Gotowe bibliografie tematyczne / Cluster of galaxie

Gotowa bibliografia na temat „Cluster of galaxie”

Autor: Grafiati
Data publikacji: 1 kwietnia 2023

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Spis treści

  1. Artykuły w czasopismach
  2. Rozprawy doktorskie
  3. Książki
  4. Części książek
  5. Streszczenia konferencji
  6. Raporty organizacyjne

Artykuły w czasopismach na temat "Cluster of galaxie":

1

Bogdán, Ákos, Lorenzo Lovisari, Patrick Ogle, Orsolya E. Kovács, Thomas Jarrett, Christine Jones, William R. Forman i Lauranne Lanz. "Detection of a Superluminous Spiral Galaxy in the Heart of a Massive Galaxy Cluster". Astrophysical Journal 930, nr 2 (1.05.2022): 138. http://dx.doi.org/10.3847/1538-4357/ac62cd.

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Abstract It is well established that brightest cluster galaxies (BCGs), residing in the centers of galaxy clusters, are typically massive and quenched galaxies with cD or elliptical morphology. An optical survey suggested that an exotic galaxy population, superluminous spiral and lenticular galaxies, could be the BCGs of some galaxy clusters. Because the cluster membership and the centroid of a cluster cannot be accurately determined based solely on optical data, we followed up a sample of superluminous disk galaxies and their environments using XMM-Newton X-ray observations. Specifically, we explored seven superluminous spiral and lenticular galaxies that are candidate BCGs. We detected massive galaxy clusters around five superluminous disk galaxies and established that one superluminous spiral, 2MASX J16273931+3002239, is the central BCG of a galaxy cluster. The temperature and total mass of the cluster are kT 500 = 3.55 − 0.20 + 0.18 keV and M 500 = (2.39 ± 0.19) × 1014 M ⊙. We identified the central galaxies of the four clusters that do not host superluminous disk galaxies at their cores, and established that the centrals are massive elliptical galaxies. However, for two of the clusters, the offset superluminous spirals are brighter than the central galaxies, implying that the superluminous disk galaxies are the brightest cluster galaxies. Our results demonstrate that superluminous disk galaxies are rarely the central systems of galaxy clusters. This is likely because galactic disks are destroyed by major mergers, which are more frequent in high-density environments. We speculate that the disks of superluminous disk galaxies in cluster cores may have been reformed due to mergers with gas-rich satellites.
2

Godłowski, W., i F. Baier. "Galaxy Orientation in Some Abell Clusters". Symposium - International Astronomical Union 186 (1999): 410. http://dx.doi.org/10.1017/s0074180900113245.

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We analyze a sample of galaxies in a region of three rich Abell Clusters. The data are taken from the Edinburgh Catalogue of the cluster. First, we divide the whole cluster area into different parts according to the assumed subclusters. Now we can find the position angles of the cluster and subclusters. We find strong evidence that the position angles of galaxies within our clusters are aligned to a large extent. For the cluster A754, position angles of galaxies tend to be perpendicular to the direction of the position angle of the cluster. Consequently, the angular momentum of galaxies are preferentially perpendicular to the cluster plane. For the cluster A14, position angles of galaxies tend to be parallel to the direction of the position angle of the cluster. Consequently, the angular momentum of galaxies are preferentially parallel to the cluster plane. For the cluster A3667 we obtain a more complicated picture suggesting that the alignment of galaxies in this cluster may have a different shape. From the distribution of the positions angles of galaxies we also found evidence for possible subclustering inside the whole cluster. This result is confirmed by the investigation of the distribution of the vectors normal to the galactic planes. Moreover we confirm the existence of a “line of sight” effect, originally found by Godłowski &, Ostrowski (1996) for galaxies belonging to the clusters in the Tully Catalogue (1988), for the clusters in our basic catalog.
3

Jeon, Seyoung, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon i Jinsu Rhee. "Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation". Astrophysical Journal 941, nr 1 (1.12.2022): 5. http://dx.doi.org/10.3847/1538-4357/ac9d8c.

