Star Clusters(성단)란 무엇입니까?
Star Clusters 성단 - Membership of stars in open clusters is one of the most crucial parameters in studies of star clusters. [1] As self-consistent structures, such idealized systems can serve as heuristic models for DML, astronomical systems, such as dwarf spheroidal galaxies, low-surface-density elliptical galaxies and star clusters, and diffuse galaxy groups. [2] Most stars are formed as star clusters in galaxies, which then disperse into galactic disks. [3] Lastly, as a practical example in the astrophysical study, we show that this method can determine the main-sequence ridge line precisely in the color-magnitude diagram of star clusters. [4] Direct N-body simulations of star clusters are accurate but expensive, largely due to the numerous (N2) pairwise force calculations. [5] Many discoveries have been carried out at BAO related to stars, star clusters and other systems, nebulae, galaxies and systems of galaxies. [6] Here we investigate the process of particle acceleration at the termination shock that develops in the bubble excavated by star clusters' winds in the interstellar medium. [7] RVs are not only used to detect and characterize exoplanets, but also play a key role in studies of binary stars, star clusters, and moving group member identification. [8] We present a search for “hypercompact” star clusters in the Milky Way using a combination of Gaia and the Dark Energy Camera Legacy Survey (DECaLS). [9] Some of them show embedded stellar substructures, such as star clusters and even globular star clusters. [10] Despite these caveats, the quality of Gaia astrometry has been significantly improved in EDR3 and provides valuable insights into the properties of star clusters. [11]산개 성단의 별 구성원은 성단 연구에서 가장 중요한 매개 변수 중 하나입니다. [1] 이러한 이상화된 시스템은 일관된 구조로서 DML, 왜소 회전 타원체 은하, 표면 밀도가 낮은 타원 은하 및 성단, 확산 은하 그룹과 같은 천문 시스템에 대한 발견적 모델 역할을 할 수 있습니다. [2] 대부분의 별은 은하에서 성단으로 형성되어 은하 원반으로 흩어집니다. [3] 마지막으로 천체 물리학 연구의 실제 사례로 이 방법이 성단의 색등급도에서 주계열 능선을 정확하게 결정할 수 있음을 보여줍니다. [4] 성단의 직접 N체 시뮬레이션은 정확하지만 많은 (N2) 쌍별 힘 계산으로 인해 비용이 많이 듭니다. [5] BAO에서는 별, 성단 및 기타 시스템, 성운, 은하 및 은하계와 관련된 많은 발견이 수행되었습니다. [6] 여기에서 우리는 성간 매질에서 성단의 바람에 의해 굴착된 거품에서 발생하는 종단 충격에서 입자 가속 과정을 조사합니다. [7] RV는 외행성을 탐지하고 특성화하는 데 사용될 뿐만 아니라 쌍성, 성단 및 움직이는 그룹 구성원 식별 연구에서도 중요한 역할을 합니다. [8] 우리는 Gaia와 DECaLS(Dark Energy Camera Legacy Survey)의 조합을 사용하여 우리은하에서 "초소형" 성단에 대한 검색을 제시합니다. [9] 그들 중 일부는 성단과 구상 성단과 같은 내장된 항성 하부 구조를 보여줍니다. [10] 이러한 경고에도 불구하고 Gaia 천문학의 품질은 EDR3에서 크게 향상되었으며 성단의 속성에 대한 귀중한 통찰력을 제공합니다. [11]
Nuclear Star Clusters 핵성단
Only environments with escape speed $\gtrsim 100$ km s$^{-1}$, as found in galactic nuclear star clusters as well as in the most massive globular clusters and super star clusters, could efficiently retain the merger remnants of the LIGO/Virgo BBH population even for low progenitor spins ($\chi_{\rm max}=0. [1] A Bayesian analysis using the χeff, χp, and mchirp distributions suggests that 1g BHs have the maximum mass of ∼15–$30\, {\rm M}_\odot$ if the majority of mergers are of high-generation BHs (not among 1g–1g BHs), which is consistent with mergers in active galactic nucleus discs and/or nuclear star clusters, while if mergers mainly originate from globular clusters, 1g BHs are favoured to have non-zero spin magnitudes of ∼0. [2] Thereafter, the binary orbit shrinks rapidly due to the high central stellar densities furnished by nuclear star clusters (NSCs). [3] We study Population III (Pop III) binary remnant mergers in nuclear star clusters (NSCs) with a semi-analytical approach for early structure formation. [4] A possible formation channel of these SMSs is the interplay of gas accretion and runaway stellar collisions inside dense nuclear star clusters (NSCs). [5] We explore hierarchical black hole (BH) mergers in nuclear star clusters (NSCs), globular clusters (GCs) and young star clusters (YSCs), accounting for both original and dynamically assembled binary BHs (BBHs). [6] Promising locations for efficient production of hierarchical mergers include nuclear star clusters and accretion disks surrounding active galactic nuclei, though environments that are less efficient at retaining merger products such as globular clusters may still contribute significantly to the detectable population of repeated mergers. [7] Nuclear star clusters (NSCs) are the densest stellar systems in the Universe and are found in the centres of all types of galaxies. [8] Here, we present a fast semi-analytic approach to simulate hierarchical mergers in nuclear star clusters (NSCs), globular clusters (GCs) and young star clusters (YSCs). [9] We focus our analysis on the balance between ordered rotation and random motions, which can provide insights into the dominant formation mechanism of nuclear star clusters (NSCs). [10] We also explore whether MOND allows GC systems of isolated UDGs to survive without sinking into nuclear star clusters. [11] We use deep high resolution HST/ACS imaging of two fields in the core of the Coma cluster to investigate the occurrence of nuclear star clusters (NSCs) in quiescent dwarf galaxies as faint as MI = −10 mag. [12] Nuclear star clusters in AGNs are a plausible formation site of compact-stellar binaries (CSBs) whose coalescences can be detected through gravitational waves (GWs). [13] Nuclear star clusters (NSCs) are a common phenomenon in galaxy centres and are found in a vast majority of galaxies of intermediate stellar mass $\approx 10^9\, \mathrm{M}_{\odot }$. [14] The orbital decay of a perturber within a larger system plays a key role in the dynamics of many astrophysical systems—from nuclear star clusters or globular clusters in galaxies, to massive black holes in galactic nuclei, to dwarf galaxy satellites within the dark matter halos of more massive galaxies. [15] When gravitational waves pass through the nuclear star clusters of galactic lenses, they may be microlensed by the stars. [16] These kick velocities suggest that globular clusters and nuclear star clusters may retain up to and of their remnant black holes, respectively, while young star clusters would only retain a few tenths of a percent. [17] Stars may form in gravitationally unstable regions of these disks, or may be captured from nuclear star clusters. [18] Nuclear Star Clusters (NSCs) are dense clusters of stars that reside in the centers of a majority of the galaxies. [19] Nuclear star clusters are found at the centers of most galaxies. [20] This is larger than the escape speeds of most globular clusters, requiring denser and heavier environments such as nuclear star clusters or disks-assisted migration in galactic nuclei. [21] The infall may produce episodic star formation in the centre, building up nuclear star clusters simultaneously with the growth of the central black hole. [22]은하핵성단은 물론 가장 거대한 구상성단과 초성단에서 발견되는 탈출 속도가 $\gtrsim 100$ km s$^{-1}$인 환경만이 LIGO의 병합 잔해를 효율적으로 유지할 수 있습니다. 낮은 전구 스핀에도 /Virgo BBH 개체수($\chi_{\rm max}=0. [1] χeff, χp 및 mchirp 분포를 사용한 베이지안 분석에 따르면 1g BH의 최대 질량은 ~15–$30\, 합병의 대부분이 세대 BH(다음 중 아님)인 경우 {\rm M}_\odot$ 1g-1g BHs)은 활성은하핵 원반 및/또는 핵성단의 병합과 일치하는 반면, 병합이 주로 구상성단에서 발생하는 경우 1g BH는 ~0의 0이 아닌 스핀 크기를 갖는 것이 좋습니다. [2] 그 후, 쌍성 궤도는 핵성단(NSC)이 제공하는 높은 중심 별 밀도로 인해 빠르게 축소됩니다. [3] nan [4] nan [5] nan [6] nan [7] nan [8] nan [9] nan [10] nan [11] nan [12] nan [13] nan [14] nan [15] nan [16] nan [17] nan [18] nan [19] nan [20] nan [21] nan [22]
Young Star Clusters 젊은 성단
