Cosmic Temperature Research Articles

Cosmic ray flux variations and their correlation with the global temperatures of the Earth’s troposphere and stratosphere in the 23rd and 24th solar cycles (2002–2014)

The mutual correlation between cosmic ray flux variations and average daily global temperatures of various layers of the troposphere and stratosphere of the Earth in the period from the second half of the 23rd cycle of solar activity until recently with values ranging from −0.21 to −0.5, depending on the altitude above the Earth’s surface, is studied. A method for plotting a combined spectral periodogram is used to examine the temporal structure of the above data and to identify common groups of quasi-harmonic components with periods ranging from several days to six months.

On the evolving and emitting quantum black holes and the scale independent black hole cosmology

Along with presently the believed black holes that are expected to be formed by gravitational collapse of a massive star, there may exist primordial evolving black holes. By absorbing the hidden vacuum energy primordial evolving black holes become massive. Planck mass can be considered as the basic mass of any black hole and can be called as the baby Planckion. Very high temperature of the baby Planckion is the only heat source for the evolving black holes or evolving Planckion’s decreasing temperature. Considering the current cosmic microwave back ground temperature as a quantum gravitational effect of the evolving primordial cosmic black hole, general theory of relativity and quantum mechanics can be combined into a ‘scale independent’ true unified model of quantum gravity. Considering cosmic black hole’s light speed rotation and galactic revolution, observed galactic rotational curves can be understood. In the past, decreasing high cosmic black hole temperature forced hydrogen atom to emit increasing photon energy resulting in the observed redshift. Aged super novae dimming may be due to the effect of past high cosmic black hole temperature. As cosmic time passes, decreasing current cosmic black hole temperature makes hydrogen atom to emit increased quanta of energy causing the future redshift. In future, with reference to the laboratory hydrogen atom, decreasing current cosmic temperature and measured rate of increase in emitted photon energy - true rate of future cosmic expansion can be understood. With reference to the decreasing current Hubble constant and decreasing current cosmic black hole temperature, true rate of future cosmic expansion can also be understood. Foundations of Quantum mechanics and General theory of relativity may be reviewed in this unified way. Keywords: Quantum Gravity, Evolving Black Holes, Geometric Horizon, Standard Cosmology, Black Hole Cosmology, CMBR Isotropy and Anisotropy, Redshift, Galactic Rotational Curves.

Cosmology with Planck

The European Space Agency (hereafter ESA) Planck satellite was launched on May 2009 and has been surveying the microwave and the submillimeter sky since August 2009. In March 2013, ESA and the Planck Collaboration publicly released the initial cosmology products based on the first 15.5 months of Planck operations. In this contribution we present the first cosmological results based on Planck measurements of the Cosmic Microwave Radiation temperature and lensing-potential power spectra. The Planck spectra at high multipoles are well described by the standard Lambda Cold Dark Matter (?CDM) cosmological model based on six parameters. We find a low value of the Hubble parameter, H 0 = 67.3 ± 1.2 km/s/Mpc, and, consequently, an high value of the matter parameter density Ω m = 0.315±0.017 (±1σ errors), in agreement with the measurements of baryon acoustic oscillation (BAO) surveys. We also present results from several possible extensions of the standard cosmological model, by using astrophysical datasets in addition to the Planck data. None of these models are favored significantly over the standard ?CDM. Using BAO and CMB data, we find N eff = 3.30 ± 0.27 for the effective number of relativistic degrees of freedom, and an upper limit of 0.25 eV for the summed neutrino mass.