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Abstract Cluster galaxies exhibit substantially lower star formation rates than field galaxies today, but it is conceivable that clusters were sites of more active star formation in the early universe. Herein, we present an interpretation of the star formation history (SFH) of group/cluster galaxies based on the large-scale cosmological hydrodynamic simulation, Horizon-AGN. We find that massive galaxies in general have small values of e-folding timescales of star formation decay (i.e., “mass quenching”) regardless of their environment, while low-mass galaxies exhibit prominent environmental dependence. In massive host halos (i.e., clusters), the e-folding timescales of low-mass galaxies are further decreased if they reside in such halos for a longer period of time. This “environmental quenching” trend is consistent with the theoretical expectation from ram pressure stripping. Furthermore, we define a “transition epoch” as where cluster galaxies become less star-forming than field galaxies. The transition epoch of group/cluster galaxies varies according to their stellar and host-cluster halo masses. Low-mass galaxies in massive clusters show the earliest transition epoch of ∼7.6 Gyr ago in lookback time. However, this decreases to ∼5.2 Gyr for massive galaxies in low-mass clusters. Based on our findings, we can describe a cluster galaxy’s SFH with regard to the cluster halo-to-stellar mass ratio.
4

Larsen, Søren S. "Open, Massive and Globular Clusters — Part of the Same Family?" Symposium - International Astronomical Union 207 (2002): 421–27. http://dx.doi.org/10.1017/s0074180900224133.

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Populations of young star clusters show significant differences even among “normal” disk galaxies. In this contribution I discuss how properties of young cluster systems are related to those of their host galaxies, based on a recent study of clusters in a sample of 22 nearby spiral galaxies. Luminous young clusters similar to the “super” star clusters observed in starbursts and mergers exist in several of these galaxies, and it is found that the luminosity of the brightest star cluster as well as the specific luminosity of the cluster systems both correlate well with the host galaxy star formation rate. When considering star clusters in different environments the traditional distinction between “open”, “massive” and “globular” clusters breaks down, underscoring the need for a universal physical description of cluster formation.
5

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 some new observational efforts aimed at constraining how and when elliptical galaxies and their globular cluster systems formed. These include systematic studies of the number of globular clusters around galaxies as a function of morphological type, studies of the kinematics of globular cluster populations in elliptical galaxies, and a variety of observational programs aimed at constraining the relative ages of globular clusters within galaxies as a function of cluster metallicity. The understanding of the formation of globular cluster systems and their host galaxies has grown dramatically in recent years, and the future looks equally promising.
6

Hashimoto, Yasuhiro, J. Patrick Henry i Hans Böhringer. "Dwarf Galaxies and Cluster Environments". Proceedings of the International Astronomical Union 14, S344 (sierpień 2018): 373–76. http://dx.doi.org/10.1017/s1743921318006890.

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AbstractWe report an investigation of the properties of dwarf galaxies (Mr < -15) inside 26 clusters at z = 0.15 – 0.25, using the X-ray data from the Chandra archive, and optical images taken with Subaru Suprime-Cam. Our results include: 1. Investigation of the dwarf galaxy density distribution is sensitive to the background galaxies and the choice of colour selection of galaxies. 2. Cluster-centric dwarf-to-giant ratio is highly sensitive to the level of subtracted background galaxies. 3. A certain fraction of faint galaxies always remain undetected by the detection algorithm near the center of clusters, even after carefully treating the halo or extra diffuse light created by bright galaxies. The number of ‘undetected’ faint galaxies varies significantly from cluster to cluster, and even from pointing to pointing. 4. Dwarf galaxies extend up to 2 Mpc from the center in most clusters. Meanwhile, the distribution of blue dwarf galaxies extends more to the outside. 5. For a given colour, the spatial distributions of dwarf galaxies and giant galaxies become similar. Namely, the most of the radial distribution comes from the colour, rather than the size, of galaxies. 6. Relative to the NFW profile, all of the galaxy populations are showing a deficit near the cluster core (r < 0.3 Mpc). 7. The dwarf-to-giant ratio shows no variation against cluster measures such as the richness and X-ray luminosity, as well as various cluster X-ray characteristics related to possible dynamical status of clusters.
7

Maier, C., C. P. Haines i B. L. Ziegler. "Star-formation quenching of cluster galaxies as traced by metallicity and presence of active galactic nuclei, and galactic conformity". Astronomy & Astrophysics 658 (luty 2022): A190. http://dx.doi.org/10.1051/0004-6361/202141498.

