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Journal articles on the topic 'Galaxy formation clusters'

Author: Grafiati

Published: 11 March 2023

Last updated: 31 July 2025

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1

Larson, Richard B. "Galaxy Formation and Cluster Formation." Symposium - International Astronomical Union 126 (1988): 311–21. http://dx.doi.org/10.1017/s007418090004256x.

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A primary motivation for studying globular clusters is that, as the oldest known galactic fossils, they trace the earliest stages of galactic evolution; indeed, they may hold the key to understanding galaxy formation. Thus it is clearly of great importance to learn how to read the fossil record. To do this, we need to understand something about how the globular clusters themselves formed. Were they the first bound objects to form, or did they form in larger pre-existing systems of which they are just small surviving fragments? If the latter, what were the prehistoric cluster-forming systems li

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Robertson, Andrew. "The galaxy–galaxy strong lensing cross-sections of simulated ΛCDM galaxy clusters". Monthly Notices of the Royal Astronomical Society: Letters 504, № 1 (2021): L7—L11. http://dx.doi.org/10.1093/mnrasl/slab028.

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ABSTRACT We investigate a recent claim that observed galaxy clusters produce an order of magnitude more galaxy–galaxy strong lensing (GGSL) than simulated clusters in a Λ cold dark matter (CDM) cosmology. We take galaxy clusters from the c-eagle hydrodynamical simulations and calculate the expected amount of GGSL for sources placed behind the clusters at different redshifts. The probability of a source lensed by one of the most massive c-eagle clusters being multiply imaged by an individual cluster member is in good agreement with that inferred for observed clusters. We show that numerically c

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Blau, Steven K. "Galaxy clusters in formation." Physics Today 68, no. 6 (2015): 20. http://dx.doi.org/10.1063/pt.3.2807.

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Kravtsov, Andrey V., and Stefano Borgani. "Formation of Galaxy Clusters." Annual Review of Astronomy and Astrophysics 50, no. 1 (2012): 353–409. http://dx.doi.org/10.1146/annurev-astro-081811-125502.

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Neumayer, Nadine. "Nuclear Star Clusters." Proceedings of the International Astronomical Union 12, S316 (2015): 84–90. http://dx.doi.org/10.1017/s1743921316007018.

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AbstractThe centers of galaxies host two distinct, compact components: massive black holes and nuclear star clusters. Nuclear star clusters are the densest stellar systems in the universe, with masses of ~ 107M⊙and sizes of ~ 5pc. They are almost ubiquitous at the centres of nearby galaxies with masses similar to, or lower than the Milky Way. Their occurrence both in spirals and dwarf elliptical galaxies appears to be a strong function of total galaxy light or mass. Nucleation fractions are up to 100% for total galaxy magnitudes of MB= −19mag or total galaxy luminosities of about LB= 1010L⊙and

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van den Bergh, S. "Star clusters in the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 161–64. http://dx.doi.org/10.1017/s0074180900200259.

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Star clusters in the Magellanic Clouds (MCs) differ from those in the Galaxy in a number of respects: (1) the Clouds contain a class of populous open clusters that has no Galactic counterpart; (2) Cloud clusters have systematically larger radii rh than those in the Galaxy; (3) clusters of all ages in the Clouds are, on average, more flattened than those in the Galaxy. In the Large Magellanic Cloud (LMC) there appear to have been two distinct epochs of cluster formation. LMC globulars have ages of 12-15 Gyr, whereas most populous open clusters have ages <5 Gyr. No such dichotomy is observed

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Anders, Peter, Uta Fritze –. v. Alvensleben, and Richard de Grijs. "Young Star Clusters: Progenitors of Globular Clusters!?" Highlights of Astronomy 13 (2005): 366–68. http://dx.doi.org/10.1017/s1539299600015987.

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AbstractStar cluster formation is a major mode of star formation in the extreme conditions of interacting galaxies and violent starbursts. Young clusters are observed to form in a variety of such galaxies, a substantial number resembling the progenitors of globular clusters in mass and size, but with significantly enhanced metallicity. From studies of the metal-poor and metal-rich star cluster populations of galaxies, we can therefore learn about the violent star formation history of these galaxies, and eventually about galaxy formation and evolution. We present a new set of evolutionary synth

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Henriksen, Mark J., and Prajwal Panda. "Exploiting Machine Learning and Disequilibrium in Galaxy Clusters to Obtain a Mass Profile." Astrophysical Journal Letters 961, no. 2 (2024): L36. http://dx.doi.org/10.3847/2041-8213/ad1ede.

