Relevant bibliographies by topics / Galaxy Cluster Formation

Academic literature on the topic 'Galaxy Cluster Formation'

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Published: 6 September 2023

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Journal articles on the topic "Galaxy Cluster Formation"

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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 like? And how did they manage to produce objects like globular clusters?
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Lee, Seong-Kook, Myungshin Im, Eunhee Ko, Changbom Park, Juhan Kim, Jaehyun Lee, and Minhee Hyun. "Star-formation Property of High Redshift Galaxies in Clusters: Perceptive View from Observation and Simulation." Proceedings of the International Astronomical Union 17, S373 (August 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 ‘Web-feeding model’ to explain this trend. Star-forming galaxies falling into the galaxy cluster from surrounding large-scale structure make the quiescent galaxy fraction of the cluster lower than relatively isolated clusters.
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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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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 (September 2, 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 origin eroding rapidly in 1–3 Gyr after infall. Substructure plays a dominant role in fostering the conditions for galaxy mergers to happen, even within the cluster environment. Integrated over time, we identify (per cluster) an average of 17 ± 9 mergers that occur in infalling galaxy associations, of which 7 ± 3 occur well within the virial radius of their cluster hosts. The number of mergers shows large dispersion from cluster to cluster, with our most massive system having 42 mergers above our mass cut-off. These mergers, which are typically gas rich for dwarfs and a combination of gas rich and gas poor for M⋆ ∼ 1011 $\rm M_\odot$, may contribute significantly within ΛCDM to the formation of specific morphologies, such as lenticulars (S0) and blue compact dwarfs in groups and clusters.
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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 for clusters in the Small Magellanic Cloud (SMC) The fact that the SMC exhibits no enhanced cluster formation at times of bursts of cluster formation in the LMC, militates against encounters between the Clouds as a cause for enhanced rates of star and cluster formation.
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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, no. 1 (March 22, 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 converged results for the GGSL probability require higher resolution simulations than had been used previously. On top of this, different galaxy formation models predict cluster substructures with different central densities, such that the GGSL probabilities in ΛCDM cannot yet be robustly predicted. Overall, we find that GGSL within clusters is not currently in tension with the ΛCDM cosmological model.
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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 (August 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 increase around the same epochs.
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Danieli, Shany, Pieter van Dokkum, Sebastian Trujillo-Gomez, J. M. Diederik Kruijssen, Aaron J. Romanowsky, Scott Carlsten, Zili Shen, 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 (March 1, 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 galaxy luminosity of L V,gal ≈ 6 × 107 L ⊙ (M ⋆ ≈ 1.2 × 108 M ⊙) and a total globular cluster luminosity of L V,GCs ≈ 7.6 × 106 L ⊙, we find that the clusters currently comprise ∼13% of the total light. Taking into account the effects of mass loss from clusters during their formation and throughout their lifetime, we infer that most of the stars in the galaxy likely formed in globular clusters, and very little to no “normal” low-density star formation occurred. This result implies that the most extreme conditions during early galaxy formation promoted star formation in massive and dense clumps, in contrast to the dispersed star formation observed in galaxies today.
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Riccio, G., M. Paolillo, R. D’Abrusco, M. Cantiello, X. Jin, Z. Li, A. Venhola, et al. "Intra-cluster GC-LMXB in the Fornax galaxy cluster." Proceedings of the International Astronomical Union 14, S351 (May 2019): 151–54. http://dx.doi.org/10.1017/s1743921319007890.