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Aims. We strive to explore the differences in the properties and quenching processes of satellite galaxies in a sample of massive clusters with passive and star-forming (SF) brightest cluster galaxies (BCGs). One aim is to investigate galactic conformity effects, manifested in a correlation between the fraction of satellite galaxies that halted star formation and the state of star formation in the central galaxy. Methods. We explored 18 clusters from the Local Cluster Substructure Survey at 0.15 < z < 0.26, using spectra from the Arizona Cluster Redshift Survey Hectospec survey of about 1800 cluster members at R < R200 in a mass-complete sample. Nine clusters have a SF BCG and nine have a passive BCG, which enable the exploration of galactic conformity effects. We measured the fluxes of emission lines of cluster members, allowing us to derive O/H gas metallicities and to identify active galactic nuclei (AGN). We compared our cluster galaxy sample with a control field sample of about 1300 galaxies with similar masses and at similar redshifts observed with Hectospec as part of the same survey. We used the location of SF galaxies, recently quenched galaxies (RQGs) and AGN in the projected velocity versus the position phase-space (phase-space diagram) to identify objects in the inner regions of the clusters and to compare their fractions in clusters with SF and passive BCGs. Results. The metallicities of log(M/M⊙)≥10 SF cluster galaxies with R < R200 were found to be enhanced with respect to the mass-metallicity relation obtained for our sample of coeval field SF galaxies. This metallicity enhancement among SF cluster galaxies is limited to lower-mass satellites (10 < log(M/M⊙) < 10.7) of the nine clusters with a passive BCG, with no metallicity enhancement seen for SF galaxies in clusters with active BCGs. Many of the SF galaxies with enhanced metallicities are found in the core regions of the phase-space diagram expected for virialized populations. We find a higher fraction of log(M/M⊙)≥10.7 SF galaxies at R < R500 in clusters with active BCGs as compared to clusters with passive BCGs, which stands as a signal of galactic conformity. In contrast, much higher fractions at R < R500 of AGN and, particularly of RQGs, are found in clusters with passive BCGs in comparison to clusters with active BCGs. Conclusions. We deduce that strangulation is initiated in clusters with passive BCGs when SF satellite galaxies pass R200, by stopping the pristine gas inflow that would otherwise dilute the interstellar medium and would keep their metallicities at the level of values similar to those of field galaxies at similar redshifts. These satellite galaxies continue to form stars by consuming the available gas in the disk. For galaxies with massses above log(M/M⊙)∼10.7 that manage to survive and remain SF when traveling to R < R500 of clusters with passive BCGs, we assume that they suffer a rapid quenching of star formation, likely due to AGN triggered by the increasing ram pressure stripping toward the cluster center, which can compress the gas and fuel AGN. These AGN can rapidly quench and maintain quenched satellite galaxies. On the other hand, we found that surviving SF massive satellite galaxies around active BCGs are less affected by environment when they enter R < R500, since we observe R < R500 SF galaxies with masses up to M ∼ 1011 M⊙ and with metallicities typical of coeval field galaxies. This observed galactic conformity implies that active BCGs must maintain their activity over timescales of at least ∼1 Gyr.
8

Teague, P. F., i D. Carter. "Modelling Clusters of Galaxies". Publications of the Astronomical Society of Australia 6, nr 2 (1985): 198–202. http://dx.doi.org/10.1017/s1323358000018087.

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AbstractThorough investigation of clusters of galaxies involves the complete modelling of their dynamics and structure. Presented here is a description of such a substantial project utilizing a sample of several rich southern clusters of galaxies. Incorporating results from radial velocity analyses of cluster galaxies and X-ray images of the clusters into rigorously constructed models of the cluster potential well and atmosphere will enable the dynamics, structure and evolution of clusters to be tied down.
9

Ali, Sadman S., Malcolm N. Bremer, Steven Phillipps i Roberto De Propris. "Environmental effects on the UV upturn in local clusters of galaxies". Monthly Notices of the Royal Astronomical Society 487, nr 3 (3.06.2019): 3021–28. http://dx.doi.org/10.1093/mnras/stz1502.

