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Marylee Guffy
This paper summarizes studies of the mass and galaxy distribution in and around four massive galaxy clusters. It is the first paper that made use of data from the Dark Energy Survey, taken during an initial testing phase called Science Verification that lasted from September 2012 to February 2013. Not only does this paper present new research into clusters, but it provides important early tests of data delivered by the Dark Energy Camera (DECam) and data analysis methods used by the Dark Energy Survey.
Task Force Aurora is divided into three projects: Project Aurora, Project Basilisk and Project Scarab. Each project has three different goals; Aurora oversees the full extent of the research and conducts the bulk of the research aggregation, Basilisk follows up on leads across the galaxy at large, Scarab goes to sites verified by Basilisk to conduct deeper field research.
Gravitational lensing occurs because the trajectory of photons from a distant object is deflected while passing through the gravitational field of a less-distant massive object along the line of sight with the observer. We call the more distant object a "source" and the less-distant object a "lens." If the source, the lens, and the observer are sufficiently separated and collinear, and if the mass of the lens is sufficiently large, then the apparent shape of the source can be noticeably distorted. Indeed, the source can appear as an extended arc or ring or even appear multiple times around the lens. This effect is called "strong" gravitational lensing.
For each system, we measure an average radius of the source images, with respect to the primary lens. The uncertainty on the mean is drawn from the standard deviation on the mean, summed in quadrature with the pixel scale of DES, 0263. The pixel scale represents the resolution of DES images, which we use as a minimum uncertainty. The average radius of source images is an approximation for the Einstein radius, and is identical to that when the true source position is directly behind the lens. The image separation distribution is sensitive to a number of inputs such as the halo mass, the lens mass distribution, and the source redshift. It therefore contains information about the cosmological parameters and various scaling relations between galaxy properties and halo mass and can be measured from galaxy to cluster scales (Oguri 2006; More et al. 2016). Figure 18 is the distribution of the radii.
Based on the symmetric quantum physics [1], this paper explicates the general correlations developing between the variety of host galaxies and the core black holes in the post-inflation big bang. This is the culminate unraveling for the current preoccupation; its special case, among others, explains the observationally purported mass correlation between the core black hole mass, Mb, and the host elliptical galaxy mass, Mg, in the approximation [2],
A dearth of intermediate black holes is found from the mass to the mass [5]; to overleap such a large gap, impossible O(1,000) simultaneous black hole mergers would in effect be required. Moreover, black holes of mass range 2 (109-1010) have also been found in the dawn of time [6,7]. Obviously, the standard theories have no systematic mechanism that could create such behemoth black holes from the foot-loose matters in the open early Universe [8], giving support to the direct collapses, rather than the alleged mergers, for their formations.
The predicted mini-sized primordial quark black hole [30] has never been realized. However, the observation of the dark dwarf galaxy of mass indicates that the post-inflation big-bang dynamics according to Figure 1 may become amenable to the black hole formations of around [31, 32] with excessive. This explains why the black holes of mass along the dwarf galaxies of mass with overabundant, emerge after their incipient stage absence. The black holes of b > 105 [in f > fl, crit] along the dwarf galaxies then follow with gradually decreasing rdm. With the time increasing to, a likely critical value, b increases and, through the super-massive black holes, the ultra-massive black holes of would in principle be realized with correspondingly large host galaxies in mass correlation, but with much lower.
What really happens in the post-inflation big-bang, however, might not be that simple and categorical as projected above. The increasing number of large galaxy-black hole duos would disturb the post-inflation big-bang ambiance for, and gradually subdue their additional autonomous formations. The galaxy-black hole duo production efficiency then could peak, say, around (or), building up to it from (or), then tapering off from it toward (or). It is possible that some additionally heavier duos might have been produced via mergers of those autonomous duos. Because the Equation (13) is independent of b, the mergers of the duos that increase their size would maintain their indigenous mass correlation ratio. This guarantees the realization of the observed super-massive and ultra-massive black holes in the early Universe [6,7].