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AbstractThe formation of Low mass X-ray binaries (LMXB) is favored within dense stellar systems such as Globular Clusters (GCs). The connection between LMXB and Globular Clusters has been extensively studied in the literature, but these studies have always been restricted to the innermost regions of galaxies. We present a study of LMXB in GCs within the central 1.5 deg2 of the Fornax cluster with the aim of confirming the existence of a population of LMXB in intra-cluster GCs and understand if their properties are related to the host GCs, to the environment or/and to different formation channels.
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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 synthesis models of our GALEV code, with special emphasis on the gaseous emission of presently forming star clusters, and a new tool to compare extensive model grids with multi-color broad-band observations to determine individual cluster masses, metallicities, ages and extinction values independently. First results for young star clusters in the dwarf starburst galaxy NGC 1569 are presented. The mass distributions determined for the young clusters give valuable input to dynamical star cluster system evolution models, regarding survival and destruction of clusters. We plan to investigate an age sequence of galaxy mergers to see dynamical destruction effects in process.
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Dissertations / Theses on the topic "Galaxy Cluster Formation"

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Strader, Jay. "Extragalactic globular cluster subpopulations and galaxy formation /." Diss., Digital Dissertations Database. Restricted to UC campuses, 2007. http://uclibs.org/PID/11984.

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Cho, Jaeil. "Globular cluster systems and their implications of galaxy formation." Thesis, Durham University, 2008. http://etheses.dur.ac.uk/2427/.

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In this thesis the spectroscopic and photometric results of the Galactic and extragalactic globular clusters are presented. And their implications on galaxy formation have been investigated. Integrated spectroscopy with a high resolution of 24 Galactic globular clusters were obtained using the Isacc Newton Telescope, from which 21 line indices were carefully measured and calibrated. By comparing with recent simple stellar population models (Thomas et al. 2003 and Lee & Worthey 2005), it is confirmed that Galactic globular clusters are old (~10- 12 Gyr). There is a discrepancy between the two models in low metallicity and the line indices measured have a better fit to Lee & Worthey (2005) model. These is a significant effect of blue horizontal branch stars on the Balmer absorption lines in integrated spectra, which could cause globular clusters to be underestimated their age. Shell in elliptical galaxies are probably signature of recent galaxy merger/interaction. Properties of globular cluster systems (GCSs) in six shell galaxies have been examined and whether this signature can be seen in GCSs have been investigated. The GCSs in shell galaxies are found not to differ noticeably from those in normal elliptical galaxies in the sense and blue subpopulations are consistent with previous studies. This result is contradictory to results by Sikkema et al. (2006), who have found possible young globular clusters in the two galaxies. Using the Advanced Camera for Survey on the Hubble Space telescope, 10 low density early-type galaxies were observed and properties of their GCSs have been investigated to constrain galaxy formation history depending on environments. By comparing results from the Virgo Cluster Survey as a high-density counterpart, both similarities and differences between the two density groups were found. General behaviour of colour distributions of GCSs found in cluster environment are also seen in those in field galaxies; mean colour gets redder as increasing with galaxy luminosity, less bimodal colour distributions are detected in lower galaxy luminosity, and there is a correlation between red colour peak and host galaxy luminosity. However, mean colours of GCS in low-density appear to be slightly bluer than those in high-density at a given galaxy luminosity, which implies that GCS in field environments is either less metal-rich or younger than those in cluster environments. More diverse shape of colour distributions are found in dense region than in low-density region, which would reflects more complicated galaxy formation history in dense region. In spite of finding environmental this effect on galaxy formation, this effect is so subtle that galaxy (final) mass is still a dominant factor to determine galaxy formation and stellar populations in there.
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Santoro, Fernando. "Semi analytical simulations of primordial star cluster formation." Thesis, University of Sussex, 2003. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.288843.

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Simanton, Lesley Ann. "Star Cluster Populations in the Spiral Galaxy M101." University of Toledo / OhioLINK, 2015. http://rave.ohiolink.edu/etdc/view?acc_num=toledo1437587267.

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Cai, Zheng. "Cosmic Structure Formation: From First Star to Large-scale Filamentary Structure." Diss., The University of Arizona, 2015. http://hdl.handle.net/10150/578387.