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ABSTRACT We explore the dependence of ultraviolet (UV) upturn colours in early-type cluster galaxies on the properties of their parent clusters (such as velocity dispersion and X-ray luminosity) and on the positions and kinematics of galaxies within them. We use a sample of 24 nearby clusters with highly complete spectroscopy and optical/infrared data to select a suitable sample of red-sequence galaxies, whose far-ultraviolet and NUV magnitudes we measure from archival GALEX data. Our results show that the UV upturn colour has no dependence on cluster properties and has the same range in all clusters. There is also no dependence on the projected position within clusters or on line-of-sight velocity. Therefore, our conclusion is that the UV upturn phenomenon is an intrinsic feature of cluster early-type galaxies, irrespective of their cluster environment.
10

Lee, Jong Chul, Ho Seong Hwang i Hyunmi Song. "Searching for Mg ii absorbers in and around galaxy clusters". Monthly Notices of the Royal Astronomical Society 503, nr 3 (5.03.2021): 4309–19. http://dx.doi.org/10.1093/mnras/stab637.

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ABSTRACT To study environmental effects on the circumgalactic medium (CGM), we use the samples of redMaPPer galaxy clusters, background quasars, and cluster galaxies from the Sloan Digital Sky Survey (SDSS). With ∼82 000 quasar spectra, we detect 197 Mg ii absorbers in and around the clusters. The detection rate per quasar is 2.7 ± 0.7 times higher inside the clusters than outside the clusters, indicating that Mg ii absorbers are relatively abundant in clusters. However, when considering the galaxy number density, the absorber-to-galaxy ratio is rather low inside the clusters. If we assume that Mg ii absorbers are mainly contributed by the CGM of massive star-forming galaxies, a typical halo size of cluster galaxies is smaller than that of field galaxies by 30 ± 10 per cent. This finding supports that galaxy haloes can be truncated by interaction with the host cluster.
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Artykuły w czasopismach Rozprawy doktorskie Książki

Rozprawy doktorskie na temat "Cluster of galaxie":

1

Březina, Karel. "Generátor herní mapy galaxie". Master's thesis, Vysoké učení technické v Brně. Fakulta informačních technologií, 2018. http://www.nusl.cz/ntk/nusl-385941.

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This thesis is focused on design and implementation of procedural generator of galaxy for games or simulations. Second goal is implementation of demonstration application which is showing possible usage of generator. Generator is able to create galaxy by predefined types or by user created map.
2

Zatloukal, Michael. "A search for distant cluster of galaxies in the COSMOS field". [S.l. : s.n.], 2008. http://nbn-resolving.de/urn:nbn:de:bsz:16-opus-88001.

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Jeltema, Tesla Erin. "Cosmology with clusters of galaxies : high-redshift clusters and the evolution of cluster substructure". Thesis, Massachusetts Institute of Technology, 2004. http://hdl.handle.net/1721.1/28372.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 2004.
Includes bibliographical references (p. 85).
Clusters of galaxies have become an important cosmological tool, yet we do not un-erstand many aspects of their formation and development. In this thesis, I pursue two projects aimed at using clusters to constrain cosmology and better understanding cluster evolution. First, I examine the Chandra observation of MS1054-0321. MS1054-0321 is the highest redshift cluster in the Einstein Medium Sensitivity Survey (EMSS), and it was one of the first high-redshift clusters observed with Chandra. I confirm that this cluster is hot and massive, although its temperature is slightly lower than inferred previously. I also detected an iron line in this cluster, one of the first detections of iron in a cluster at these redshifts, with an abundance consistent with early enrichment of the ICM. MS1054-0321 exhibits significant substructure, which I study in detail for the first time. In X-rays, it appears to be a nearly equal mass double cluster in the process of merging. Both the cluster galaxies and mass associated with the western subclump are offset from the X-ray peak, possibly indicating that the gas in the subclump is being stripped off as it falls into the cluster. Despite the lower temperature, I find that the detection of this cluster in the EMSS constrains Qm to be less than one.
(cont.) In the second project, I investigate the evolution of cluster substructure with redshift, quantifying for the first time cluster structure out to z [approx.] 1. My sample includes 40 X-ray selected, luminous clusters from the Chandra archive, and I quantify cluster morphology using the power ratio method (Buote & Tsai 1995). I find that, as expected qualitatively from hierarchical models of structure formation, high-redshift clusters have more substructure and are dynamically more active than low-redshift clusters. Specifically, the clusters with z > 0.5 have significantly higher average third and fourth order power ratios than the lower redshift clusters. This observation of structure evolution indicates that dynamical state may be an important systematic effect in cluster studies seeking to constrain cosmology, and when calibrated against numerical simulations, structure evolution will itself provide interesting bounds on cosmological models.
by Tesla Erin Jeltema.
Ph.D.
4