Basics of the decelerating black hole universe

Throughout the cosmic evolution, currently believed cosmic ‘critical density’ can be shown to be a default result of the ‘positively curved’ light speed rotating black hole universe ‘volume density’. As there is no observational or experimental evidence to Friedmann’s second assumption, the density classification scheme of Friedmann cosmology must be reviewed at fundamental level and possibly can be relinquished. The observed cosmic redshift can be reinterpreted as an index of ‘cosmological’ thermodynamic light emission mechanism. Clearly speaking during cosmic evolution, at any time in the past, in hydrogen atomemitted photon energy was always inversely proportional to the cosmic temperature. Thus past light emitted from older galaxy’s excited hydrogen atom will show redshift with reference to the current laboratory data. Note that there will be no change in the energy of the emitted photon during its journey from the distant galaxy to the observer. In no way ‘redshift’ seems to be connected with ‘galaxy receding’. By considering the ‘Stoney mass’ as the initial mass of the baby cosmic black hole, past and current physical and thermal parameters (like angular velocity, growth rate, age, redshift, thermal energy density and matter density) of the cosmic black hole can be understood. For a cosmic temperature of 3000 K, obtained redshift is 1100. From now onwards, CMBR temperature can be called as ‘Comic Black Hole’s Thermal Radiation’ temperature and can be expressed as ‘CBHTR’ temperature. Current cosmic black hole is growing at a rate of 14.66 km/sec in a decelerating mode. Uncertainty relation and all other microscopic physical constants play a crucial role in understanding the halt of the present cosmic expansion. In view of the confirmed zero rate of change in inverse of the Fine structure ratio (from the ground based laboratory experimental results), zero rate of change in the current CMBR temperature (from satellite data) and zero rate of change in the current Hubble’s constant (from satellite data), it can be suggested that, current cosmic expansion is almost all saturated and at present there is no significant cosmic acceleration.

Cool start to hydrogen ionization

Simulations of the cosmos cast doubt on assumptions about the temperature of primordial hydrogen gas when it was ionized by the first stars and galaxies, complicating the interpretation of ongoing observations. See Letter p.197 The epoch of reionization was a one during which the neutral gas of the 'dark age' Universe became an ionized plasma. Simulations suggest that the 21-cm spectral transition of atomic hydrogen will show a clear fluctuation peak at a redshift and scale that mark the central stage of reionization. This prediction is based on the assumption that heating of the cosmic gas, which occurs before reionization, is caused by stellar remnants (particularly X-ray binaries) and reaches temperatures well above the cosmic microwave background of the time (30 kelvin). However, Rennan Barkana and colleagues report that the hard spectra of X-ray binaries (with more high-energy than low-energy photons) make such heating ineffective, resulting in a delayed and spatially uniform heating. In this new model, the 21-cm signature of reionization is modified to a more complex signal with a distinct minimum temperature (below 1 millikelvin) that marks the rise of the cosmic mean gas temperature above the microwave background.

Cosmic Redshift, Temperature, Growth Rate and Age in Stoney Scale Black Hole Cosmology

Throughout the cosmic evolution, currently believed cosmic “critical density” can be shown to be a default result of the “positively curved” light speed rotating black hole universe “mass density”. As there is no observational or experimental evidence to Friedmann’s second assumption, the density classification scheme of Friedmann cosmology must be reviewed at fundamental level and possibly can be relinquished. With cosmic light speed rotation galactic rotational curves can be understood. The observed cosmic redshift can be reinterpreted as an index of “cosmological” thermodynamic light emission mechanism. Clearly speaking during cosmic evolution, at any time in the past, in hydrogen atom—emitted photon energy was always inversely proportional to the cosmic temperature. Thus past light emitted from older galaxy’s excited hydrogen atom will show redshift with reference to the current laboratory data. Note that there will be no change in the energy of the emitted photon during its journey from the distant galaxy to the observer. Past high cosmic temperature may be the root cause of observed super novae dimming. By considering the “Stoney mass” as the initial mass of the baby cosmic black hole, past and current physical and thermal parameters (like angular velocity, growth rate, age, redshift, thermal energy density and matter density) of the cosmic black hole can be understood. For a past cosmic temperature of 3000 K, obtained redshift is 1100. From now onwards, CMBR temperature can be called as “Comic Black Hole’s Thermal Radiation” temperature and can be expressed as “CBHTR” temperature. Current cosmic black hole is growing at a rate of 14.66 km/sec in a decelerating mode. In view of the confirmed zero rate of change, the current CMBR temperature (from satellite data) and zero rate of change in the current Hubble’s constant (from satellite data), it can be suggested that, current cosmic expansion is almost all saturated and at present there is no significant cosmic acceleration. From microscopic physics point of view, can be considered as a true index of future cosmic rate of expansion.