The implosions at the extreme high densities , , in the earlier part of this duration (perhaps, around f -1.5) would be so powerful that the impending galaxy portion could be swept away with the incipient core black hole in the upheaval disarranging to form the globular clusters, the comparatively simple, yet very poorly understood phenomenon in the standard theory. This solves the mystery of why the globular clusters, really the wrecks of inchoate (visible matter) black holes, do not contain much dark matter [33,34] , emerging with high density visible matter. Moreover, the globular clusters that stopped short of becoming the black hole before the formation of the dark dwarf galaxies with black hole mass of, would have (see Figure 1) total visible masses in the range of (105 - 104) as so in fact observed [35].
With d 1, the galaxies would be primarily elliptical [41] to give the special mass correlation of Equation (1). The correlations would be generalized with the inclusive that embraces all possible situation in the post-inflation big-bang. For d > 1, likely during the later period in the big-bang, the ratio Mg/Mb in Table 1 is very sensitive to the modification in d, indicating that a small local tweak in in the big-bang turmoil could reduce Mg/Mb by a large ratio. This trend might be enhanced because, with a weaker Fpull/Fpush, the enfolding of the matter to the galaxy would be weakened. This dumbfounding prediction has been verified by the observations of the unusually small Mg/Mb 30 [42] as well as the super-massive black holes in the small galaxies [43].
During the earlier period in the post-inflation big-bang when the black hole size was relatively small, a reduction in d could also have made a sensitive change in the culminating spiral galaxy configurations. The galaxy bulges here are generated mostly by the visible matter portion inside the filing column of radius Rb that moves toward the core parallel to the rotational axis. The bulge size, Mg,bulge, would thus be only a portion of the galaxy mass Mg. Because the increased centrifugal force would push the matter outwards, the Mg,bulge may become prostrated as the galaxy rotational velocity increases, and the spiral galaxy with modest bulges could be formed with certain mid-weight black holes.
The dark and regular dwarf galaxies with very high initial dark matter densities may still loiter in. As a dwarf galaxy in encounters another galaxy, however, the dark matter in it may suffer a sudden dispersion, switching over to satisfy the condition Equation (19). The dwarf galaxy then lights up in starburst. This might be how the Messier 82 shines even though it is relatively puny in both size and mass compared to its big partner Messier 81 [52].
On the other hand, the predictions by symmetric quantum physics of the Universe [1] have been verified by the observation of the massive galaxies in the fog of time and distance in the primordial Universe, seemingly formed quickly but surprisingly peacefully, without having to invoke much violent mergers and galaxy interactions [65]. And the bountiful dark matter and energy of Equation (8) could again be the viable rejoinder for the governing dynamics in the primordial Universe.
We analyze the Michelson type experiment performed by Brillet and Hall. The order of magnitude of the gravitational effect (a beating frequency between two lasers) is calculated. We prove that Newtonian tidal forces could be observed when they originate from the oblateness of the Earth, from its rotation, from local masses, from the Moon or the Sun but not from the Galaxy (contrary to what has been recently claimed). We conclude that it is important to build a new parametrized theoretical framework for the analysis of high-precision experiments.
Water vapor masers have been detected in over 150 galaxies, most of them with active nuclei. In at least 20 percent of megamasers, the emission originates in an edge-on, circumnuclear disk surrounding the AGN. Spectacular VLBI observations show these megamasers in Keplerian rotation within a parsec of the dynamical center of the galaxy. Megamasers provide gold-standard masses of supermassive black holes, and in some cases we can use the masers to measure geometric distances to the host galaxies. The megamaser distance to NGC 4258 provides a fundamental anchor for the extragalactic distance scale. Other megamaser galaxies measure H_0 directly. In this talk I will describe the method and latest results from measurements of maser distances to galaxies.
Quantifying how the gas content varies with star formation and structural properties of galaxies is of paramount importance for constraining models of galaxy formation. Equally important is to perform such studies on large and unbiased samples of galaxies, in order to obtain results that are truly representative of the local population. The ongoing GALEX Arecibo SDSS Survey (GASS) is designed to provide such a representative sample for massive galaxies, with the aim of understanding the role played by gas in the transition between blue, star-forming galaxies and red, passively-evolving systems.
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