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Abstract We use 3D k-means clustering to characterize galaxy substructure in the A2146 cluster of galaxies (z = 0.2343). This method objectively characterizes the cluster’s substructure using projected position and velocity data for 67 galaxies within a 2.305 Mpc circular region centered on the cluster's optical center. The optimal number of substructures is found to be four. Four distinct substructures with rms velocity typical of galaxy groups or low-mass subclusters, when compared to cosmological simulations of galaxy cluster formation, suggest that A2146 is in the early stages of formation

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Lee, Seong-Kook, Myungshin Im, Eunhee Ko, et al. "Star-formation Property of High Redshift Galaxies in Clusters: Perceptive View from Observation and Simulation." Proceedings of the International Astronomical Union 17, S373 (2021): 260–63. http://dx.doi.org/10.1017/s1743921322004409.

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AbstractThe evolution of star formation properties of galaxies depends on the environment where galaxies reside, and generally star formation of galaxies in dense environment decreases more quickly. Interestingly, the star formation property of high-redshift galaxies clusters vary largely even though they are at similar redshift. We have found that the large-scale environment surrounding each galaxy cluster can contribute to make this cluster-by-cluster variation. This correlation is found in the results from observational data as well as in the simulations of galaxy formation. We suggest the

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Danieli, Shany, Pieter van Dokkum, Sebastian Trujillo-Gomez, et al. "NGC 5846-UDG1: A Galaxy Formed Mostly by Star Formation in Massive, Extremely Dense Clumps of Gas." Astrophysical Journal Letters 927, no. 2 (2022): L28. http://dx.doi.org/10.3847/2041-8213/ac590a.

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Abstract It has been shown that ultra-diffuse galaxies (UDGs) have higher specific frequencies of globular clusters, on average, than other dwarf galaxies with similar luminosities. The UDG NGC 5846-UDG1 is among the most extreme examples of globular cluster–rich galaxies found so far. Here we present new Hubble Space Telescope observations and analysis of this galaxy and its globular cluster system. We find that NGC 5846-UDG1 hosts 54 ± 9 globular clusters, three to four times more than any previously known galaxy with a similar luminosity and higher than reported in previous studies. With a

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Ko 고, Eunhee 은희, Myungshin Im, Seong-Kook Lee, and Clotilde Laigle. "Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field." Astrophysical Journal 976, no. 2 (2024): 154. http://dx.doi.org/10.3847/1538-4357/ad86c2.

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Abstract It is yet to be understood how large-scale environments influence star formation activity in galaxy clusters. One recently proposed mechanism is that galaxy clusters can remain star forming when fed by infalling groups and star-forming galaxies from large-scale structures (LSSs) surrounding them (the “web-feeding” model). Using the COSMOS2020 catalog that has half a million galaxies with high-accuracy (σ Δz/1+z ∼ 0.01) photometric redshifts, we study the relationship between star formation activities in galaxy clusters and their surrounding environment to test the web-feeding model. W

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Benavides, José A., Laura V. Sales, and Mario G. Abadi. "Accretion of galaxy groups into galaxy clusters." Monthly Notices of the Royal Astronomical Society 498, no. 3 (2020): 3852–62. http://dx.doi.org/10.1093/mnras/staa2636.

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ABSTRACT We study the role of group infall in the assembly and dynamics of galaxy clusters in ΛCDM. We select 10 clusters with virial mass M200 ∼ 1014 $\rm M_\odot$ from the cosmological hydrodynamical simulation Illustris and follow their galaxies with stellar mass M⋆ ≥ 1.5 × 108 $\rm M_\odot$. A median of ${\sim}38{{\ \rm per\ cent}}$ of surviving galaxies at z = 0 is accreted as part of groups and did not infall directly from the field, albeit with significant cluster-to-cluster scatter. The evolution of these galaxy associations is quick, with observational signatures of their common origi

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Elbaz, D. "Infrared Observations of Galaxy Clusters." Highlights of Astronomy 11, no. 2 (1998): 1128–30. http://dx.doi.org/10.1017/s1539299600019754.

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The evolution of galaxy clusters from their formation due to the merging of sub structures, the bulk of star formation and subsequent chemical enrichment of the intra-cluster medium, is expected to be quite recent (z<l-2) in the hierarchical clustering scenario (White & Frenk 1991).

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Lindholmer, Mikkel O., and Kevin A. Pimbblet. "Redshift measurement through star formation." Astronomy & Astrophysics 629 (August 23, 2019): A7. http://dx.doi.org/10.1051/0004-6361/201833046.

