Gotowe bibliografie tematyczne / Clusters of galaxies

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  1. Artykuły w czasopismach
  2. Rozprawy doktorskie
  3. Książki
  4. Części książek
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Gotowa bibliografia na temat „Clusters of galaxies”

Autor: Grafiati
Data publikacji: 4 czerwca 2021
Data aktualizacji: 18 maja 2024

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Artykuły w czasopismach na temat "Clusters of galaxies"

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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.
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Kuchner, Ulrike, Roan Haggar, Alfonso Aragón-Salamanca, Frazer R. Pearce, Meghan E. Gray, Agustín Rost, Weiguang Cui, Alexander Knebe i Gustavo Yepes. "An inventory of galaxies in cosmic filaments feeding galaxy clusters: galaxy groups, backsplash galaxies, and pristine galaxies". Monthly Notices of the Royal Astronomical Society 510, nr 1 (27.11.2021): 581–92. http://dx.doi.org/10.1093/mnras/stab3419.

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ABSTRACT Galaxy clusters grow by accreting galaxies from the field and along filaments of the cosmic web. As galaxies are accreted they are affected by their local environment before they enter (pre-processing), and traverse the cluster potential. Observations that aim to constrain pre-processing are challenging to interpret because filaments comprise a heterogeneous range of environments including groups of galaxies embedded within them and backsplash galaxies that contain a record of their previous passage through the cluster. This motivates using modern cosmological simulations to dissect the population of galaxies found in filaments that are feeding clusters, to better understand their history, and aid the interpretation of observations. We use zoom-in simulations from The ThreeHundred project to track haloes through time and identify their environment. We establish a benchmark for galaxies in cluster infall regions that supports the reconstruction of the different modes of pre-processing. We find that up to 45 per cent of all galaxies fall into clusters via filaments (closer than 1 h−1Mpc from the filament spine). 12 per cent of these filament galaxies are long-established members of groups and between 30 and 60 per cent of filament galaxies at R200 are backsplash galaxies. This number depends on the cluster’s dynamical state and sharply drops with distance. Backsplash galaxies return to clusters after deflecting widely from their entry trajectory, especially in relaxed clusters. They do not have a preferential location with respect to filaments and cannot collapse to form filaments. The remaining pristine galaxies (∼30–60 per cent) are environmentally affected by cosmic filaments alone.
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Aguerri, J. A. L., M. Girardi, I. Agulli, A. Negri, C. Dalla Vecchia i L. Domínguez Palmero. "Deep spectroscopy in nearby galaxy clusters – V. The Perseus cluster". Monthly Notices of the Royal Astronomical Society 494, nr 2 (24.03.2020): 1681–92. http://dx.doi.org/10.1093/mnras/staa800.

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ABSTRACT Dwarfs are the largest population of galaxies in number in the nearby Universe. Deep spectroscopic data are still missing to obtain a better understanding of their formation and evolution processes. This study shows the results obtained from a spectroscopic campaign in the Perseus cluster. We have obtained 963 new galaxy spectra. We have measured the recessional velocity of the galaxies by using a cross-correlation technique. These data have been used to obtain the cluster membership, the dynamics of the galaxies, and the spectroscopic luminosity function (LF) of the cluster. The cluster membership was obtained by using the peak + gap technique, reporting a total of 403 galaxies as cluster members within 1.4r200. The mean velocity and velocity dispersion of the cluster galaxies are Vc = 5258 km s−1 and σc = 1040 km s−1, respectively. We obtained M200 = 1.2 × 1015 M⊙ and r200 = 2.2 Mpc for this cluster. The clusters members were classified blue and red according to their g − r stellar colour. The velocity dispersion of these two families of galaxies is different, indicating that the blue galaxies can be classified as recently accreted into the cluster. We present the spectroscopic galaxy LF of the cluster. This function turned to be flat: α = 0.99 ± 0.06. In addition, blue and red galaxies show similar densities in the faint end of the LF. This indicates that Perseus does not have a population of red dwarf galaxias as large as other nearby clusters. We have compared the LF of the Perseus cluster with other spectroscopic LFs of nearby clusters and those from cosmological simulations. This comparison shows that the spectroscopic LF of nearby galaxy cluster is far from universal.
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Pallero, Diego, Facundo A. Gómez, Nelson D. Padilla, Yannick M. Bahé, Cristian A. Vega-Martínez i S. Torres-Flores. "Too dense to go through: the role of low-mass clusters in the pre-processing of satellite galaxies". Monthly Notices of the Royal Astronomical Society 511, nr 3 (17.11.2021): 3210–27. http://dx.doi.org/10.1093/mnras/stab3318.