The color–magnitude diagrams of young star clusters show that, particularly at ultraviolet wavelengths, their upper main sequences (MSs) bifurcate into a sequence comprising the bulk population and a blue periphery. [1] Here, we investigate the possibility that IMBHs form in young star clusters via runaway collisions and BH mergers. [2] Recent studies indicate that the progenitors of merging black hole (BH) binaries from young star clusters can undergo a common envelope phase just like isolated binaries. [3] Young star clusters are dynamically active stellar systems and are a common birthplace for massive stars. [4] The analysis of the MUSE dataset, which provides a map of the ionised gas and a census of Wolf Rayet stars, is complemented with a sample of young star clusters (YSCs) and O star candidates observed with the Hubble Space Telescope (HST) and of giant molecular clouds traced in CO(2-1) emission with the Atacama Large Millimeter/submillimeter Array (ALMA). [5] Given distinct uncertainties in detailed binary evolution calculations, we investigate a rigorous and model independent upper limit for the production of Be stars through binary interaction and aim to confront this limit with observations of Be stars in young star clusters. [6] A pioneering study showed that the fine structure in the luminosity function (LF) of young star clusters contains information about the evolutionary stage (age) and composition of the stellar population. [7] We measure the projected half-light radii of young star clusters in 31 galaxies from the Legacy Extragalactic UV Survey (LEGUS). [8] An analysis of the spatial separation between young star clusters and nearby H ii regions has made it possible to determine the position of the corotation radius in the galaxies studied. [9] We use the angular two-point correlation function (TPCF) to investigate the hierarchical distribution of young star clusters in 12 local (3–18 Mpc) star-forming galaxies using star cluster catalogs obtained with the Hubble Space Telescope (HST) as part of the Treasury Program Legacy ExtraGalactic UV Survey. [10] To this effect, we make use of state-of-the-art population synthesis and N-body simulations, to represent two distinct formation channels: BBHs formed in the field (isolated channel) and in young star clusters (dynamical channel). [11] We test claims that the power-law mass functions of young star clusters (ages $<\mbox{few}\times10^8~$yr) have physical upper cutoffs at $M_*\sim10^5~M_{\odot}$. [12] Here, we investigate the demography of merging BBHs in young star clusters (SCs), which are the nursery of massive stars. [13] Extended γ\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\gamma $$\end{document}-ray emissions in the vicinity of young star clusters are believed to be produced by the interaction of CRs accelerated therein with the ambient gas. [14] We present the first UV integrated-light spectroscopic observations for 15 young star clusters in the starburst M83 with a special focus on metallicity measurements. [15]젊은 성단의 색-등급 도표는 특히 자외선 파장에서 상위 주계열(MS)이 벌크 개체군과 청색 주변부를 포함하는 계열로 분기됨을 보여줍니다. [1] 여기에서 우리는 폭주 충돌과 BH 합병을 통해 젊은 성단에서 IMBH가 형성될 가능성을 조사합니다. [2] 최근 연구에 따르면 젊은 성단에서 생성된 결합 블랙홀(BH) 쌍성의 조상은 고립된 쌍성처럼 공통의 외피 단계를 거칠 수 있습니다. [3] 젊은 성단은 역동적으로 활동하는 항성계이며 무거운 별의 일반적인 발상지입니다. [4] 이온화된 가스 지도와 Wolf Rayet 별의 인구 조사를 제공하는 MUSE 데이터 세트의 분석은 허블 우주 망원경(HST)으로 관찰된 젊은 성단(YSC) 및 O성 후보 샘플로 보완됩니다. ALMA(Atacama Large Millimeter/submillimeter Array)로 CO(2-1) 방출을 추적하는 거대 분자 구름. [5] 상세한 쌍성 진화 계산의 뚜렷한 불확실성을 감안할 때, 우리는 쌍성 상호 작용을 통해 Be 별 생성에 대한 엄격하고 모델 독립적인 상한을 조사하고 젊은 성단에서 Be 별을 관찰하여 이 한계에 맞서는 것을 목표로 합니다. [6] nan [7] nan [8] nan [9] nan [10] nan [11] nan [12] nan [13] nan [14] nan [15]
Dense Star Clusters 조밀한 성단