Zibetti, Stefano. "Diffuse stellar components in galaxies and galaxy clusters". Diss., lmu, 2004. http://nbn-resolving.de/urn:nbn:de:bvb:19-30331.

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Makiya, Ryu. "Cosmic-Ray Acceleration in Galaxies and Galaxy Clusters". 京都大学 (Kyoto University), 2013. http://hdl.handle.net/2433/175125.

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Buote, David Augustin. "The structure of elliptical galaxies and galaxy clusters". Thesis, Massachusetts Institute of Technology, 1995. http://hdl.handle.net/1721.1/36556.

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Yoshikawa, Koji. "Cosmological Hydrodynamic Simulations of Galaxies and Galaxy Clusters". 京都大学 (Kyoto University), 2002. http://hdl.handle.net/2433/149981.

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Pracy, Michael Benjamin Physics Faculty of Science UNSW. "The properties and evolution of galaxy populations in the rich cluster environment". Awarded by:University of New South Wales. Physics, 2006. http://handle.unsw.edu.au/1959.4/23033.

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This thesis is concerned with the role the rich cluster environment plays in the evolution of its galaxy population. We approach this issue from two angles, first we use deep wide-field imaging to investigate the effect of the cluster environment on the spatial and luminosity distribution of galaxies. Secondly, we focus on one particularly interesting class of galaxy, the enigmatic E+A galaxies, using a combination of state-of-the-art telescopes and novel instrumentation to elucidate the physical mechanisms and environmental influences causing the rapid change in star-formation activity in these galaxies. We present results from a deep photometric study of the rich galaxy cluster Abell 2218 (z=0.18) based on Hubble Space Telescope images. These have been used to derive the cluster luminosity function to extremely faint limits. We find the faint-end slope of the luminosity function to vary with environment within the cluster - in the sense that the ratio of `dwarf' galaxies to `giant' galaxies increases in the lower-density outskirt regions. Using imaging obtained with the Isaac Newton Telescope (INT) we confirm the presence of luminosity segregation in Abell 2218. However, luminosity segregation in clusters does not appear to be ubiquitous, with two other clusters studied with the INT (A119 at z=0.04 and A2443 at z=0.11) showing no sign of luminosity segregation of their galaxy populations. We use integral field spectroscopy of a sample of E+A galaxies in intermediate redshift clusters, obtained with the FLAMES system on the European Southern Observatory's VLT and the GMOS instrument on Gemini-North, to determine the radial variation in the strength of Hdelta absorption in these galaxies, and hence map out the distribution of the recently formed stellar population. We find a diversity of behaviour amongst these galaxies in terms of the radial variation in Hdelta absorption: with gradients that are either negative, flat, or positive. By comparing with numerical simulations we suggest that the first of these different types of radial behaviour provides evidence for a merger/interaction origin, whereas the latter two types of behaviour are more consistent with the truncation of star formation in normal disk galaxies.
9

Gupta, Nikhel [Verfasser], i Joseph [Akademischer Betreuer] Mohr. "High frequency cluster radio galaxies and the Sunyaev-Zel’dovich Effect properties of galaxy clusters / Nikhel Gupta ; Betreuer: Joseph Mohr". München : Universitätsbibliothek der Ludwig-Maximilians-Universität, 2018. http://d-nb.info/1154385981/34.

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VanDalfsen, Marcel L. Harris W. E. "The globular cluster system of the Sombrero galaxy". *McMaster only, 2004.