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ABSTRACT We study the evolution of satellite galaxies in clusters of the c-eagle simulations, a suite of 30 high-resolution cosmological hydrodynamical zoom-in simulations based on the eagle code. We find that the majority of galaxies that are quenched at z = 0 (≳80${{\ \rm per\ cent}}$) reached this state in a dense environment (log10M200[M⊙] ≥13.5). At low redshift, regardless of the final cluster mass, galaxies appear to reach their quenching state in low-mass clusters. Moreover, galaxies quenched inside the cluster that they reside in at z = 0 are the dominant population in low-mass clusters, while galaxies quenched in a different halo dominate in the most massive clusters. When looking at clusters at z > 0.5, their in situ quenched population dominates at all cluster masses. This suggests that galaxies are quenched inside the first cluster they fall into. After galaxies cross the cluster’s r200 they rapidly become quenched (≲1 Gyr). Just a small fraction of galaxies ($\lesssim 15{{\ \rm per\ cent}}$) is capable of retaining their gas for a longer period of time, but after 4 Gyr, almost all galaxies are quenched. This phenomenon is related to ram pressure stripping and is produced when the density of the intracluster medium reaches a threshold of $\rho _{\rm ICM}\, \sim 3 \times 10 ^{-5}$ nH (cm−3). These results suggest that galaxies start a rapid-quenching phase shortly after their first infall inside r200 and that, by the time they reach r500, most of them are already quenched.
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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.
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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.
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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.
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Anders, Peter, Uta Fritze –. v. Alvensleben i 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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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.
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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.
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Rozprawy doktorskie na temat "Clusters of galaxies"

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Millington, S. J. C. "Clusters of galaxies". Thesis, University of Oxford, 1987. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.382461.

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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.
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De, Lucia Gabriella. "Evolution of Galaxies in Clusters". Diss., lmu, 2004. http://nbn-resolving.de/urn:nbn:de:bvb:19-25762.

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White, David Allen. "The multiphase medium of elliptical galaxies and clusters of galaxies". Thesis, University of Cambridge, 1992. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.240155.

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Piffaretti, Rocco. "Faraday rotation in clusters of galaxies". Zürich : ETH, Eidgenössische Technische Hochschule, 2000. http://e-collection.ethbib.ethz.ch/show?type=dipl&nr=17.

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Reblinsky, Katrin. "Projection effects in clusters of galaxies". Diss., lmu, 2000. http://nbn-resolving.de/urn:nbn:de:bvb:19-4153.

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Mora, Marcelo D. "Star clusters in unperturbed spiral galaxies". Diss., lmu, 2008. http://nbn-resolving.de/urn:nbn:de:bvb:19-92728.

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MacLaren, Ian. "Studies of distant clusters of galaxies". Thesis, Durham University, 1987. http://etheses.dur.ac.uk/6891/.

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A technique of constructing crude, low-resolution Spectral Energy Distributions (SEDs) for galaxies in distant clusters, using a set of intermediate bandwidth filters and a CCD detector, is developed which is capable of redressing many of the problems which have previously beset work in this field. The technique has been used to study galaxies in the distant clusters 0016+16 (z = 0.54) and Abell 370 (z = 0.37).These SEDs are then used to individually classify each object in the CCD field, ascribing both an estimated redshift and a galaxy type. The SEDs have been extended into the rest-frame ultraviolet (~ 270 nm) by imaging high redshift galaxies in blue passbands. Monitoring the behaviour of the Colour-Magnitude effect in the optical and -ultraviolet (uv) regions, indicates the presence of a new class of object which exhibits excess emission in the uv whilst having optical colours similar to nearby E/SO galaxies. The significance of this uv-excess is addressed by examining the available uv spectroscopy of nearby early-type galaxies obtained from observations carried out on the International Ul traviolet Explorer satellite. This study, in conjunction with a series of crude evolutionary models, leads to the conclusion that the uv-excess is most likely a manifestation of evolutionary differences in the spectral properties of galaxies at high redshifts, resulting from increased levels of star formation. Having developed such methods for using distant clusters of galaxies as evolutionary probes, a catalogue of candidate distant clusters is constructed from high contrast copies of deep 4m photographic plates. Finally, a series of possible future observations bcised on such a resource, combining a wide range of techniques, is outlined.
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Basson, J. F. "Cold gas in clusters of galaxies". Thesis, University of Cambridge, 2003. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.596456.