Most of the low-surface density, CO-emitting gas will disperse without forming stars but some of the high-density gas will probably collapse and form dense star clusters, such as the luminous HII region close to UGC 12915. [1] On the other hand, dense star clusters, such as the Orion Nebula Cluster (ONC), have experienced rapid dynamical relaxation, and have lost the memory of the initial turbulent kinematics. [2] An important application is stellar collisions, which occur commonly in dense star clusters, and their relevance for the formation of various types of stellar exotica. [3] In all the simulations, dense star clusters form before the collisions occur, and we find that star formation remains confined to these systems and is little affected by the collisions. [4] In dense star clusters, such as globular and open clusters, dynamical interactions between stars and black holes (BHs) can be extremely frequent, leading to various astrophysical transients. [5] In part I we discuss a new formation channel of compact binaries: tidal encounters with a massive BH at galactic centres or potentially in dense star clusters. [6] The BH binaries that consist of second-generation BHs can also be assembled in dense star clusters through binary interactions. [7] When binary black holes merge in dense star clusters, their remnants can pair up with other black holes in the cluster, forming heavier and heavier black holes in a process called hierarchical merger. [8] Black holes formed in dense star clusters, where dynamical interactions are frequent, may have fundamentally different properties than those formed through isolated stellar evolution. [9] Merging BH–NS binaries are expected to form mainly through the evolution of massive binary stars in the field, since their dynamical formation in dense star clusters is strongly suppressed by mass segregation. [10] 6×109M⊙ FDM halo with mb=8×10−23eV in isolation, we demonstrate that the wobbling, oscillating soliton gravitationally perturbs nuclear objects, such as supermassive black holes or dense star clusters, causing them to diffuse outwards. [11] Using a grid of 96 dynamical models of dense star clusters and a cosmological model of cluster formation, we explore the production of binary black hole mergers where at least one component of the binary was forged in a previous merger. [12] Our results provide evidence that, for computationally challenging regions of phase-space, a trained ANN can replace existing numerical solvers, enabling fast and scalable simulations of many-body systems to shed light on outstanding phenomena such as the formation of black-hole binary systems or the origin of the core collapse in dense star clusters. [13]낮은 표면 밀도의 CO 방출 가스의 대부분은 별을 형성하지 않고 분산되지만 고밀도 가스의 일부는 아마도 붕괴되어 UGC 12915에 가까운 빛나는 HII 영역과 같은 조밀한 성단을 형성할 것입니다. [1] 반면에 오리온 성운(ONC)과 같은 조밀한 성단은 빠른 역학 이완을 경험했고 초기의 난류 운동학에 대한 기억을 잃었습니다. [2] 중요한 응용은 조밀한 성단에서 일반적으로 발생하는 항성 충돌과 다양한 유형의 이국적인 항성 형성에 대한 관련성입니다. [3] 모든 시뮬레이션에서 충돌이 일어나기 전에 빽빽한 성단이 형성되며, 우리는 별 형성이 이러한 시스템에 국한되어 있고 충돌의 영향을 거의 받지 않는다는 것을 발견했습니다. [4] 구상 성단과 산개 성단과 같은 조밀한 성단에서는 별과 블랙홀(BH) 간의 동적 상호 작용이 매우 빈번하여 다양한 천체 물리학적 과도 현상이 발생할 수 있습니다. [5] nan [6] nan [7] nan [8] nan [9] nan [10] nan [11] nan [12] nan [13]
Massive Star Clusters 거대한 성단
Massive star clusters (MSCs) have recently received renewed attention as possible cosmic ray (CR) factories. [1] Here, we investigate the formation of GW190521-like systems via three-body encounters in young massive star clusters. [2] G1, also known as Mayall II, is one of the most massive star clusters in M31. [3] Analyzing the dynamical state of nearby young massive star clusters is essential for understanding star cluster formation and evolution during their earliest stages. [4] massive star clusters) as well as simulations where diffuse emission is important. [5] , their first pass) and discover a spectacular ∼10 kpc long string