Cosmic ray measurement and experimental temperature analysis with a muon detector

The Basic Atomic Energy Research Institute (BAERI) of Hanyang University in Korea constructed and operates a cosmic ray detection system. In this study, a muon detector composed of a plastic scintillator and a wavelength shifter was used to obtain data over a total of six experimental periods. Using the collected data, we analyzed the response dependence of the developed muon detector on the laboratory’s environmental temperature. The detection results showed a correlation coefficient of over 0.7, as well as a negative proportional correlation in the experiments in which the thermostat did not operate. We performed a correction for the laboratory’s environmental temperature and analyzed the correlation between the muon count rate and the atmospheric pressure. As a result, we obtained a barometric coefficient of −0.1191 ± 0.0054%/hPa. The analyzed data were compared with data from the eighteen NM64 type neutron monitors at our station. The correlation coefficient between the two detection systems was approximately 0.8046, confirming that the response changes were roughly identical to response of neutron monitors.

Reconstruction of internal gravity wave parameters from radio occultation retrievals of vertical temperature profiles in the Earth's atmosphere

Abstract. A new method for the reconstruction of internal gravity wave (IGW) parameters from a single vertical temperature profile measurement in the Earth's atmosphere has been developed. This method does not require any additional information not contained in the profile and may be used for the analysis of profiles measured by various techniques. The criterion for the IGW identification has been formulated and argued. In the case when this criterion is satisfied, then analyzed temperature fluctuations can be considered as wave-induced. The method is based on the analysis of relative amplitude thresholds of the temperature wave field and on the linear IGW saturation theory in which amplitude thresholds are restricted by dynamical (shear) instability processes in the atmosphere. When the amplitude of an internal gravity wave reaches the shear instability limit, energy is assumed to be dissipated in such a way that the amplitude is maintained at the instability limit as the wave propagates upwards. In order to approbate the method we have used data of simultaneous high-resolution balloon measurements of the temperature and wind velocity in the Earth's stratosphere over France where a long-period inertia-gravity wave has been detected. Using the radiosonde temperature data only, we have reconstructed all wave parameters, which were determined by radiosondes, with relative deviations not larger than 30%. An application of the method to the radio occultation (RO) data has given the possibility to identify the IGWs in the Earth's stratosphere and to determine the magnitudes of key wave parameters such as the intrinsic frequency, amplitudes of vertical and horizontal perturbations of the wind velocity, vertical and horizontal wavelengths, intrinsic vertical and horizontal phase (and group) speeds, kinetic and potential energy, vertical fluxes of the wave energy and horizontal momentum. The obtained results of internal wave studies in the Earth's stratosphere deduced from the COSMIC and CHAMP GPS occultation temperature profiles are presented and discussed.

Investigation of Kelvin Waves in the Stratosphere Using FORMOSAT-3/COSMIC Temperature Data

Temperature data from Global Positioning System based Radio Occultation (GPS RO) soundings of the Formosa Satellite mission 3/Constellation Observing System for Meteorology, Ionosphere, and Climate (FORMOSAT-3/COSMIC or F-3/C) micro satellites has been investigated in detail to study the Kelvin wave properties. The high temporal and spatial resolution satellite data from August 2006 to August 2009 have enabled the investigation of Kelvin wave activity on each day. The dominant waves of wave numbers 1 and 2 (W1 and W2) have been investigated in detail at three altitudes—19, 25 and 30 km, and it is found that the amplitude of W1 is greater than that of W2 during 60% of the time. A statistical study of the amplitudes of W1 and W2 is also presented and it is found that the dominant amplitudes are 0.5 to 1.0 K for both waves. At lower altitudes (19 km), the amplitudes of W1 are larger and the distribution is also broader. The amplitudes of both waves in the stratosphere are higher during the easterlies of the quasi-biennial oscillation (QBO) and are maximum when the zonal wind changes from easterlies to westerlies. In the lower altitudes near the tropopause they vary in consonance with the outgoing long wave radiation, a proxy of deep convection. Deduction of the Kelvin wave periods and phase velocities has been possible with better accuracy with the use of the F-3/C data. The average periods of W1 for all years are 15 ± 3, 13 ± 4, and 10 ± 3 days at altitudes 19, 25, and 30 km, respectively and the average periods of W2 for all years are 10 ± 2, 7 ± 2, and 6 ± 2 days, respectively. These standard deviations are geophysical and are due to the variation in the periods of the individual Kelvin wave events and identification of the period for a single Kelvin wave event is correct to within ± one day. We found that the Kelvin waves of both the zonal wave numbers are slow in the lower altitudes and fast in the higher altitudes. Also, the periods decrease gradually with height. This is the most important result of the present study.