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In this work we use the property that, on average, star formation rate increases with redshift for objects with the same mass – the so called galaxy main sequence – to measure the redshift of galaxy clusters. We use the fact that the general galaxy population forms both a quenched and a star-forming sequence, and we locate these ridges in the SFR–M⋆ plane with galaxies taken from the Sloan Digital Sky Survey in discrete redshift bins. We fitted the evolution of the galaxy main sequence with redshift using a new method and then subsequently apply our method to a suite of X-ray selected galaxy c

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Hwang, Narae, and Myung Gyoon Lee. "Tracing star cluster formation in the interacting galaxy M51." Proceedings of the International Astronomical Union 5, S266 (2009): 423–26. http://dx.doi.org/10.1017/s1743921309991591.

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AbstractWe present a study of star clusters in the interacting galaxy M51 using a star cluster catalog that includes about 3600 star clusters with mF555W < 23 mag, compiled by Hwang & Lee (2008). Combined with mF336W-band imaging data taken with the Hubble Space Telescope (HST)'s WFPC2 camera, we have derived the ages and masses of star clusters in M51 using theoretical population synthesis models. The cluster age distribution displays multiple peaks that correspond to the epochs of dynamical encounters predicted by theoretical model studies and the cluster-formation rate appears to inc

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Gouin, C., N. Aghanim, V. Bonjean, and M. Douspis. "Probing the azimuthal environment of galaxies around clusters." Astronomy & Astrophysics 635 (March 2020): A195. http://dx.doi.org/10.1051/0004-6361/201937218.

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Galaxy clusters are connected at their peripheries to the large-scale structures by cosmic filaments that funnel accreting material. These filamentary structures are studied to investigate both environment-driven galaxy evolution and structure formation and evolution. In the present work, we probe in a statistical manner the azimuthal distribution of galaxies around clusters as a function of the cluster-centric distance, cluster richness, and star-forming or passive galaxy activity. We performed a harmonic decomposition in large photometric galaxy catalogue around 6400 SDSS clusters with masse

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Lee, Seong-Kook, Myungshin Im, Minhee Hyun, et al. "More connected, more active: galaxy clusters and groups at z ∼ 1 and the connection between their quiescent galaxy fractions and large-scale environments." Monthly Notices of the Royal Astronomical Society 490, no. 1 (2019): 135–55. http://dx.doi.org/10.1093/mnras/stz2564.

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ABSTRACT High-redshift galaxy clusters, unlike local counterparts, show diverse star formation activities. However, it is still unclear what keeps some of the high-redshift clusters active in star formation. To address this issue, we performed a multiobject spectroscopic observation of 226 high-redshift (0.8 < z < 1.3) galaxies in galaxy cluster candidates and the areas surrounding them. Our spectroscopic observation reveals six to eight clusters/groups at z ∼ 0.9 and z ∼ 1.3. The redshift measurements demonstrate the reliability of our photometric redshift measurements, which in turn gi

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Li, Yuexing, Mordecai-Mark Mac Low, and Ralf S. Klessen. "Globular Cluster Formation in Galaxy Mergers." Highlights of Astronomy 13 (2005): 205. http://dx.doi.org/10.1017/s1539299600015719.

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AbstractWe present preliminary results of a high resolution simulation of globular cluster formation in a galaxy merger using GADGET (Springel et al. 2001). A barotropic equation of state (Li et al 2003) is implemented to include effects of cooling and heating. After one orbital period, a dozen proto-globular clusters are identified in the tidal tails.

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Chun, Kyungwon, Jihye Shin, Rory Smith, Jongwan Ko, and Jaewon Yoo. "The Formation of the Brightest Cluster Galaxy and Intracluster Light in Cosmological N-body Simulations with the Galaxy Replacement Technique." Astrophysical Journal 943, no. 2 (2023): 148. http://dx.doi.org/10.3847/1538-4357/aca890.

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Abstract We investigate the formation channels of the intracluster light (ICL) and the brightest cluster galaxy (BCG) in clusters at z = 0. For this, we perform multi-resolution cosmological N-body simulations using the “galaxy replacement technique.” We study the formation channels of the ICL and BCG as a function of distance from the cluster center and the dynamical state of the clusters at z = 0. To do this, we trace back the stars of the ICL and BCG, and identify the stellar components in which they existed when they first fell into the clusters. We find that the progenitors of the ICL and

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Gnedin, Oleg Y. "Modeling Formation of Globular Clusters: Beacons of Galactic Star Formation." Proceedings of the International Astronomical Union 6, S270 (2010): 381–84. http://dx.doi.org/10.1017/s1743921311000676.