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Theory of cosmic structure formation outlines how stars, galaxies, clusters of galaxies, and large-scale structures formed out of primordial density fluctuations. It presents us a picture of cosmic mass assembly, and places strong constraints on cosmological model. Both observations and theories suggest that structures formation follows a "bottom up" process, in which small, low-mass component form first, and gradually develop into larger, more massive systems. This dissertation focuses on three crucial stages of cosmic structure formation: first generation stars, quasar host galaxies and the large-scale galaxy overdensities. In Chapter 1, I present an overview of structure formation, acquainting readers with a general picture from first object in the Universe to large-scale structures at later epochs. In Chapter 2 and Chapter 3, I derive strong constraints to the star formation rates (SFRs) of very massive Population III (Pop III) stars in two high redshift galaxies at z = 7. By probing the He II emission lines for both galaxies, I conclude that the contributions of very massive Pop III stars to total the SFRs are less than 3%. In Chapter 4, I move to more massive systems, quasar host galaxies at z ~ 3. Using damped Lyman alpha absorption systems as natural coronagraphs, I report that rest-frame far-UV emission of quasar host galaxy correlates strongly with quasar luminosity. This result suggests a co-evolution of supermassive black holes and their host galaxies. In Chapter 5, I develop a novel method for searching the most massive protoclusters at z = 2-3, by utilizing intergalactic Lyman alpha absorption. My investigations suggest that large intergalactic Lyman alpha absorption systems effectively trace the most overdense regions at large scale of ~ 15 h⁻¹ Mpc. In Chapter 6, I present our imaging observations of an extreme galaxy overdensity (protocluster) BOSS1441+4000, which is discovered using the techniques developed in Chapter 5. Furthermore, I report an intergalactic-scale Lyman alpha nebula detected at the density peak of BOSS1441+4000. This discovery, together with previously discovered Slug nebula, provide us a first look of intergalactic medium in emission in the early Universe. In the Chapter 7, I give a summary of this dissertation and discuss several future prospects.
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Rudick, Craig S. "The Formation and Evolution of Intracluster Light: Simulations and Observations." Case Western Reserve University School of Graduate Studies / OhioLINK, 2011. http://rave.ohiolink.edu/etdc/view?acc_num=case1282831433.

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Kriwattanawong, Wichean. "The formation and evolution of the galaxy population in the nearby cluster abell 1367." Thesis, Liverpool John Moores University, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.502762.

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Bai, Lei. "The Effects of Dense Cluster Environments on Galaxies and Intracluster Dust." Diss., The University of Arizona, 2007. http://hdl.handle.net/10150/193609.

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Dense cluster environment influences the properties of galaxies and their evolution. In order to understand this environmental effect and how it evolves with time, we study the infrared (IR) properties of galaxies in three rich clusters. The IR luminosities provide us with extinction-free measurements of the star formation rates (SFRs) of these cluster galaxies. We find a strong evolution in the IR luminosity function (LF) of two z ∼ 0:8 clusters when compared to two local clusters. The evolution rate of the IR LF found in these clusters is consistent with the evolution in field IR LFs. The similar evolution rate found in very different environments favors some internal mechanism, e.g., the gradual consumption of the gas fuel in galaxies, as being responsible for much of the star formation evolution. The mass-normalized integrated SFRs within 0.5R₂₀₀ of these clusters also shows an evolution trend, ∝ (1 + z)5. But this evolution has large scatter and may be affected by the mass selection effect of the sample. In the dense cluster core regions (r < 0.3 Mpc), we find evidence for enhanced SFR suppression. A substantial fraction of members in MS 1054-03 (z ∼ 0.8) are still forming stars actively. This cannot be explained by the scenario where the cluster is only passively accreting star-forming galaxies from the surrounding field, after which their star formation is quenched quickly. We also study the extended IR emission from the intracluster dust (ICD) in A2029. We only find weak signals at 24 and 70 μm and obtain upper limits for the ICD emission.
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Fensch, Jérémy. "Star and stellar cluster formation in gas-dominated galaxies." Thesis, Sorbonne Paris Cité, 2017. http://www.theses.fr/2017USPCC207/document.