SPEEDING THE FRIEDMANN EXPANSION BY CHIRAL TENSOR PARTICLES

The status of the chiral tensor particles in the extended electroweak model, their experimental constraints, signatures and the possibilities for their detection at the new colliders are shortly reviewed. The cosmological effects of the additional particles are discussed. Namely, their characteristic interactions with the other components of the early Universe plasma and the corresponding cosmic times and temperatures are determined. The dynamical cosmological effect, namely the speeding of the Friedmann expansion due to the density increase caused by the chiral tensor particles and the additional Higgs doublet is discussed. The presence of the chiral tensor particles is allowed from cosmological considerations and welcomed by the particle physics phenomenology.

A SIMPLIFIED TOP DOWN MODEL FOR COSMIC RAY PARTICLE PRODUCTION

We investigate the implications of a minimal top down model on cosmic ray particle production from super heavy vector boson annihilation with subsequent pseudo-scalar boson decay. Super heavy particles are assumed to exist according to a homogeneous distribution. Besides the particle production via decay, the thermal momentum distribution of the initial state as well as expansion effects and cosmic temperature corrections are considered in the context of a Friedmann–Robertson–Walker universe.

Can oscillating scalar fields decay into particles with a large thermal mass?

We calculate the dissipation rate of a coherently oscillating scalar field in a thermal environment using nonequilibrium quantum field theory and apply it to the reheating stage after cosmic inflation. It is shown that the rate is nonvanishing even when particles coupled to the oscillating inflaton field have a larger thermal mass than it, and therefore the cosmic temperature can be much higher than inflaton's mass even in the absence of preheating. Its cosmological implications are also discussed.

CMB spectrum in Cardassian models

Department of Physics, University of Oslo, N-0316 Oslo, Norway(Dated: February 2, 2008)The dark energy in the Universe is described in the context of modified Friedmann equations asa fluid parameterized by the density of dark matter and undergoing an adiabatic expansion. Thisformulation is applied to the Cardassian model. Choosing then parameters consistent with the su-pernova observations, it gives a background expansion in which the cosmic temperature fluctuationsare calculated. The resulting spectrum is quite similar to what is obtained in the standard concor-dance model. If the Cardassian fluid is interpreted as a new kind of interacting dark matter, itsoverdensities are driven into oscillations when the interaction energy is rising in importance. Thisdoes not occur in a description of the Cardassian fluctuations motivated by theories of modifiedgravity. There the energy of the underlying matter is also conserved, which requires appearance ofeffective shear stress in the late Universe. In both approaches that allow fluctuations the thermalpower spectrum at large scales is much too strongly enhanced by the late integrated Sachs-Wolfeeffect. With the interacting dark matter assumption, we conclude that the Cardassian model isruled out by observations, expect in a small neighbourhood of the ΛCDM limit.Introduction

Evolution of cosmic magnetic fields: From the very early Universe, to recombination, to the present