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The intracluster gas has only been fully explored in the last decade or so with the launch of the ROSAT satellite in 1990, and more recently the Chandra and XMM-Newton satellites in 1999. The data obtained from these X-ray telescopes has provided significant information about the intracluster medium. In this thesis, a theoretical and numerical study of the nature of the ICM is undertaken. In particular the formation and influence of cold gas clouds and the effects of powerful FR-II radio sources are considered. Clusters are modelled as a multi-phase cooling gas in a dark-matter potential well. The formation of cold gas clouds through the thermal instability is studied, as is the effects of shocks on cold clouds. The latter is important because of the alignment effect which implies that the presence of a radio source increases the luminosity of the clouds. Radio sources which occur as a result of feedback from the accretion of the cooling intracluster gas onto a central AGN have a noticeable effect on the energetics of the cluster. Observationally, they manifest themselves as cavities in the X-ray emitting ICM. Whether they are capable of halting the inflowing cooling ICM depends on the relative powers of the cooling flow and radio source. The jets expand supersonically into the ICM, heating and dragging the cluster gas out of the potential well. As this shocked gas rises, it cools adiabatically. As it falls back inwards, it forms a layer of cooler gas around the cocoon. The ICM gas is thermally unstable, and the contact discontinuity will be Rayleigh-Taylor unstable provided that its deceleration does not exceed the gravitational force. Coupling between the Rayleigh-Taylor and thermal instability modes can occur, and it is found that the growth rate increases over the individual uncoupled rates when they are of the same order of magnitude. This could provide a mechanism for the information of cold clouds around this interface.
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Moore, Ben. "Groups, clusters and superclusters of galaxies". Thesis, Durham University, 1991. http://etheses.dur.ac.uk/6091/.

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Galaxies are observed in a diverse range of associations. Understanding the dynamical, statistical and clustering properties of aggregations of galaxies forms the main body of this thesis. On the smallest scale, we use a model for the Local Group to study the formation of a typical galaxy system and to understand the mass distribution within the Local Group. Our model is a binary system excised from numerical simulation of a Universe dominated by cold dark matter which has similar radial velocity and separation as M31 and the Milky Way. We find that the timing argument provides a reliable method for placing a lower limit to the mass of the Local Group. The anisotropy parameter of the particle orbits within the dark halos of CDM are predicted to radially biased. To reconcile the mass of the Milky Way with the predictions from the timing argument and the mass of our model halo, the satellites of our Galaxy must be on circularly biased orbits. The asymptotic values of the rotation curves of the two halos match very closely those of M31 and the Milky Way, as the halos come closer together the curves become very distorted. A simple treatment of gas within our model extends the rotation curves into the central regions of the halos. In our model, M31 and the Milky Way collide 2.5 Gyrs from the present time, a fraction of the current crossing time. Intermediate scales are probed using a statistical analysis of groups of galaxies identified using well defined selection criteria from the CfA redshift survey. The grouping algorithm is optimised using artificial galaxy catalogues constructed from N-body simulations which have similar low order correlations to the original survey. We develop a method of estimating the total luminosity of groups of galaxies identified within magnitude limited redshift surveys and use it to calculate the luminosity function of galactic systems. This statistic measures the abundance of gravitationally bound structures, independent of the detailed arrangement of the luminous material within them. We find that this function has a smooth transition from single galajdes to rich clusters. The distribution of group velocity dispersions shows a discontinuity at the transition between groups and rich clusters. The correlation function of groups is found to depend on the mass range of the sample, luminous groups are more strongly correlated than faint groups. We compare these results with predictions from the CDM model and have extended to intermediate scales the previous success of the model on galactic and cluster scales. On large scales we have used an all sky redshift survey of galaxies detected by IRAS to investigate the topology of the Universe to a depth of 200h(^-1) Mpc. Qualitatively, the distribution of galaxies out to this distance appears similar to a Gaussian density field with a sponge-like topology. High and low density regions are topologically similar and surfaces of constant density are interconnected. Quantitatively, we have used the genus-threshold density relation of Hamilton et al. to measure the slope of the power spectrum over a range of length scales between l0 (^-1) Mpc and 50h(^-1) Mpc. To constrain the slope of the power spectrum we used artificial "galaxy" catalogues constructed from N-body simulations and a variety of Monte-Carlo and bootstrap techniques. Our topological analysis is consistent with a spectrum of power-law form with n ~ -1 (in δk(^2) x k(^n)) over the range of scales considered. Values of n < -1.8 and n > 0 are strongly ruled out by our data. The inferred power spectrum of the distribution of IRAS galaxies is similar to the predicted mass spectrum in the standard cold dark matter model on scales <15 h(^-1) Mpc, but falls off less steeply on larger scales. This discrepancy is significant at over 2σ and implies that structure identified by IRAS galaxies is coherent over scales larger than expected from the CDM model.
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Książki na temat "Clusters of galaxies"

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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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Galaxies. Cambridge, Mass: Harvard University Press, 1986.

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

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

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Richtler, Tom, i Søren Larsen, red. Globular Clusters - Guides to Galaxies. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-76961-3.

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Fabian, A. C., red. Clusters and Superclusters of Galaxies. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2482-9.

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NATO, Advanced Study Institute on Clusters and Superclusters of Galaxies (1991 Cambridge England). Clusters and superclusters of galaxies. Dordrecht: Kluwer Academic Publishers, 1992.