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Nous étudions la formation d’étoiles et d’amas d’étoiles dans les galaxies dominées par le gaz. Ce terme réfère en premier lieu aux galaxies de l’époque du pic de formation d’étoiles dans l’histoire de l’Univers, qui s’est déroulé vers z ~ 2, mais aussi à leurs analogues locaux, les galaxies naines de marées. En premier lieu, en utilisant des simulations numériques, nous montrons que les galaxies massives typiques de z=2, avec une fraction de gaz d’environ 50%, forment des structures gazeuses massives (10**7-8 masses solaires) et liées gravitationnellement, appelées grumeaux dans la suite. Ces grumeaux ne se forment dans des galaxies avec une fraction de gaz inférieure à 25%. Nous présentons ensuite une étude observationnelle d’un analogue local de grumeaux de galaxies à z=2, la galaxie naine de marée NGC 5291N. Une analyse des raies d’émission de cette galaxie montre la présence de chocs sur les pourtours de l’objet. La photométrie des amas d’étoiles de cette galaxie montre que les amas les plus jeunes (< 10 millions d’années) sont significativement moins massifs que les amas plus âgés. Ceci peut être le signe de fusions progressives d’amas et/ou d’une forte activité de formation stellaire dans ce système il y a environ 500 millions d’années.Dans un second lieu nous étudions comment la fraction de gaz influe sur la formation d’étoiles et d’amas stellaires dans des fusions de galaxies à z=2. En utilisant des simulations numériques nous montrons que ces fusions n’augmentent que relativement peu le taux de formation d’étoiles et d’amas stellaires comparativement aux fusions de galaxies locales, à faible fraction de gaz. Nous montrons que ceci est due à une saturation de plusieurs facteurs physiques, qui sont déjà présents naturellement dans les galaxies isolées à z=2 et sont donc comparativement peu accentués par les fusions. Il s’agit de la turbulence du gaz, des zones de champ de marée compressif et des flux de matières vers le noyau de la galaxie. Nous montrons aussi que les structures stellaires formées au sein des grumeaux de gaz sont préservées par la fusion : elles sont éjectées des disques et orbitent dans le halo de la galaxie résultante de la fusion, où elles peuvent devenir les progéniteurs de certains amas globulaires
We study the formation of stars and stellar clusters in gas-dominated galaxies. This term primarily refers to galaxies from the epoch of the peak of the cosmic star formation history, which occurred at z ~ 2, but also to their local analogues, the tidal dwarf galaxies.Firstly, using numerical simulations, we show that the massive galaxies at z = 2, which have a gas fraction of about 50%, form massive (10**7-8 solar masses) and gravitationally bound structures, which we call clumps thereafter. These clumps do not form in galaxies with a gas fraction below 25%. We then present an observational study of a local analogue of a z = 2 galactic clump, which is the tidal dwarf galaxy NGC 5291N. The analysis of emission lines show the presence of shocks on the outskirts of the object. Photometry of this galaxy’s stellar clusters show that the youngest clusters (< 10 million years) are significantly less massive than older clusters. This could be the sign of ongoing cluster mergers and/or of a strong star formation activity in this system about 500 million years ago).Secondly, we study how the gas fraction impacts the formation of stars and stellar clusters in galaxy mergers at z = 2. Using numerical simulations we show that these mergers only slightly increase the star and stellar cluster formation rate, compared to local galaxy mergers, which have a lower gas fraction. We show that this is due to the saturation of several physical quantities, which are already strong in isolated z=2 galaxies and are thus less enhanced by the merger. These factors are gas turbulence, compressive tides and nuclear gas inflows, We also show that the stellar structures formed in the gaseous clumps are preserved by the fusion: they are ejected from the disk and orbit in the halo of the remnant galaxy, where they may become the progenitors of some globular clusters
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Fabjan, Dunja. "The effect of star formation and feedback on the X-ray properties of simulated galaxy clusters." Doctoral thesis, Università degli studi di Trieste, 2010. http://hdl.handle.net/10077/3434.