A detailed numerical and analytical examination of the evolution of stochastic magnetic fields between a putative magnetogenesis era at high cosmic temperatures $T\ensuremath{\sim}100\text{ }\mathrm{M}\mathrm{e}\mathrm{V}--100\text{ }\mathrm{G}\mathrm{e}\mathrm{V}$ and the present epoch is presented. The analysis includes all relevant dissipation processes, such as neutrino- and photon-induced fluid viscosities as well as ambipolar and hydrogen diffusion. A simple and intuitive analytical model matching the results of the three-dimensional MHD simulations allows for the prediction of prerecombination and present day magnetic field correlation lengths and energy densities as a function of initial magnetic field energy density, helicity, and spectral index. Our conclusions are multifold. (a) Initial primordial fields with only a small amount of helicity are evolving into maximally helical fields at the present. Furthermore, the simulations show a self-similarity in the evolution of maximally helical fields implying a seemingly acausual amplification of magnetic fields on large scales is observed. (b) There exists a correlation between the strength of the magnetic field $B$ at the peak of its spectrum and the location of the peak, given at the present epoch by $B\ensuremath{\approx}5\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}12}\text{ }\mathrm{G}(L/\mathrm{k}\mathrm{p}\mathrm{c})$, where $L$ is the magnetic field correlation length determined by the initial properties of the magnetic field. (c) Concerning studies of the generation of cosmic microwave background (CMBR) anisotropies due to primordial magnetic fields of $B\ensuremath{\sim}{10}^{\ensuremath{-}9}\text{ }\mathrm{G}$ on $\ensuremath{\gtrsim}10\text{ }\mathrm{M}\mathrm{p}\mathrm{c}$ scales, such fields are not only impossible to generate in early causal magnetogenesis scenarios but also seemingly ruled out by distortions of the CMBR spectrum due to magnetic field dissipation on smaller scales and the overproduction of cluster-magnetic fields. (d) The most promising detection possibility of CMBR distortions due to primordial magnetic fields may be on much smaller scales at higher multipoles $l\ensuremath{\sim}{10}^{6}$ where the signal is predicted to be the strongest. (e) It seems possible that magnetic fields in clusters of galaxies are entirely of primordial origin, without invoking dynamo amplification. Such fields would be of (precollapse) strength ${10}^{\ensuremath{-}12}--{10}^{\ensuremath{-}11}\text{ }\mathrm{G}$ with correlation lengths in the kpc range and would also exist in voids of galaxies.

Cosmological Relativity: A New Theory ofCosmology1

A new general-relativistic theory of cosmology, the dynamical variables of whichare those of Hubble's, namely distances and redshifts, is presented. The theorydescribes the universe as having a three-phase evolution with a deceleratingexpansion followed by a constant and an accelerating expansion, and it predictsthat the universe is now in the latter phase. The theory is actually a generalizationof Hubble's law taking gravity into account by means of Einstein's theory ofgeneral relativity. The equations obtained for the universe expansion are elegantand very simple. It is shown, assuming Ω0 = 0.24, that the time at which theuniverse goes over from a decelerating to an accelerating expansion, i.e., theconstant expansion phase, occurs at 0.03 τ from the big bang, where τ is theHubble time in vacuum. Also, at that time the cosmic radiation temperature was11 K. Recent observations of distant supernovae imply, in defiance of expectations,that the universe's growth is accelerating, contrary to what has always beenassumed, that the expansion is slowing down due to gravity. Our theory confirmsthese recent experimental results by showing that the universe now is definitelyin a stage of accelerating expansion.

Breaking Degeneracy of Dark Matter Models by the Scale‐Scale Correlations of Galaxies

Recently, scale-scale correlations have been detected in the distributions of quasars' Lyα absorption lines and the maps of cosmic temperature fluctuations. This paper investigates the scale-scale correlations in galaxy distributions. Using samples of mass field given by N-body simulation, we first show that the scale-scale correlation of two-dimensional and three-dimensional mass distributions at present day are capable of breaking the degeneracy between the SCDM (standard cold dark matter model) and OCDM (open CDM model) or LCDM (flat CDM model) and even show the difference between the OCDM and LCDM. Using biased galaxy samples produced in an appropriate bias model, we show that the scale-scale correlation of galaxy distribution at zero redshift is still a powerful tool to break the degeneracy in the parameter space, including both cosmological and biasing parameters. We analyze the scale-scale correlations of the APM bright galaxy catalog and compare it with the mock catalog in the SCDM, OCDM, and LCDM models. We find that all the spectra of local and nonlocal scale-scale correlations predicted by the OCDM model are in excellent agreement with those of the APM-BGC sample, while the SCDM and LCDM mock catalog appear to have somewhat weaker scale-scale correlations than the observation.