of young massive star clusters (t ≲ 10 Myr; M ⋆ ≳ 105 M ⊙) between the galaxies triggered by the interaction. [6] In our model, the mechanical feedback from massive star clusters evolving within high-density pre-enriched media allows to pile-up a large amount of matter into massive supershells. [7] The results of RT instability are significantly affected by the variation of radiation pressure in dense magnetized nonuniform plasmas and have relevance for understanding dense astrophysical environments, such as massive star clusters and white dwarfs. [8] By performing three-dimensional radiation hydrodynamics simulations, we study the formation of young massive star clusters (YMCs, M* > 104 M⊙) in clouds with the surface density ranging from Σcl = 80 to 3200 M⊙ pc−2. [9] This is a natural outcome of galaxies with higher star-formation rates producing more massive star clusters, spawning a larger number of SNIa progenitors per star. [10] These models suggest that dual or multiple populations can emerge rapidly in massive star clusters undergoing the typical mode of star cluster formation. [11] 8 pc), and have substantially more scatter in their sizes than in situ metal-rich GCs in the Milky Way and young massive star clusters forming in M83 (〈Reff〉 ≃ 2. [12]거대 성단(MSC)은 최근 우주선(CR) 공장 가능성으로 다시 주목받고 있다. [1] 여기에서 우리는 젊고 무거운 성단에서 3체 조우를 통해 GW190521과 같은 시스템의 형성을 조사합니다. [2] Mayall II라고도 알려진 G1은 M31에서 가장 무거운 성단 중 하나입니다. [3] 가까운 젊은 무거운 성단의 역학 상태를 분석하는 것은 초기 단계의 성단 형성과 진화를 이해하는 데 필수적입니다. [4] 거대한 성단) 뿐만 아니라 확산 방출이 중요한 시뮬레이션. [5] nan [6] nan [7] nan [8] nan [9] nan [10] nan [11] nan [12]
Open Star Clusters 열린 성단
We have carried out a search for massive white dwarfs (WDs) in the direction of young open star clusters using the Gaia DR2 database. [1] The monograph poses issues related to the study of the non-stationarity of open star clusters (OSCs), starting with an analysis of the properties of the trajectories of individual stars to the study of collective motion of stars. [2] We present a first derivation of the semiempirical IFMR for hydrogen-deficient (non-DA) white dwarfs in open star clusters. [3] In this study were discussed the LAMOST catalog opportunities in the statistical studies of the spectra of stars in open star clusters (OSC). [4] Open star clusters (OCs) are stellar systems that originated under the same astrophysical environments, at the same distance, with identical ages, original chemical compositions, and various masses. [5] We investigate some aspects of Galactic disc kinematics based on the data on open clusters from the current version of “The Homogeneous Catalog of the Main Parameters of Open Star Clusters” and from Gaia DR2. [6] Binary white dwarfs in open star clusters are particularly useful because cluster parameters such as distance, metal content, and total system age are more tightly constrained than for field double degenerates. [7]우리는 Gaia DR2 데이터베이스를 사용하여 젊은 산개성단 방향으로 거대한 백색왜성(WD)에 대한 검색을 수행했습니다. [1] 이 논문은 개별 별의 궤적 특성 분석을 시작으로 별의 집합적 운동 연구에 이르기까지 산개성단(OSC)의 비정상성 연구와 관련된 문제를 제기합니다. [2] nan [3] nan [4] nan [5] nan [6] nan [7]
Super Star Clusters 슈퍼 스타 클러스터
He 2–10 is also one of the first galaxies in which embedded super star clusters (SSCs) were discovered. [1] Young massive clusters and super star clusters (SSCs) represent an extreme mode of star formation. [2] 8\times10^8$ L$_\odot$ is typical of proto-Super Star Clusters (proto-SSC) observed in the SB galaxy NGC 253. [3] Mechanical feedback from young massive stars in super star clusters contributes to the formation of superwinds and superbubbles in star-forming regions. [4] The recombination line emission primarily originates from a population of approximately a dozen embedded super star clusters in the early stages of formation. [5] The metal-poor galaxy ESO 338-4 has experienced vigorous starburst during the last 40 Myr and contains some of the most massive super star clusters in the nearby Universe. [6] Some of them have inferred sizes of less than 40 pc for stellar masses between 106 and 107M⊙, comparable to individual super star clusters or star cluster complexes at low redshift. [7]He 2–10은 또한 내장된 슈퍼 스타 클러스터(SSC)가 발견된 최초의 은하 중 하나입니다. [1] 젊은 거대 성단과 초성단(SSC)은 극단적인 별 형성 방식을 나타냅니다. [2] nan [3] nan [4] nan [5] nan [6] nan [7]