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Fabian, A. C. Clusters and Superclusters of Galaxies. Dordrecht: Springer Netherlands, 1992.

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Części książek na temat "Clusters of galaxies"

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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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Contopoulos, Georgios, i Dimitrios Kotsakis. "Galaxies and Clusters of Galaxies". W Cosmology, 32–61. Berlin, Heidelberg: Springer Berlin Heidelberg, 1987. http://dx.doi.org/10.1007/978-3-642-71464-1_3.

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Unsöld, Albrecht, i Bodo Baschek. "Galaxies and Clusters of Galaxies". W The New Cosmos, 402–67. Berlin, Heidelberg: Springer Berlin Heidelberg, 2002. http://dx.doi.org/10.1007/978-3-662-04356-1_12.

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Chincarini, Guido. "Clusters of Galaxies". W Astrophysics and Space Science Library, 217–25. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2919-7_27.

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Bower, Richard. "Clusters of Galaxies". W Planets, Stars and Stellar Systems, 265–303. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5609-0_6.

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BÖhringer, H. "Clusters of Galaxies". W Astrophysics and Space Science Library, 359–68. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0794-5_36.

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Mushotzky, Richard. "Clusters of galaxies". W The Century of Space Science, 473–98. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0320-9_21.

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Longair, Malcolm S. "Clusters of Galaxies". W Astronomy and Astrophysics Library, 71–105. Berlin, Heidelberg: Springer Berlin Heidelberg, 1998. http://dx.doi.org/10.1007/978-3-662-03571-9_4.

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Takase, Bunshiro, Keiichi Kodaira i Sadanori Okamura. "Clusters of Galaxies". W An Atlas of Selected Galaxies, 16–20. London: Routledge, 2023. http://dx.doi.org/10.1201/9781315137216-9.

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Takase, Bunshiro, Keiichi Kodaira i Sadanori Okamura. "Clusters of Galaxies". W An Atlas of Selected Galaxies, 64–70. London: Routledge, 2023. http://dx.doi.org/10.1201/9781315137216-18.

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Streszczenia konferencji na temat "Clusters of galaxies"

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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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Chincarini, Guido. "Clusters of Galaxies: A Commentary". W A Festschrift in Honor of Ricardo Giacconi. WORLD SCIENTIFIC, 2000. http://dx.doi.org/10.1142/9789812792174_0012.

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Bahcall, Neta A. "Cosmology with Clusters of Galaxies". W Proceedings of Nobel Symposium 109. WORLD SCIENTIFIC, 2001. http://dx.doi.org/10.1142/9789812810434_0003.

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DONAHUE, M. "COSMOLOGY WITH CLUSTERS OF GALAXIES". W Proceedings of the 32nd Coral Gables Conference. WORLD SCIENTIFIC, 2005. http://dx.doi.org/10.1142/9789812701992_0018.

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Poggianti, Bianca. "Evolution of galaxies in clusters". W Baryons in Dark Matter Halos. Trieste, Italy: Sissa Medialab, 2004. http://dx.doi.org/10.22323/1.014.0104.

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Mushotzky, Richard F. "The missing mass in clusters of galaxies and elliptical galaxies". W After the first three minutes. AIP, 1991. http://dx.doi.org/10.1063/1.40402.

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CAVALIERE, A. "CLUSTERS OF GALAXIES IN X-RAYS". W A Festschrift in Honor of Ricardo Giacconi. WORLD SCIENTIFIC, 2000. http://dx.doi.org/10.1142/9789812792174_0010.

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FABIAN, A. C., i S. W. ALLEN. "X-RAYS FROM CLUSTERS OF GALAXIES". W Proceedings of the XXI Symposium on Relativistic Astrophysics. WORLD SCIENTIFIC, 2003. http://dx.doi.org/10.1142/9789812704009_0018.

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Ferrari, L., D. Bagliani, A. Bardi, E. Battistelli, M. Birkinshaw, S. Colafrancesco, A. Conte i in. "Spectroscopic Active Galaxies and Clusters Explorer". W THE THIRTEENTH INTERNATIONAL WORKSHOP ON LOW TEMPERATURE DETECTORS—LTD13. AIP, 2009. http://dx.doi.org/10.1063/1.3292383.

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Garilli, Bianca, Dario Maccagni, Luis Carrasco i Elsa Recillas. "Photometric properties of clusters of galaxies". W Dark matter. AIP, 1995. http://dx.doi.org/10.1063/1.48328.

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Raporty organizacyjne na temat "Clusters of galaxies"

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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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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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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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Press, W. H. (Astrophysics of binary stars, Seyfert galaxies, quasars, and globular clusters. Final technical report. Office of Scientific and Technical Information (OSTI), marzec 1985. http://dx.doi.org/10.2172/6429223.

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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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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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