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2008/2009
The aim of this Thesis was to study the X--ray properties of the IntraCluster Medium (ICM) in a cosmological context resorting to high resolution hydrodynamical simulations. The thermodynamical and chemical properties of the ICM were inspected and studied within a set of galaxy clusters that were simulated with the TREE-SPH Gadget2 code (Springel 2005). This code included a detailed model of chemical evolution (Tornatore et al. 2007) as well as prescriptions for different physical processes: star formation, galactic winds and AGN feedback. We use this large set of simulated galaxy clusters with a twofold aim. First, we study the effect of different sources of feedback on the ICM observable properties, in particular on its metal enrichment and on thermo and chemo--dynamical properties when AGN feedback is at work. Second, we test the robustness of cluster mass proxies against the different physical processes included in the simulations. When exploring the effect on metal enrichment and its evolution we found that among different prescriptions for the stellar Initial Mass Function (IMF), the best results on Iron abundance profiles and global Iron evolution are found when applying the Salpeter IMF (Salpeter 1955). We also found that the positive evolution of the metal abundance in the central regions of simulated clusters can not be simply interpreted as a consequence of an excess of low--redshift star formation. Instead the evolution of the metallicity pattern is driven by the combined action of gas--dynamical processes, which redistribute already enriched gas, and of star formation, which acts both as a source and as a sink of metals (Fabjan et al. 2008, Borgani et al. 2008). Our analysis on the AGN feedback effect on ICM properties lends further support to the idea that a feedback source associated to gas accretion onto super-massive BHs is required by the observational properties of the ICM (e.g. McNamara & Nulsen 2007). However, our results also show that there are still a number of discrepancies between observations and the predictions made by simulations. This is especially true within the core regions of massive clusters, where a more efficient way of extracting and/or thermalising energy released by AGN is required. Our results further demonstrate that different astrophysical feedback sources leave distinct signatures on the pattern of chemical enrichment of the ICM. These differences are much more evident in the outskirts of galaxy clusters, which retain memory of the past efficiency that energy feedback had in displacing enriched gas from star-forming regions and in regulating star formation itself (Fabjan et al. 2010). The characterization of thermal and chemical properties in cluster external regions requires X--ray telescopes with large collecting area and an excellent control of the background, characteristics which should be eventually met by a future generation of X--ray satellites. In the last part of this Thesis we studied the effect that different physical processes included in the simulations have on the mass--observable scaling relations and their evolution with redshift. We focused on two cluster mass proxies, the gas mass M_gas and a new Y_X proxy defined by Kravtsov et al. (2006) as the product of gas mass and cluster temperature and test the robustness of the two relations, M_tot-M_gas and M_tot-Y_X, in simulations before including any observational effect. Furthermore we test the relations against the change of prescription for the physics that describes the ICM, such as viscosity, thermal conduction, star formation, galactic winds and AGN feedback. We found that the evolutions of both relations do not show any significant deviation from the predictions of the simple self--similar model. However we found that the Y_X proxy is less sensitive to the change of physical processes included in simulations. Since Y_X is by definition a measure of the thermal pressure support in the ICM, once the central cluster region is excised, the relation M_tot-Y_X is more stable against the change of physical processes included in the simulations (Fabjan et al., in preparation). In the future, the improved numerical resolution expected to be reached in simulations of the next generation needs to be accompanied by a suitable description of the subresolution physics, both concerning the star formation physics and and the AGN feedback. Within the latter, the inclusion of the jet injection by AGN would of course provide a physically meaningful description of the interplay between BH accretion and ICM properties. While Chandra, XMM and Suzaku will be pushed to their limits in these studies in the next few years, there is no doubt that a detailed knowledge of the ICM out the cluster virial boundaries and reaching very high redshift has to await for the advent of the next generation of X--ray telescopes (Giacconi et al. 2009, Arnaud et al.2009).
XXII Ciclo
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Books on the topic "Galaxy Cluster Formation"

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International, School of Physics "Enrico Fermi" (1991 Varenna Italy). Galaxy formation: Varenna on Lake Como, Villa Monastero, 21-31 July 1992. Amsterdam: North-Holland, 1994.

