Magellanic Cloud (SMC). [16] 1 Msun not associated with a young cluster. [17] It is shown that the shallow, power-law density profiles characteristic of young clusters is predicted by the hierarchical star formation scenario. [18] In this work we report the discovery of a young cluster of asteroids that originated by the breakup of an asteroid member of the (221)Eos family. [19] (abridged) NGC6530 is a young cluster with a complex morphology and star-formation history. [20] W40 is a blistered Hii region, and Serpens South is an infrared dark cloud accompanied by a young cluster. [21]這是動力學模型的預測截止值，其中今天觀察到的舊球狀星團和年輕星團是由具有相似初始質量函數的類似過程形成的。 [1] 在它被發現時，它是年輕星團中的第一個多行星系統。 [2] 在大麥哲倫星雲 (LMC) 中觀察到的星團的大小隨年齡的分佈非常令人費解：年輕的星團都是緊湊的，而最古老的系統則顯示出既小又大的尺寸。 [3] 然而，流的低表面亮度（通常 >30 mag/arcsec$^2$）將使它們難以被發現，除非流來自非常年輕的星團。 [4] 然而，最大質量的 GMC 的集群強度，據說是年輕星團的前身，恆星形成效率只有百分之幾，是相當的（α = -0. [5] 我們的研究不僅強化了一些年輕星團（如 NGC 1866）擁有多個群體的觀點，而且還暗示第一個群體（較老的群體）可能繼承母雲的角動量，而第二個群體（較年輕的星團）則可以不是。 [6] 擴展主序列關閉（eMSTO）是年輕集群的常見屬性。 [7] 如果我們認為非常年輕的星團的主序列由於不同的滅絕而有點寬泛，則所有 655 個候選星團都有一個明確定義的主序列，除了兩個候選星團。 [8] 我們為 269 個疏散星團樣本推導出年齡、距離模量和消光等參數，僅選擇低紅化對象並丟棄非常年輕的星團，對於這些參數，等時擬合以外的技術更適合估計年齡。 [9] 在這裡，我們概述了對年輕星團的光學光度觀測，從它們的光變曲線中識別可變性質，以及它們的環星盤的特徵。 [10] 這些觀察結果揭示了年輕星團中噴射事件的頻率。 [11] 年輕的星團和協會為多恆星系統的起源和性質提供了線索。 [12] 這一發現對於理解 MP 現象的物理學很重要，因為這些年輕的星團可以提供更強的約束（例如。 [13] 我們認為變星、雙星相互作用和恆星旋轉會影響這些非常年輕的星團的 eMSTO 形態。 [14] 銀河系內盤的盾牌複合體擁有許多年輕的星團和紅超巨星組合，這些星團被塵埃滅絕嚴重遮蔽。 [15] 我們針對小麥哲倫星雲 (SMC) 中的年輕星團 NGC 346 對 61 個 B 型類似目標進行了類似分析。 [16] 1 Msun 未與年輕集群關聯。 [17] 結果表明，年輕星團的淺冪律密度分佈特徵是由分層恆星形成情景預測的。 [18] 在這項工作中，我們報告了一個年輕的小行星集群的發現，該集群起源於 (221)Eos 家族的一個小行星成員的解體。 [19] （節略）NGC6530 是一個年輕的星團，具有復雜的形態和恆星形成歷史。 [20] W40 是一個起泡的 Hii 區域，Serpens South 是一個紅外暗雲，伴隨著一個年輕的星團。 [21]
Massive Young Cluster 大規模年輕集群
The very bright and compact massive young cluster, NGC 3603, has been cited as an example of a starburst in the Milky Way and compared with the much-studied R136/30 Doradus region in the Large Magellanic Cloud. [1] 5If* star RFS8 ($\sim$70 $M_{\odot}$), found within $\approx$ 53 and 58 pc respectively from the Galactic massive young cluster NGC 3603, using Gaia data. [2]非常明亮和緻密的大質量年輕星團 NGC 3603 被引用為銀河系中星暴的一個例子，並與大麥哲倫星雲中經過大量研究的 R136/30 劍魚座區域進行了比較。 [1] 5If* 星 RFS8 ($\sim$70 $M_{\odot}$)，使用 Gaia 數據，分別在距銀河系大質量年輕星團 NGC 3603 的 $\約 53 和 58 pc 範圍內發現。 [2]
Dynamically Young Cluster 動態年輕集群
Multiwavelength observations show that Abell 1367 (A1367) is a dynamically young cluster, with at least two subclusters merging along the SE–NW direction. [1] Multiwavelength observations show that Abell 1367 (A1367) is a dynamically young cluster, with at least two subclusters merging along the SE–NW direction. [2]多波長觀測表明 Abell 1367 (A1367) 是一個動態年輕的星團，至少有兩個子星團沿 SE-NW 方向合併。 [1] 多波長觀測表明 Abell 1367 (A1367) 是一個動態年輕的星團，至少有兩個子星團沿 SE-NW 方向合併。 [2]
young cluster ngc 年輕集群 Ngc
0 to several open clusters with different properties and environments to show the capabilities of the tool: an area of five degrees around NGC 2682 (M 67), an old, well known cluster; a young cluster NGC 2516 with a striking elongate structure extended up to four degrees; NGC 1750 & NGC 1758, a pair of partly overlapping clusters; in the area of NGC 1817 we confirm a little-known cluster, Juchert 23; and in an area with many clusters we disentangle the existence of two overlapping clusters where only one was previously known: Ruprecht 26 and the new, Clusterix 1. [1] We examine the mass-dependence of the velocity dispersion of stars in the young cluster NGC 6530 to better understand how it formed. [2] Spectroscopy for 247 stars towards the young cluster NGC 346 in the Small Magellanic Cloud has been combined with that for 116 targets from the VLT-FLAMES Survey of Massive Stars. [3] 5If* star RFS8 ($\sim$70 $M_{\odot}$), found within $\approx$ 53 and 58 pc respectively from the Galactic massive young cluster NGC 3603, using Gaia data. [4]0 到幾個具有不同屬性和環境的疏散星團，以展示該工具的功能：NGC 2682 (M 67) 周圍五度的區域，一個古老的、眾所周知的星團；一個年輕的星團 NGC 2516，具有驚人的細長結構，延伸至四度； NGC 1750 & NGC 1758，一對部分重疊的星團；在 NGC 1817 區域，我們確認了一個鮮為人知的星團 Juchert 23；在一個有許多星團的區域，我們解開了兩個重疊星團的存在，而以前只知道一個：Ruprecht 26 和新的 Clusterix 1。 [1] 我們研究了年輕星團 NGC 6530 中恆星速度色散的質量依賴性，以更好地了解它是如何形成的。 [2] 麥哲倫星雲中年輕星團 NGC 346 的 247 顆恆星的光譜與 VLT-FLAMES 大質量恆星巡天中的 116 個目標的光譜相結合。 [3] 5If* 星 RFS8 ($\sim$70 $M_{\odot}$)，使用 Gaia 數據，分別在距銀河系大質量年輕星團 NGC 3603 的 $\約 53 和 58 pc 範圍內發現。 [4]