The Redistribution Of Matter In The Cores Of Galaxy Clusters
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Convergence and scatter of cluster density proﬁles
the central few percent of a dark matter structure - the lat-est observations of galaxy and clusters probe the mass dis-tribution within one percent of the virial radius, which un-til recently was unresolved by numerical simulations. Forth-coming experiments, such as VERITAS (Weekes et. al 2002) and MAGIC (Flix, Martinez & Prada 2004) will
RESIDUAL GAS MOTIONS IN THE INTRACLUSTER MEDIUM AND BIAS IN
cosmological simulations of 16 simulated clusters, including both very relaxed and unrelaxed systems and spanning a virial mass range of 5 × 1013 2 × 1015 h−1 M. We investigate effects of the residual subsonic gas motions on the hydrostatic estimates of mass proﬁles and concentrations of galaxy clusters. In agreement
Chromospheric Modelling in Late-typeDwarfs 2. CES
Again, their position relative to the parent galaxy and their colours indicate typical halo objects. A huge HII region in the main body of A0142-43shows that star-formingprocesses took place quite recently in it. If there are populous clusters ofvery young age associated with it they are veiled by this bright gas complex. It should be
The Scaling Properties of Fossil Galaxy Groups
resemble those of clusters with cool cores Fossil cooling time << 1 Gyr, despite old age & no signs of strong cooling! => heat input / redistribution => feedback Fossils have high mass density => early formation epoch
The Formation of Galaxies: connecting theory to data
AGN evolution BH growth, feedback to galaxy and environment Reionisation suppression of dwarf galaxy formation Galaxy interactions/mergers morphological transformation Only the last can be simulated realistically ab initio semi-analytic (phenomenological) techniques N.B. SA modelling is a technique for studying galaxy formation
CHANDRA X-RAY SPECTRA FROM HYDRO SIMULATIONS OF GALAXY CLUSTERS
of hydrodynamic simulations of galaxy clusters is then constructed and for each cluster all of the hydro variables are output at various redshifts. In order to obtain simulated spectral ﬁt temperatures the simulated photon spectra are ﬁrst calculated from the simulated clusters observed at various redshifts along a given line of sight.
Perfection Learning Correlation of Earth Science: The
Earth s interior. [Clarification Statement: Evidence should include drill cores, gravity, seismic waves, and laboratory experiments on Earth materials.] b. Use a model of Earth s interior and the mechanisms of thermal convection to explain the cycling of matter and the impact of plate tectonics on Earth s surface.
SUMMARY AND REVIEW: INTERACTION OF OBSERVATIONS AND THEORY OF
degenerate matter. The collective properties of the variable stars uncovered by the MACHO and OGLE surveys are extremely illuminating for the understanding of stellar pulsation, as illustrated by Kern Cook and Dante Minniti at this meeting. 2. Fundamental Properties Fundamental observed properties of stars have always played crucial roles
Angular momentum and the formation of stars and black holes
spin angular momentum of the matter from which each star forms could in principle be transferred to outlying gas or to the orbital motions of other stars, and both magnetic and gravitational forces can play important roles in this loss or redistribution of angular momentum. As will be reviewed in section 2, magnetic torques
Durham Research Online
ulars are the dominant morphological galaxy type in the cores of nearby rich clusters such as Coma (Dressler 1980). This relatively large abundance of lenticulars and a high central galaxy density make Coma an excellent laboratory for studying the environmental dependence of bars. In order to develop and test techniques for bar detection and
The role of tidal interactions in star formation
cloud rotating with the Galaxy, and showed that this is many orders of magnitude more than can be accommodated in a single star even when rotating at breakup speed (Mestel 1965; Spitzer 1968). We have learned since then that stars form in dense molecular cloud cores that rotate much more slowly than would be expected on this
The physics of star formation
Jul 01, 2003 The physics of star formation 1653 forming stars, may be chaotic and create a large dispersion in the properties of stars and stellar systems. Thus, star formation processes, like most natural phenomena, probably involve a
TIDALLY INDUCED BARS OF GALAXIES IN CLUSTERS
clusters. Our progenitor is a massive, late-type galaxy similar to the Milky Way, composed of an exponential disk and a Navarro-Frenk-White dark matter halo. We place the galaxy on four different orbits in a Virgo-like cluster and evolve it for 10Gyr. As a reference case, we also evolve the same model in isolation. Tidally induced bars
Hipparcos: some scientiﬁc results
matter halo is triaxial, and tumbles with a characteristic rate of ~ 2 rad/Hubble time, or about 30 microarcsec/year This (and other effects) results in the rotation of the angular momentum vector of the Galaxy stellar disk population with respect to the quasar reference frame Gaia should establish the spin vector of the transformation
How Baryonic Processes aﬀect Strong Lensing properties of
Komatsu et al. 2011), including the formation of galaxy clusters (e.g. Kravtsov & Borgani 2012). However, the inter-nal structure of galaxy clusters has posed a challenge. The earliest comparisons between simulated clusters and the ob-served frequency of gravitational lensing arcs revealed a se-rious discrepancy between the observations and
EVOLUTIONARY MODELS OF ROTATING DENSE STELLAR SYSTEMS WITH
We present evolutionary models of rotating self-gravitating systems (e.g. globular clusters, galaxy cores). These models are characterized by the presence of an initial axi-symmetry due to rotation. Central black hole seeds are included in our models, and black hole growth due to the consumption of stellar matter
Turbulence, magnetic ﬁelds, and plasma physics in clusters of
cool cores and hotter, more diffuse material in the outlying regions.1 Necessarily, the ﬁrst observations and the ﬁrst theoretical models of clusters concerned what one might call large-scale features, such as the overall proﬁles of mass and tempera-ture, the structure formation, and the role of the central ob-jects.