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AbstractModern hydrodynamic simulations of galaxy formation are able to predict accurately the rates and locations of the assembly of giant molecular clouds in early galaxies. These clouds could host star clusters with the masses and sizes of real globular clusters. I describe current state-of-the-art simulations aimed at understanding the origin of the cluster mass function and metallicity distribution. Metallicity bimodality of globular cluster systems appears to be a natural outcome of hierarchical formation and gradually declining fraction of cold gas in galaxies. Globular cluster formatio

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Arnaboldi, Magda, and Ortwin Gerhard. "JD2 - Diffuse Light in Galaxy Clusters." Proceedings of the International Astronomical Union 5, H15 (2009): 97–110. http://dx.doi.org/10.1017/s174392131000846x.

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AbstractDiffuse intracluster light (ICL) has now been observed in nearby and in intermediate redshift clusters. Individual intracluster stars have been detected in the Virgo and Coma clusters and the first color-magnitude diagram and velocity measurements have been obtained. Recent studies show that the ICL contains of the order of 10% and perhaps up to 30% of the stellar mass in the cluster, but in the cores of some dense and rich clusters like Coma, the local ICL fraction can be high as 40%-50%. What can we learn from the ICL about the formation of galaxy clusters and the evolution of cluste

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Anders, Peter, Uta Fritze-V. Alvensleben, and Richard de Grijs. "Young Star Clusters: Clues to Galaxy Formation and Evolution." Symposium - International Astronomical Union 217 (2004): 210–11. http://dx.doi.org/10.1017/s0074180900197529.

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Young clusters are observed to form in a variety of interacting galaxies and violent starbursts, a substantial number resembling the progenitors of the well-studied globular clusters in mass and size. By studying young clusters in merger remnants and peculiar galaxies, we can therefore learn about the violent star formation history of these galaxies. We present a new set of evolutionary synthesis models of our GALEV code specifically developed to include the gaseous emission of presently forming star clusters, and a new tool that allows to determine individual cluster metallicities, ages, exti

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Fujita, Yutaka, Keiichi Umetsu, Elena Rasia, et al. "The new fundamental plane dictating galaxy cluster evolution." Proceedings of the International Astronomical Union 15, S341 (2019): 271–72. http://dx.doi.org/10.1017/s1743921319001376.

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AbstractIn this study, we show that the characteristic radius rs, mass Ms, and the X-ray temperature, TX, of galaxy clusters form a thin plane in the space of (log rs, log Ms, log TX). This tight correlation indicates that the cluster structure including the temperature is affected by the formation time of individual clusters. Numerical simulations show that clusters move along the fundamental plane as they evolve. The plane and the cluster evolution within the plane can be explained by a similarity solution of structure formation. The angle of the plane shows that clusters have not achieved “

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Wen, Z. L., J. L. Han, and Z. S. Yuan. "A catalogue of merging clusters of galaxies: cluster partners, merging subclusters, and post-collision clusters." Monthly Notices of the Royal Astronomical Society 532, no. 2 (2024): 1849–86. http://dx.doi.org/10.1093/mnras/stae1614.

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ABSTRACT Clusters of galaxies are merging during the formation of large-scale structures in the Universe. Based on optical survey data, we identify a large sample of pre-mergers of galaxy clusters and merging subclusters in rich clusters. We find 39 382 partners within a velocity difference of 1500 km s$^{-1}$ and a projected separation of 5 $r_{500}$ around 33 126 main clusters, where $r_{500}$ is the radius of the main cluster. Based on the galaxy distribution inside rich clusters with more than 30 member galaxy candidates, we identify subclusters by modelling the smoothed optical distributi

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Zepf, Stephen E. "Formation Scenarios for Globular Clusters and Their Host Galaxies." Symposium - International Astronomical Union 207 (2002): 653–63. http://dx.doi.org/10.1017/s0074180900224492.

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This review focuses on how galaxies and their globular cluster systems form. I first discuss the now fairly convincing evidence that some globular clusters form in galaxy starbursts/mergers. One way these observations are valuable is they place important constraints on the physics of the formation of globular clusters. Moreover, it is natural to associate the typically metal-rich clusters forming in mergers with the substantial metal-rich population of globulars around ellipticals, thereby implying an important role for galaxy mergers in the evolution of elliptical galaxies. I also highlight s

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Rieder, Steven, Clare Dobbs, Thomas Bending, Kong You Liow, and James Wurster. "The formation and early evolution of embedded star clusters in spiral galaxies." Monthly Notices of the Royal Astronomical Society 509, no. 4 (2021): 6155–68. http://dx.doi.org/10.1093/mnras/stab3425.