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Książki na temat "Cluster of galaxie":

1

Feretti, L., I. M. Gioia i G. Giovannini. Merging processes in galaxy clusters. Dordrecht: Springer, 2011.

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Kaastra, Jelle, red. Clusters of Galaxies. New York, NY: Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-78875-3.

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Hodge, Paul W. Galaxies. Cambridge, Mass: Harvard University Press, 1986.

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4

ESO Workshop on the Virgo Cluster of Galaxies (1984 Garching bei München, Germany). The Virgo cluster of galaxies. Garching bei München, Federal Republic of Germany: European Southern Observatory, 1985.

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Gustafson, John R. Stars, clusters, and galaxies. New York, NY: J. Messner, 1992.

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Ip, Peter Shun Sang. Binary galaxies in clusters. Toronto: University of Toronto, Dept. of Astronomy, 1994.

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Gustafson, John R. Stars, clusters, and galaxies. New York, NY: Scholastic Inc., 1992.

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Barrientos, Luis Felipe. The evolution of cluster elliptical galaxies. Toronto: Graduate Dept. of Astronomy, University of Toronto, 1999.

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Ashman, Keith M. Globular cluster systems. Cambridge, U.K: Cambridge University Press, 1998.

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Hobbs, Ian Stuart. The motions of galaxies in clusters of galaxies. Birmingham: University of Birmingham, 1997.

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Części książek na temat "Cluster of galaxie":

1

Chincarini, Guido. "Galaxy Environment and Clusters of Galaxies". W Cosmological Aspects of X-Ray Clusters of Galaxies, 19–38. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1022-8_4.

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van Kampen, Eelco. "The First Galaxies and Galaxy Clusters". W Astrophysics and Space Science Proceedings, 183–85. Dordrecht: Springer Netherlands, 2009. http://dx.doi.org/10.1007/978-1-4020-9190-2_31.

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Vollmer, Bernd. "Ram Pressure Stripping in the Virgo Cluster". W Mapping the Galaxy and Nearby Galaxies, 253–60. New York, NY: Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_37.

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Cortés, Juan R., Jeffrey D. P. Kenney i Eduardo Hardy. "Kinematics and Morphology of Peculiar Virgo Cluster Galaxies". W Mapping the Galaxy and Nearby Galaxies, 316. New York, NY: Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_52.

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Cooperstock, Fred I., i Steven Tieu. "The Motion of Galaxies in Galaxy Clusters". W Einstein's Relativity, 115–22. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-30385-2_10.

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Cudnik, Brian. "The Nature of Galaxies and Galaxy Clusters". W Astronomers' Observing Guides, 71–91. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4419-6757-2_4.

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Jiang, Biwei, Shuang Gao i Yongheng Zhao. "Candidate Streams of the Galactic Globular Clusters". W Mapping the Galaxy and Nearby Galaxies, 339. New York, NY: Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_75.

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Saitoh, Takayuki R., Jin Koda, Takashi Okamoto, Keiichi Wada i Asao Habe. "Tidal Disruption of Dark Matter Halos Around Proto-globular Cluster". W Mapping the Galaxy and Nearby Galaxies, 373. New York, NY: Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_109.

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de Grijs, Richard. "Star Cluster Evolution: From Young Massive Star Clusters to Old Globulars". W Globular Clusters - Guides to Galaxies, 353–56. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-76961-3_81.

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Parker, Barry. "Clusters and Superclusters". W Colliding Galaxies, 237–55. Boston, MA: Springer US, 1990. http://dx.doi.org/10.1007/978-1-4899-3348-5_12.

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Streszczenia konferencji na temat "Cluster of galaxie":

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Kopylova, F., i A. Kopylov. "Study of groups/clusters of galaxies with the SDSS". W 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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Streszczenie:
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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Victor Ribeiro de Jesus, João, i Rodrigo Lyra. "Um Estudo Sobre Identificação de Aglomerados de Galáxias". W Computer on the Beach. Itajaí: Universidade do Vale do Itajaí, 2020. http://dx.doi.org/10.14210/cotb.v11n1.p048-049.