Globular Star Clusters 구상성단
The clusters have characteristics close to those of typical globular star clusters. [1] Finding IMBHs in globular star clusters (GCs) would validate a formation channel for massive black-hole seeds in the early universe. [2] The thus constrained stellar IMF then accounts for the observed trend of metallicity and M/L ratio found amongst M31 globular star clusters. [3] Till now, 157 globular star clusters (GSCs) were revealed in the Galaxy, and there is a large bank of observation data for them, which have been collected for a long time (see, e. [4]성단은 전형적인 구상성단과 유사한 특성을 갖고 있다. [1] 구상성단(GC)에서 IMBH를 찾는 것은 초기 우주에서 거대한 블랙홀 씨앗의 형성 채널을 검증할 것입니다. [2] nan [3] nan [4]
Bound Star Clusters 묶인 성단
Understanding the formation of bound star clusters with low star-formation efficiency is very important to know about the star-formation history of galaxies. [1] 6, respectively, with the faintest or most magnified ones probing possible single gravitationally bound star clusters. [2] We report the formation of bound star clusters in a sample of high-resolution cosmological zoom-in simulations of z>5 galaxies from the FIRE project. [3]별 형성 효율이 낮은 묶인 성단의 형성을 이해하는 것은 은하의 별 형성 역사를 아는 데 매우 중요합니다. [1] 각각 6개에서 가장 희미하거나 가장 확대된 별들이 단일 중력으로 묶인 성단을 조사하고 있다. [2] nan [3]
Fmy Star Clusters
The effectiveness of the method is verified with the low-resolution stellar spectra of ELODIE, SDSS (Sloan Digital Sky Survey), LAMOST (Large Sky Area Multi-Object Fibre Spectroscopic Telescope), and four star clusters. [1] Only four star clusters are known within ~100 pc of Earth. [2]New Star Clusters 새로운 성단
We apply bayesian algorithms to studying the effects of binary stellar population models on the age determination of 46 new star clusters in Gaia DR2. [1] Recently, a noticeable number of new star clusters was identified in the outskirts of the Large Magellanic Cloud (LMC) populating the so-called star-cluster age gap, a space of time (∼4–12 Gyr) where the only known star cluster is up-to-date ESO 121-SC 03. [2]우리는 가이아 DR2에 있는 46개의 새로운 성단의 나이 결정에 대한 쌍성 항성 인구 모델의 영향을 연구하기 위해 베이지안 알고리즘을 적용합니다. [1] 최근에, 유일하게 알려진 성단이 존재하는 시공간(~4–12 Gyr)인 소위 성단 연령 차이를 채우고 있는 대마젤란운(LMC) 외곽에서 눈에 띄게 많은 수의 새로운 성단이 확인되었습니다. 최신 ESO 121-SC 03입니다. [2]
Known Star Clusters 알려진 성단
If this scenario could be confirmed, then the cluster would be significantly fainter and more compact than most of the known star clusters residing in the extreme outskirts of the Galactic halo, but quite similar to Laevens 3. [1] There are more than two dozen known star clusters in its line of sight, but it is not clear which ones are physically associated with CMa OB1. [2]이 시나리오가 확인될 수 있다면 그 성단은 은하 후광의 극단에 있는 알려진 대부분의 성단보다 훨씬 더 희미하고 더 조밀할 것이지만 Laevens 3와 매우 유사합니다. [1] 그 시야에는 24개 이상의 알려진 성단이 있지만 어떤 것이 CMa OB1과 물리적으로 연관되어 있는지는 분명하지 않습니다. [2]
star clusters form 성단 형태
In all the simulations, dense star clusters form before the collisions occur, and we find that star formation remains confined to these systems and is little affected by the collisions. [1] Star clusters form via clustering star formation inside molecular clouds. [2]모든 시뮬레이션에서 충돌이 일어나기 전에 빽빽한 성단이 형성되며, 우리는 별 형성이 이러한 시스템에 국한되어 있고 충돌의 영향을 거의 받지 않는다는 것을 발견했습니다. [1] 성단은 분자 구름 내부의 성단 형성을 통해 형성됩니다. [2]