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ABSTRACT We present Ekster, a new method for simulating star clusters from birth in a live galaxy simulation that combines the smoothed-particle hydrodynamics (SPH) method Phantom with the N-body method PeTar. With Ekster, it becomes possible to simulate individual stars in a simulation with only moderately high resolution for the gas, allowing us to study whole sections of a galaxy rather than be restricted to individual clouds. We use this method to simulate star and star cluster formation in spiral arms, investigating massive giant molecular clouds (GMCs) and spiral arm regions with lower m

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Zepf, Stephen E. "The Formation and Evolution of Star Clusters and Galaxies." Highlights of Astronomy 13 (2005): 347–49. http://dx.doi.org/10.1017/s1539299600015938.

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AbstractThis paper addresses the questions of what we have learned about how and when dense star clusters form, and what studies of star clusters have revealed about galaxy formation and evolution. One important observation is that globular clusters are observed to form in galaxy mergers and starbursts in the local universe, which both provides constraints on models of globular cluster formation, and suggests that similar physical conditions existed when most early-type galaxies and their globular clusters formed in the past. A second important observation is that globular cluster systems typi

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Hashimoto, Tetsuya, Tomotsugu Goto, Rieko Momose, et al. "A young galaxy cluster in the old Universe." Monthly Notices of the Royal Astronomical Society 489, no. 2 (2019): 2014–29. http://dx.doi.org/10.1093/mnras/stz2182.

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ABSTRACT Galaxies evolve from a blue star-forming phase into a red quiescent one by quenching their star formation activity. In high-density environments, this galaxy evolution proceeds earlier and more efficiently. Therefore, local galaxy clusters are dominated by well-evolved red elliptical galaxies. The fraction of blue galaxies in clusters monotonically declines with decreasing redshift, i.e. the Butcher–Oemler effect. In the local Universe, observed blue fractions of massive clusters are as small as ≲0.2. Here we report a discovery of a ‘blue cluster’ that is a local galaxy cluster with a

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Brodie, Jean P., and Jay Strader. "Extragalactic Globular Clusters and Galaxy Formation." Annual Review of Astronomy and Astrophysics 44, no. 1 (2006): 193–267. http://dx.doi.org/10.1146/annurev.astro.44.051905.092441.

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Laganá, T. F., G. B. Lima Neto, F. Andrade-Santos, and E. S. Cypriano. "Star formation efficiency in galaxy clusters." Astronomy & Astrophysics 485, no. 3 (2008): 633–44. http://dx.doi.org/10.1051/0004-6361:20079168.

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Cohn, J. D., and Martin White. "The formation histories of galaxy clusters." Astroparticle Physics 24, no. 4-5 (2005): 316–33. http://dx.doi.org/10.1016/j.astropartphys.2005.07.006.

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Khosroshahi, Habib G., and T. J. Ponman. "Fossil Galaxy Groups; Scaling Relations, Galaxy Properties and Formation of BCGs." Proceedings of the International Astronomical Union 2, S235 (2006): 214. http://dx.doi.org/10.1017/s174392130600620x.

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AbstractWe study fossil galaxy groups, their hot gas and the galaxy properties. Fossils are more X-ray luminous than non-fossil groups, however, they fall comfortably on the conventional L-T relation of galaxy groups and clusters indicating that their X-ray luminosity and temperature are both boosted, arguably, as a result of their early formation. The central dominant galaxy in fossils have optical luminosity comparable to the brightest cluster galaxies (BCGs), however, the isophotal shapes of the central galaxy in fossils are non-boxy in contrast to the isophotes of majority of the BCGs.

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Brodie, Jean P. "Constraints on Galaxy Formation from Extragalactic Globular Clusters." Symposium - International Astronomical Union 187 (2002): 175–84. http://dx.doi.org/10.1017/s0074180900113907.

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The merger model for elliptical galaxy formation has received increasing attention since it was first suggested by Toomre & Toomre (1972). Van den Bergh (1984) pointed out a problem with the idea that elliptical galaxies were formed by simply combining two, or more, spiral galaxies. He noted that the specific frequency (SN, number of globular clusters per unit galaxy light) is systematically lower for spirals than for ellipticals. Schweizer (1987) suggested that globular clusters might be expected to form in the merger process, thereby alleviating or possibly eliminating the SN problem. As

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Elmegreen, Bruce G. "Triggering the Formation of Young Clusters." Symposium - International Astronomical Union 207 (2002): 390–400. http://dx.doi.org/10.1017/s0074180900224108.