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Frieswijk, Willem Freerk. Early stages of clustered star formation: Massive dark clouds throughout the galaxy. Enschede, the Netherlands: Ipskamp B.V. (printer), 2008.

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Symposium, International Astronomical Union. The central regions of the galaxy and galaxies: Proceedings of the 184th Symposium of the International Astronomical Union, held in Tokyo, Japan, August 18-22. Boston, Mass: Kluwer Academic, 1998.

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Symposium, International Astronomical Union. The central regions of the galaxy and galaxies: Proceedings of the 184th Symposium of the International Astronomical Union, held in Tokyo, Japan, August 18-22, 1997. Dordrecht: Kluwer Academic, 1998.

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Euro-Asian Astronomical Society, _., ed. Astronomical and Astrophysical Transactions, Vol. 32, No. 2. Cambridge Scientific Publishers, 2021. http://dx.doi.org/10.17184/eac.9781908106797.

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This issue of Astronomical and Astrophysical Transactions comprises the papers presented at the tenth annual conference on Modern Stellar Astronomy, held in Special Astrophysical Observatory of the Russian Academy of Sciences in October 2019. The “Modern Stellar Astronomy” conferences provide a forum for Russian scientists and scientists from the former Soviet Union concerned with stellar astronomy and related topics. The program consisted of invited talks, contributed oral talks, and poster papers. There were about 110 registered participants at the meeting. The program of the 2019 conference included 84 oral and 26 poster presentations. The key topics for the conference were Binary stars, Variable stars, Stellar clusters, Star formation, Exoplanets, Structure, kinematics and dynamics of the Milky Way Galaxy, Other galaxies. This volume comprises eleven of the papers that were presented at the conference.
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Book chapters on the topic "Galaxy Cluster Formation"

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Larson, Richard B. "Galaxy Formation and Cluster Formation." In The Harlow-Shapley Symposium on Globular Cluster Systems in Galaxies, 311–19. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-015-1104-9_43.

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Beasley, Michael A. "Globular Cluster Systems and Galaxy Formation." In Reviews in Frontiers of Modern Astrophysics, 245–77. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-38509-5_9.

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Fritze, Uta, and V. Alvensleben. "Star and Globular Cluster Formation in Mergers." In New Light on Galaxy Evolution, 376. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0229-9_88.

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Elbaz, D., and L. Vigroux. "Timescales for Galaxy Formation and Intra-Cluster Medium Enrichment." In New Light on Galaxy Evolution, 370. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0229-9_82.

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Harris, William E. "The Formation of Globular Cluster Systems: How, When, and Where?" In New Light on Galaxy Evolution, 87–96. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0229-9_13.

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Marín-Franch, A., and A. Aparicio. "Galaxy Formation Clues from Globular Cluster Systems: Preliminary Results for Coma." In The Evolution of Galaxies, 479. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-3313-7_122.

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Parmentier, Geneviève. "What cluster gas expulsion can tell us about star formation, cluster environment and galaxy evolution." In Reviews in Modern Astronomy, 183–97. Weinheim, Germany: Wiley-VCH Verlag GmbH & Co. KGaA, 2010. http://dx.doi.org/10.1002/9783527629190.ch10.

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Aragón-Salamanca, A., C. M. Baugh, and G. Kauffmann. "The K-Band Hubble Diagram For The Brightest Cluster Galaxies: A Test Of Galaxy Formation Models." In Galaxy Interactions at Low and High Redshift, 407. Dordrecht: Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-011-4665-4_109.

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Frenk, Carlos S. "Galaxy Clusters and the Epoch of Galaxy Formation." In The Epoch of Galaxy Formation, 257–64. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0919-9_28.

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Silk, Joseph. "Galaxy Formation in Galaxy Clusters: A Phenomenological Approach." In Cosmological Aspects of X-Ray Clusters of Galaxies, 293–98. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1022-8_31.