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Galaxy clusters are fundamental blocks of our universe, like stars and galaxies. The study of galaxy clusters has shown complexity due to a large number of stars superimposed on these clusters, which emit light and block the clear optical band visualization of the phenomenon. In this paper, we present the implementation of an algorithm capable of classifying and remove the stars of spatial images. The purpose is to improve not only the existing studies around galaxy clusters but also to assist the developing in astronomic researches with available treated spatial images.
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Labini, F. Sylos. "On the distribution of galaxies and galaxy clusters". W Proceedings of the International School of Cosmic Ray Astrophysics 20th Anniversary, 11th Course. WORLD SCIENTIFIC, 2000. http://dx.doi.org/10.1142/9789812793997_0007.

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Balakina, E. A., i M. V. Pruzhinskaya. "Peculiar velocities of supernovae Ia in clusters of galaxies". W Всероссийская с международным участием научная конференция студентов и молодых ученых, посвященная памяти Полины Евгеньевны Захаровой «Астрономия и исследование космического пространства». Ural University Press, 2021. http://dx.doi.org/10.15826/b978-5-7996-3229-8.03.

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Observations of supernovae Ia make it possible to estimate the values of cosmological parameters using the Hubble diagram. First of all, such observations give us a value of the Hubble constant, which is one of the most important cosmological parameters. Improving the accuracy of measurements of this parameter is a priority for modern cosmological analysis. Therefore, it is necessary to take into account the influence of the peculiar velocities of supernovae Ia on the measurement of the redshift, which is used in constructing the Hubble diagram. We study the contribution of peculiar velocities due to the motion of host galaxies in the gravitational field of galaxy clusters for a cosmological sample of supernovae Pantheon.
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Ferland, Gary J. "Powering the intra-cluster filaments in cool-core clusters of galaxies". W THE 17TH INTERNATIONAL CONFERENCE ON ATOMIC PROCESSES IN PLASMAS (ICAPIP). AIP, 2012. http://dx.doi.org/10.1063/1.4707866.

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Gontcharov, G., A. Mosenkov, M. Khovritchev, V. Il’in, A. Marchuk, S. Savchenko, A. Smirnov i P. Usachev. "The properties of Galactic globular clusters from Gaia EDR3 and other data compared with theoretical isochrones". W 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/vak2021.2022.1.1.182.

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We fit theoretical isochrones from different models of internal structure and evolution of stars to photometric data for thestars in globular clusters of our Galaxy. To select cluster members, determine cluster sizes and calculate systemic propermotions, we use parallaxes and proper motions from Gaia EDR3. To calculate the most probable distance, age, interstellarextinction in a variety of filters and differential reddening in cluster fields, we use photometry in more than 26 filters betweenthe ultraviolet and mid-infrared waverange from HST, Gaia EDR3, Pan-STARRS DR1, DES, SDSS, unWISE, SAGE andother datasets in combination with the PARSEC, MIST, DSEP, and BaSTI-IAC isochrones, as for the solar metallicityscale as for alpha- and helium-enriched scales. The metallicity and enrichment of the clusters is taken from spectroscopicobservations and tested for compliance with the photometric results. We carry out a thorough analysis of random andsystematic uncertainties of the obtained results. The derived extinctions in many filters allow us to estimate an empiricalextinction law for each cluster. A complete analysis has been performed for five clusters (NGC288, NGC362, NGC5904,NGC6205, and NGC6218), a preliminary analysis, based on the Gaia EDR3 astrometry and photometry only, has beendone for 38 more clusters. The main conclusions are as follows. First, unprecedentedly accurate astrometry of Gaia EDR3allows us to segregate the cluster members from fore- and background stars and to indicate that the size of many clustersis much larger than previously thought. Second, the distances, derived by us from the photometry-to-isochrone fitting, arestill more precise than distances from the Gaia EDR3 parallaxes. Third, contrary to the popular 2D reddening maps ofSchlegel-1998 and Planck, we found no clusters at high Galactic latitudes with an extinction A V < 0.1. Fourth, for thehorizontal branch second parameter quartet NGC 288–NGC 362–NGC 5904–NGC 6218, the age is undoubtedly the secondparameter.
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Regis, Marco. "Correlation between Gamma-ray Sky and Catalogs of Galaxies and Galaxy Clusters". W XII Multifrequency Behaviour of High Energy Cosmic Sources Workshop. Trieste, Italy: Sissa Medialab, 2018. http://dx.doi.org/10.22323/1.306.0015.