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Star formation is triggered in essentially three ways: (1) the pressures from existing stars collect and squeeze nearby dense gas into gravitationally unstable configurations, (2) random compression from supersonic turbulence makes new clouds and clumps, some of which are gravitationally unstable, and (3) gravitational instabilities in large parts of a galaxy disk make giant new clouds and spiral arms that fragment by the other two processes into a hierarchy of smaller star-forming pieces. Examples of each process are given. Most dense clusters in the solar neighborhood were triggered by exter

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Mowla, Lamiya, Kartheik Iyer, Yoshihisa Asada, et al. "Formation of a low-mass galaxy from star clusters in a 600-million-year-old Universe." Nature 636, no. 8042 (2024): 332–36. https://doi.org/10.1038/s41586-024-08293-0.

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AbstractThe most distant galaxies detected were seen when the Universe was a scant 5% of its current age. At these times, progenitors of galaxies such as the Milky Way were about 10,000 times less massive. Using the James Webb Space Telescope (JWST) combined with magnification from gravitational lensing, these low-mass galaxies can not only be detected but also be studied in detail. Here we present JWST observations of a strongly lensed galaxy at zspec = 8.296 ± 0.001, showing massive star clusters (the Firefly Sparkle) cocooned in a diffuse arc in the Canadian Unbiased Cluster Survey (CANUCS)

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Kissler-Patig, Markus. "Metal-rich and Metal-poor Globular Clusters in Ellipticals: Did we Learn Anything? or Constraints on Galaxy Formation and Evolution from Globular Cluster Sub-populations." Symposium - International Astronomical Union 207 (2002): 207–17. http://dx.doi.org/10.1017/s0074180900223760.

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A brief review on globular cluster sub-populations in galaxies, and their constraints on galaxy formation and evolution is given. The metal-poor and metal-rich sub-populations are put in a historical context, and their properties, as known to date, are summarized. We review why the study of these sub-populations is extremely useful for the study of galaxy formation and evolution, but highlight a few caveats with the current interpretations. We re-visit the current globular cluster system formation scenarios and show how they boil down to a single scenario for the metal-poor clusters (namely th

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Hattori, M. "A Metal Enriched Dark Cluster of Galaxies at Z = 1." Symposium - International Astronomical Union 187 (2002): 129–38. http://dx.doi.org/10.1017/s0074180900113841.

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Looking for and studying very distant galaxy clusters, clusters at z > 1, are one of the prime subjects of the modern observational cosmology. If the metallicity of the hot intra-cluster medium in very distant galaxy clusters is measured for example, it provides fruitful informations for us to understand the formation and evolution of galaxies. However, difficulty of the study is that there is few confirmed very distant galaxy clusters yet. We first have to search for very distant clusters but it requires very deep observations. A random selection of sky is not practical. We have to select

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Tian, Da-Chuan, Yang Yang, Zhong-Lue Wen, and Jun-Qing Xia. "COSMIC: A Galaxy Cluster–Finding Algorithm Using Machine Learning." Astrophysical Journal Supplement Series 276, no. 1 (2025): 21. https://doi.org/10.3847/1538-4365/ad8bbd.

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Abstract Building a comprehensive catalog of galaxy clusters is a fundamental task for studies on structure formation and galaxy evolution. In this paper, we present Cluster Optical Search using Machine Intelligence in Catalogs (COSMIC), an algorithm utilizing machine learning techniques to efficiently detect galaxy clusters. COSMIC involves two steps, the identification of the brightest cluster galaxies and the estimation of cluster richness. We train our models on galaxy data from the Sloan Digital Sky Survey and the WHL galaxy cluster catalog. Validated against test data in the region of th

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Abdullah, Mohamed H., Raouf H. Mabrouk, Tomoaki Ishiyama, et al. "Quantifying the Velocity Anisotropy Profile of Galaxy Clusters Using the Uchuu Cosmological Simulation." Astrophysical Journal 987, no. 1 (2025): 70. https://doi.org/10.3847/1538-4357/adde4b.

