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Register a new userLuminosity Segregation from Merging in Clusters of Galaxies
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Added by
Fusco-Femiano Roberto
Publication date
1998
fields
Physics
and research's language is
English
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We compute the evolution of the space-dependent mass distribution of galaxies in clusters due to binary aggregations by solving a space-dependent Smoluchowski equation. We derive the distribution of intergalactic distance for different ranges of mass (and of corresponding magnitude). We compare the results with the observed distributions, and find that the different degrees of luminosity segregation observed in clusters are well accounted for by our merging model. In addition, the presence of luminosity segregation is related to dynamical effects which also show up in different but connected observables, such as galaxy velocity profiles decreasing toward the center and X-ray measured beta-parameters smaller than 1. We predict both luminosity segregation and the observables above (being a product of binary aggregations) to be inversely correlated with the core radius and with the galaxy velocity dispersion; we discuss how the whole set of predictions compares with up-to-date observations.
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Galaxy mergers are key events in galaxy evolution, often causing massive starbursts and fueling active galactic nuclei (AGN). In these highly dynamic systems, it is not yet precisely known how much starbursts and AGN respectively contribute to the total luminosity, at what interaction stages they occur, and how long they persist. Here we estimate the fraction of the bolometric infrared (IR) luminosity that can be attributed to AGN by measuring and modeling the full ultraviolet to far-infrared spectral energy distributions (SEDs) in up to 33 broad bands for 24 merging galaxies with the Code for Investigating Galaxy Emission. In addition to a sample of 12 confirmed AGN in late-stage mergers, found in the $Infrared$ $Array$ $Satellite$ Revised Bright Galaxy Sample or Faint Source Catalog, our sample includes a comparison sample of 12 galaxy mergers from the $Spitzer$ Interacting Galaxies Survey, mostly early-stage. We perform identical SED modeling of simulated mergers to validate our methods, and we supplement the SED data with mid-IR spectra of diagnostic lines obtained with $Spitzer$ InfraRed Spectrograph. The estimated AGN contributions to the IR luminosities vary from system to system from 0% up to 91% but are significantly greater in the later-stage, more luminous mergers, consistent with what is known about galaxy evolution and AGN triggering.
The study of cluster populations as tracer of galaxy evolution is now quite possible with 8 m class telescopes and modern instrumentation. The cluster population can be used as a good tracer of the star forming episodes undergone by the merging system. We present two young galaxies mergers NGC3256 and NGC4038, and the studies about the young cluster population on those system. We found that the clusters ages are agree with the mergers age and their metallicities are consistent with them being the progenitors of the old metal rich globulars in ellipticals.
The relative average minimum projected separations of star clusters in the Legacy ExtraGalactic UV Survey (LEGUS) and in tidal dwarfs around the interacting galaxy NGC 5291 are determined as a function of cluster mass to look for cluster-cluster mass segregation. Class 2 and 3 LEGUS clusters, which have a more irregular internal structure than the compact and symmetric class 1 clusters, are found to be mass segregated in low mass galaxies, which means that the more massive clusters are systematically bunched together compared to the lower mass clusters. This mass segregation is not present in high-mass galaxies nor for class 1 clusters. We consider possible causes for this segregation including differences in cluster formation and scattering in the shallow gravitational potentials of low mass galaxies.
The Rees-Sciama effect produced in mergers of galaxy clusters is discussed, and an analytical approximation to compute this effect from numerical simulations is given. Using this approximation and a novel toy model describing the physics of the merger, we characterize the spatial properties and symmetries of the Rees-Sciama signal. Based on these properties, we propose a method to extract the physical parameters of the merger, which relies on the computation of the quadrupole moment of the observed brightness distribution on the sky. The relationships between the quadrupole coefficients and the physical parameters of the merger (physical separation, projection angle on the sky and angular momentum) are discussed. Finally, we propose a method to co-add coherently the RS signals from a sample of cluster mergers, in order to achieve an statistical detection of the effect for those cases where individual signals are masked by the kinetic SZ effect, the primordial CMB components, and by observational noise.
We present an observational analysis of numerical simulations of galaxy cluster mergers. We identify several observational signatures of recent merger activity, and quantitatively assess the uncertainty introduced into cluster mass estimates when invoking the commonly held assumptions of hydrostatic equilibrium, virial equilibrium, spherical symmetry and isothermality. We find that mergers result in multiple X-ray peaks, long-lived elongation of the X-ray emission as well as isophotal twisting and centroid shifting to a degree consistent with recent observations. We also find an enlargement of the X-ray core relative to the dark matter core. Mergers result in non-isothermal clusters exhibiting observable inhomogeneities in the emission-weighted X-ray temperature of several keV on linear scales of less than 0.5 Mpc. The resulting gas dynamics are extremely complex, and we present an example of what might be observed by a high resolution X-ray spectrograph. We further speculate that the gas dynamics, via shocks, bulk flows and turbulence, play an important role in the evolution of cluster galaxies and associated radio sources, particularly wide-angle tailed (WAT) sources and radio halos. We find that X-ray based by cluster mass estimates made under equilibrium assumptions can be uncertain 50% or more in the first 2 Gyrs after a merger and by up to 25% after 2 Gyrs depending on the details of the analysis and projection effects. Uncertainties can be considerably larger if the temperature is not well constrained.
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