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Strazzullo, V., P. Rosati, C. Lidman, C. Mullis, R. Demarco, R. Gobat, M. Nonino i in. "Cluster galaxies at redshift 1.4". W PROBING STELLAR POPULATIONS OUT TO THE DISTANT UNIVERSE: CEFALU 2008, Proceedings of the International Conference. AIP, 2009. http://dx.doi.org/10.1063/1.3141528.

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Delgado-Correal, Camilo, Piero Rosati, Gabriel Bartosch Caminha, Claudio Grillo, Amata Mercurio, Italo Balestra, Mario Nonino i Eros Vanzella. "Identification of low luminosity high redshift galaxies using galaxy clusters as cosmic telescopes". W Proceedings of the MG14 Meeting on General Relativity. WORLD SCIENTIFIC, 2017. http://dx.doi.org/10.1142/9789813226609_0242.

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BONAMENTE, MASSIMILIANO, i RICHARD LIEU. "EUV AND SOFT X–RAYS FROM CLUSTERS OF GALAXIES – THE 'CLUSTER SOFT–EXCESS' PHENOMENON". W Proceedings of the Third International Workshop. WORLD SCIENTIFIC, 2001. http://dx.doi.org/10.1142/9789812811363_0006.

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Raporty organizacyjne na temat "Cluster of galaxie":

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Zhang, Yuanyuan. Looking Wider and Further: The Evolution of Galaxies Inside Galaxy Clusters. Office of Scientific and Technical Information (OSTI), styczeń 2016. http://dx.doi.org/10.2172/1248222.

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

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Blanton, Elizabeth L., T. E. Clarke, Craig L. Sarazin, Scott W. Randall i Brian R. McNamara. AGN Feedback in Clusters of Galaxies. Fort Belvoir, VA: Defense Technical Information Center, styczeń 2010. http://dx.doi.org/10.21236/ada520956.

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Barkhouse, Wayne A., P. J. Green, A. Vikhlinin, D. W. Kim, D. Perley, R. Cameron, J. Silverman i in. ChaMP Serendipitous Galaxy Cluster Survey. Office of Scientific and Technical Information (OSTI), kwiecień 2006. http://dx.doi.org/10.2172/878722.

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Johnston, David E., Erin S. Sheldon, Risa H. Wechsler, Eduardo Rozo, Benjamin P. Koester, Joshua A. Frieman, Timothy A. McKay, August E. Evrard, Matthew R Becker i James Annis. Cross-correlation Weak Lensing of SDSS galaxy Clusters II: Cluster Density Profiles and the Mass--Richness Relation. Office of Scientific and Technical Information (OSTI), wrzesień 2007. http://dx.doi.org/10.2172/917267.

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Rykoff, E. S. The L_X-M relation of Clusters of Galaxies. Office of Scientific and Technical Information (OSTI), maj 2008. http://dx.doi.org/10.2172/928354.

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Werner, Norbert, J. de Plaa, J. S. Kaastra, Jacco Vink, J. A. M. Bleeker, T. Tamura, J. R. Peterson i F. Verbunt. XMM-Newton Spectroscopy of the Cluster of Galaxies 2a 0335+096. Office of Scientific and Technical Information (OSTI), styczeń 2006. http://dx.doi.org/10.2172/878003.

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Wiesner, Matthew P. Investigations of Galaxy Clusters Using Gravitational Lensing. Office of Scientific and Technical Information (OSTI), sierpień 2014. http://dx.doi.org/10.2172/1155188.

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Hao, Jiangang. Optical galaxy cluster detection across a wide redshift range. Office of Scientific and Technical Information (OSTI), kwiecień 2009. http://dx.doi.org/10.2172/971005.

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Miller, Christopher J. Complementary Probes of Dark Energy using Galaxy Clusters. Office of Scientific and Technical Information (OSTI), lipiec 2018. http://dx.doi.org/10.2172/1461837.

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