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Conference papers on the topic "Galaxy Cluster Formation"

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IVISON, ROB, IAN SMAIL, JAMES DUNLOP, and CLARE JENNER. "CLUSTER ENVIRONMENTS IN THE EARLY UNIVERSE: PROBING OBSCURED PROTO-ELLIPTICALS WITH SCUBA." In Implications for Galaxy Formation and Evolution. WORLD SCIENTIFIC, 2001. http://dx.doi.org/10.1142/9789812811738_0022.

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Diaferio, Antonaldo. "A WIDE-ANGLE VIEW OF GALAXY CLUSTER FORMATION: THE CAUSTIC TECHNIQUE." In Nineteenth Lomonosov Conference on Elementary Particle Physics. WORLD SCIENTIFIC, 2021. http://dx.doi.org/10.1142/9789811233913_0089.

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Kopylova, F., and A. Kopylov. "Study of groups/clusters of galaxies with the SDSS." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.148.

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Abstract:
For a large sample of groups/clusters of galaxies (N =185), we obtained the scaling relations among of their photometricaland dynamical parameters. We find:0.77±0.011. that in the virialized regions of the galaxy systems the total luminosity increase with mass L K ∝ M 200(M K <−21. m 0);2. that the new halo boundary of the galaxy systems corresponds to the splashback radius R sp . These radius is definedby the observed intergrated distribution of the number of galaxies as a function of the angular distance from thegroup/cluster center squared;3. that the fraction of galaxies with quenched star formation is maximal in the central regions of the galaxy systems,and it decreases to the radius R sp , but remains higher than in the field on ∼ 27%.
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Henning, Jason W., Brennan Gantner, Jack O. Burns, Eric J. Hallman, Sebastian Heinz, and Eric Wilcots. "Testing Numerical Models of Cool Core Galaxy Cluster Formation with X-Ray Observations." In THE MONSTER’S FIERY BREATH: FEEDBACK IN GALAXIES, GROUPS, AND CLUSTERS. AIP, 2009. http://dx.doi.org/10.1063/1.3293056.

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MILLER, NEAL A., and FRAZER N. OWEN. "THE FIR-RADIO CORRELATION IN NEARBY CLUSTERS: IMPLICATIONS FOR THE RADIO-TO-SUBMM INDEX REDSHIFT ESTIMATOR." In Implications for Galaxy Formation and Evolution. WORLD SCIENTIFIC, 2001. http://dx.doi.org/10.1142/9789812811738_0020.

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Seth, Anil, Michele Cappellari, Nadine Neumayer, Nelson Caldwell, Nate Bastian, Knut Olsen, Robert Blum, et al. "Nuclear Star Clusters & Black Holes." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458493.

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Jalali, Behrang, Markus Kissler-Patig, Karl Gebhardt, Eva Noyola, Nadine Neumayer, Victor P. Debattista, and C. C. Popescu. "Intermediate Mass Black Holes in Galactic Globular Clusters." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458500.

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Dokuchaev, V. I., Yu N. Eroshenko, S. G. Rubin, Victor P. Debattista, and C. C. Popescu. "Supermassive Black Hole Formation Inside Primordial Black Hole Clusters." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458495.

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Hartmann, Markus, Victor P. Debattista, Anil Seth, Michele Cappellari, Thomas Quinn, Victor P. Debattista, and C. C. Popescu. "Structural and Kinematical Constraints on the Formation of Stellar Nuclear Clusters." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458499.

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Carballo-Bello, J. A., D. Martínez-Delgado, A. Sollima, Victor P. Debattista, and C. C. Popescu. "Searching for Tidal Remnants in the Milky Way: Photometric Survey of Globular Clusters." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458513.

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Reports on the topic "Galaxy Cluster Formation"

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Miley, G., C. Carilli, G. B. Taylor, C. de Breuck, and A. Cohen. High Redshift Radio Galaxies: Laboratories for Massive Galaxy and Cluster Formation in the Early Universe. Fort Belvoir, VA: Defense Technical Information Center, January 2010. http://dx.doi.org/10.21236/ada520904.

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