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Abstract Galaxy clusters are powerful laboratories for studying both cosmic structure formation and galaxy evolution. We present a comprehensive analysis of the velocity anisotropy profile, β(r), in galaxy clusters using the Uchuu-UniverseMachine mock galaxy catalog, which combines the large-volume Uchuu N-body simulation with the UniverseMachine galaxy formation model. Focusing on clusters with log M 200 ≥ 13.9 [ h − 1 M ⊙ ] up to redshift z = 1.5, we investigate the behavior of β(r) as a function of clustercentric radius, mass, and redshift. We find that β(r) exhibits a universal shape: it r

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Anders, Peter, Uta Fritze –. v. Alvensleben, and Richard de Grijs. "Young Star Clusters: Metallicity Tracers in External Galaxies." Highlights of Astronomy 13 (2005): 667–69. http://dx.doi.org/10.1017/s1539299600017354.

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AbstractStar cluster formation is a major mode of star formation in the extreme conditions of interacting galaxies and violent star bursts. These newly-formed clusters are built from recycled gas, pre-enriched to various levels within the interacting galaxies. Hence, star clusters of different ages represent a fossil record of the chemical enrichment history of their host galaxy, as well as of the host galaxy’s violent star formation history. We present a new set of evolutionary synthesis models of our GALEV code, specifically developed to include the gaseous emission of presently forming star

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Fujita, Yutaka, Megan Donahue, Stefano Ettori, et al. "Halo Concentrations and the Fundamental Plane of Galaxy Clusters." Galaxies 7, no. 1 (2019): 8. http://dx.doi.org/10.3390/galaxies7010008.

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According to the standard cold dark matter (CDM) cosmology, the structure of dark halos including those of galaxy clusters reflects their mass accretion history. Older clusters tend to be more concentrated than younger clusters. Their structure, represented by the characteristic radius r s and mass M s of the Navarro–Frenk–White (NFW) density profile, is related to their formation time. In this study, we showed that r s , M s , and the X-ray temperature of the intracluster medium (ICM), T X , form a thin plane in the space of ( log r s , log M s , log T X ) . This tight correlation indicates t

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Fahrion, K., M. Lyubenova, G. van de Ven, et al. "Diversity of nuclear star cluster formation mechanisms revealed by their star formation histories." Astronomy & Astrophysics 650 (June 2021): A137. http://dx.doi.org/10.1051/0004-6361/202140644.

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Nuclear star clusters (NSCs) are the densest stellar systems in the Universe and are found in the centres of all types of galaxies. They are thought to form via mergers of star clusters such as ancient globular clusters (GCs) that spiral to the centre as a result of dynamical friction or through in situ star formation directly at the galaxy centre. There is evidence that both paths occur, but the relative contribution of either channel and their correlation with galaxy properties are not yet constrained observationally. Our aim was to derive the dominant NSC formation channel for a sample of 2

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Barger, A. J., A. Aragón-Salamanca, R. S. Ellis, W. J. Couch, I. Smail, and R. M. Sharples. "Starburst Cycle in Distant Clusters." Symposium - International Astronomical Union 171 (1996): 341. http://dx.doi.org/10.1017/s0074180900232609.

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A major puzzle in observational cosmology is the physical origin of a significant excess population of blue galaxies in the cores of distant rich galaxy clusters. This ‘Butcher-Oemler’ effect is now known to be a widespread starburst-related phenomenon. We test whether various spectral and photometrically-defined galaxy classes might represent different stages within a single cycle of star-formation. We compare the numbers of galaxies in various categories for three z = 0.31 clusters, AC103, AC114, and AC118, with evolutionary models generated according to the Bruzual & Chariot (1993) isoc

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McKinney, Jed, Vandana Ramakrishnan, Kyoung-Soo Lee, et al. "Measuring the Total Ultraviolet Light from Galaxy Clusters at z = 0.5–1.6: The Balance of Obscured and Unobscured Star Formation." Astrophysical Journal 928, no. 1 (2022): 88. http://dx.doi.org/10.3847/1538-4357/ac5110.

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Abstract Combined observations from UV to IR wavelengths are necessary to fully account for the star formation in galaxy clusters. Low-mass galaxies with log ( M ∗ / M ⊙ ) < 10 are typically not individually detected, particularly at higher redshifts (z ∼ 1–2) where galaxy clusters are undergoing rapid transitions from hosting mostly active, dust-obscured star-forming galaxies to hosting quiescent, passive galaxies. To account for these undetected galaxies, we measure the total light emerging from GALEX/near-UV stacks of galaxy clusters at z = 0.5–1.6. Combined with existing measurements fr

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Kroupa, Pavel. "Star-cluster formation and evolution." Proceedings of the International Astronomical Union 2, S237 (2006): 230–37. http://dx.doi.org/10.1017/s1743921307001524.