Chandra Analysis of a Possible Cooling Core Galaxy Cluster at
core clusters. Galaxy clusters form cooling cores when they have not merged with other clusters for at least one billion years. As they recover from mergers with smaller clusters of galaxies, massive clusters approach hydrostatic equilib-rium and rather than having an elliptical or irregular morphology (see Fig. 2), they gain a spherically symmet-
evolution of x ray and optical properties of galaxy groups
Galaxy Clusters 1.1 Introduction to clusters A galaxy is a dynamically bound system that consists of many stars, dust and dark matter. Most of the mass-energy in galaxies (about 95%) is dark. It is called dark because it does not emit any form of electromagnetic radiation. The existence of dark matter is inferred indirectly by its gravitational
arXiv:1409.5152v1 [astro-ph.CO] 17 Sep 2014
in their cores and surrounded by S-clusters (50%), (2) new superclusters formed by S-clusters only (40%), (3) redistribution of member clusters by fragmentation of rich (multiplicity m>15) superclusters (8%), and (4) new superclusters formed by the connection of A-clusters through bridges of S-clusters (2%). Power-law ﬁts to the cu-
arXiv:astro-ph/0603275v3 8 Jun 2006
sive galaxy clusters are especially important in tracing LSS evolution. The most massive clusters provide the cleanest re-sults in comparing theory with observations. Excluding cooling cores (Fabian & Nulsen 1977), a self-similar behaviour of the distributions of the ICM proper-ties such as the temperature, density and entropy of mas-
HI gas in galaxies from z = 0 to z = 0
Keywords: galaxy evolution; H I line emission PACS: 98.62.Ai INTRODUCTION In current scenarios of the formation and evolution of galaxies dark matter halos grow by merging, gas falls into these halos, cools and forms stars. Currently there is much debate about the physics of the gas accretion, does gas first get shock heated to the virial
How to Form (Twin) Globular Clusters?
How to Form (Twin) Globular Clusters? 2 GMC mass M, its radiusR and the gravitational constant G). Thus, the system isonlygravitationally bound(i.e. E becomesnegative), iftheSFE ,whichisthe mass fraction of the GMC transformed into stars, is larger than 50%. Though mass redistribution in a violent relaxation stage and a detailed treatment of the
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cores (Vogelsberger, Zavala & Loeb 2012; Rocha et al. 2013)and less evaporation than previously thought. A self-interaction cross-section per particle mass, σ/m ≈ 1cm2 g−1 remains as consistent with observations as non-interacting CDM. The largest bound structures in the Universe are galaxy clusters
Larger sizes of massive quiescent early-type galaxies in
a matter of debate. We have shown in previous work how the study of the mass-size relation in diﬀerent environments can provide important constraints to galaxy evolution models. In this paper, we focus on the mass-size relation of quiescent massive ETGs (M∗/M⊙ > 3×1010) living in massive clusters (M200 ∼ 1014 M⊙) at 0.8 < z < 1.5, as
Mass Modeling of Disk Galaxies: Constraints and Adiabatic
(Weinberg & Katz 2002). These processes favor extensive mass redistribution in a galaxy s central parts and can generate at stellar and gaseous cores (˘ constant surface density) frominitiallycuspy (concentrated) CDM halos. Adiscussion ofthe satellite and angular momentum problems is beyond the scope of this paper1.
Clayton H. Heller, and E. Athanassoula
STRUCTURE FORMATION INSIDE TRIAXIAL DARK MATTER HALOS: GALACTIC DISKS, BULGES AND BARS Clayton H. Heller,1 Isaac Shlosman2 and E. Athanassoula3 accepted for publication by the Astrophysical Journal ABSTRACT We investigate the formation and subsequent co-evolution of galactic disks immersed in assembling live dark matter (DM) halos.
Maximum feedback and dark matter proﬁles of dwarf galaxies
heated gas may leave the dwarf galaxy in a form of fast wind (e.g., Dekel & Silk 1986). In an idealization of this problem, a signiﬁcant fraction of the gas may be removed from the dwarf halo on a time-scale shorter than the dynamical time. We consider the reaction of the dark matter distribution to the sudden loss of baryonic mass in the centre.
How do galaxy clusters form and evolve over cosmic time
Star/galaxy formation ⇒ cooling 㱺 over-cooling 㱺 SN/SMBH feedback? Thermal regulation in (cooling) cluster cores ICM entropy in present day clusters Beyond gravity: cosmic feedback grav. heating (Voit et al 05) Relative role of cooling, (pre) heating by XMM Pratt et al, 06 Chandra When and how this excess