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AbstractStar clusters are observed to form in a highly compact state and with low star-formation efficiencies, and only 10 per cent of all clusters appear to survive to middle- and old-dynamical age. If the residual gas is expelled on a dynamical time the clusters disrupt. Massive clusters may then feed a hot kinematical stellar component into their host-galaxy's field population thereby thickening galactic disks, a process that theories of galaxy formation and evolution need to accommodate. If the gas-evacuation time-scale depends on cluster mass, then a power-law embedded-cluster mass functi

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Bahk, Hyeonguk, and Ho Seong Hwang. "UPCluster-SZ: The Updated Catalog of Galaxy Clusters from the List of Planck Sunyaev–Zel’dovich Sources." Astrophysical Journal Supplement Series 272, no. 1 (2024): 7. http://dx.doi.org/10.3847/1538-4365/ad323f.

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Abstract We present the updated galaxy cluster catalog of the second Planck catalog of Sunyaev–Zel’dovich sources (PSZ2) through the compilation of the data for clusters and galaxies with spectroscopically measured redshifts in the literature. The original version of PSZ2 comprises 1653 Sunyaev–Zel’dovich (SZ) sources, of which 1203 have been validated as genuine galaxy clusters, while the remaining 450 sources are yet to be validated. To increase the number of genuine clusters in PSZ2, we first update the validations of the cluster candidates and their redshift information using the data comp

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Durret, Florence, Christophe Adami, and Tatiana F. Laganá. "Environmental Effects on Galaxy Luminosity Functions in Clusters." Proceedings of the International Astronomical Union 6, S277 (2010): 9–12. http://dx.doi.org/10.1017/s1743921311022356.

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AbstractThe formation and evolution of galaxies is strongly influenced by environment, particularly in clusters, where galaxy luminosity functions vary in shape with the dynamical state of the cluster (relaxed or in various stages of merging), with the photometric band considered and with the position in the cluster. We present here results concerning the optical GLFs in several relaxed and merging clusters.

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Strazzullo, V., M. Pannella, J. J. Mohr, et al. "Galaxy populations in the most distant SPT-SZ clusters." Astronomy & Astrophysics 622 (February 2019): A117. http://dx.doi.org/10.1051/0004-6361/201833944.

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We present the first results from a galaxy population study in the highest redshift galaxy clusters identified in the 2500 deg2 South Pole Telescope Sunyaev Zel’dovich effect (SPT-SZ) survey, which is sensitive to M500 ≳ 3 × 1014 M⊙ clusters from z ∼ 0.2 out to the highest redshifts where such massive structures exist. The cluster selection is to first order independent of galaxy properties, making the SPT-SZ sample particularly well suited for cluster galaxy population studies. We carried out a four-band imaging campaign with the Hubble and Spitzer Space Telescopes of the five z ≳ 1.4, S/NSZE

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de los Rios, Martín, Héctor J. Martínez, Valeria Coenda, et al. "ROGER: Reconstructing orbits of galaxies in extreme regions using machine learning techniques." Monthly Notices of the Royal Astronomical Society 500, no. 2 (2020): 1784–94. http://dx.doi.org/10.1093/mnras/staa3339.

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ABSTRACT We present the ROGER (Reconstructing Orbits of Galaxies in Extreme Regions) code, which uses three different machine learning techniques to classify galaxies in, and around, clusters, according to their projected phase-space position. We use a sample of 34 massive, M200 &gt; 1015h−1M⊙, galaxy clusters in the MultiDark Planck 2 (MDLP2) simulation at redshift zero. We select all galaxies with stellar mass M⋆ ≥ 108.5h−1M⊙, as computed by the semi-analytic model of galaxy formation SAG, that are located in, and in the vicinity of, these clusters and classify them according to their or

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Rieder, Steven, Clare Dobbs, Thomas Bending, Kong You Liow, and James Wurster. "Simulating star formation in spiral galaxies." Proceedings of the International Astronomical Union 16, S362 (2020): 105–10. http://dx.doi.org/10.1017/s1743921322001892.

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AbstractWe present Ekster, a new method for simulating the formation and dynamics of individual stars in a relatively low-resolution gas background. Here, we use Ekster to simulate star cluster formation in two different regions from each of two galaxy models with different spiral potentials. We simulate these regions for 3 Myr to study where and how star clusters form. We find that massive GMC regions form more massive clusters than sections of spiral arms. Additionally we find that clusters form both by accreting gas and by merging with other proto-clusters, the latter happening more frequen

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