The COBE-DMR database and how to use it

The anisotropy experiment on board the Cosmic Background Explorer has produced six sky maps of the cosmic microwave temperature at three frequencies: 31.5, 53 and 90 GHz. These data have been the bases for the discovery of the expected anisotropies ΔT/T = 1.6 × 10−5 left as a signature of primordial density fluctuations at an early hot epoch of the universe. The National Space Science Data Center (NSSDC) has made two releases of COBE-DMR data. A description of these data products and their structure is presented.

Thermally induced density perturbations in the inflation era.

The possibility of thermally induced initial density perturbations in inflationary cosmology is examined. The fluctuation dynamics of a scalar field plus thermal bath system during slow roll is described by a Langevin-like equation. Fluctuation-dissipation arguments show that for a wide parameter range within the standard inflation model, the thermal fluctuations of the scalar field can dominate its quantum fluctuations. The initial amplitude of density perturbations is found to lie in a range which is consistent with the recent observations of cosmic temperature fluctuations.

An infrared cutoff revealed by the two years of COBE observations of cosmic temperature fluctuations.

We show that a good fitting to the first two years of observations by the Cosmic Background Explorer Differential Microwave Radiometers of the two-point angular correlation function of cosmic background radiation (CBR) temperature is given by models with a nonzero infrared cutoff ${k}_{min}$ in the spectrum of the primordial density perturbations. If this cutoff comes from the finiteness of the universe, say, a topological T3 model, we find ${k}_{min}\ensuremath{\sim}(0.3\ensuremath{-}1.1)\ensuremath{\pi}\frac{{\mathrm{H}}_{0}}{c}$ with confidence level 95%. Such a nonzero ${k}_{min}$ universe would also give a better match to the observations both of the rms quadrupole anisotropy of CBR and of galaxy clustering.

Cosmic temperature fluctuations from two years of COBE differential microwave radiometers observations

view Abstract Citations (300) References (73) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Cosmic Temperature Fluctuations from Two Years of COBE Differential Microwave Radiometers Observations Bennett, C. L. ; Kogut, A. ; Hinshaw, G. ; Banday, A. J. ; Wright, E. L. ; Gorski, K. M. ; Wilkinson, D. T. ; Weiss, R. ; Smoot, G. F. ; Meyer, S. S. ; Mather, J. C. ; Lubin, P. ; Loewenstein, K. ; Lineweaver, C. ; Keegstra, P. ; Kaita, E. ; Jackson, P. D. ; Cheng, E. S. Abstract The first two years of COBE DMR observations of the CMB anisotropy are analyzed and compared with our previously published first year results. The results are consistent, but the addition of the second year of data increases the precision and accuracy of the detected CMB temperature fluctuations. The two-year 53 GHz data are characterized by RMS temperature fluctuations of DT=44+/-7 uK at 7 degrees and DT=30.5+/-2.7 uK at 10 degrees angular resolution. The 53X90 GHz cross-correlation amplitude at zero lag is C(0)^{1/2}=36+/-5 uK (68%CL) for the unsmoothed 7 degree DMR data. A likelihood analysis of the cross correlation function, including the quadrupole anisotropy, gives a most likely quadrupole-normalized amplitude Q_{rms-PS}=12.4^{+5.2}_{-3.3} uK (68% CL) and a spectral index n=1.59^{+0.49}_{-0.55} for a power law model of initial density fluctuations, P(k)~k^n. With n fixed to 1.0 the most likely amplitude is 17.4 +/-1.5 uK (68% CL). Excluding the quadrupole anisotropy we find Q_{rms-PS}= 16.0^{+7.5}_{-5.2} uK (68% CL), n=1.21^{+0.60}_{-0.55}, and, with n fixed to 1.0 the most likely amplitude is 18.2+/-1.6 uK (68% CL). Monte Carlo simulations indicate that these derived estimates of n may be biased by ~+0.3 (with the observed low value of the quadrupole included in the analysis) and {}~+0.1 (with the quadrupole excluded). Thus the most likely bias-corrected estimate of n is between 1.1 and 1.3. Our best estimate of the dipole from the two-year DMR data is 3.363+/-0.024 mK towards Galactic coordinates (l,b)= (264.4+/-0.2 degrees, +48.1+/-0.4 degrees), and our best estimate of the RMS quadrupole amplitude in our sky is 6+/-3 uK. Publication: The Astrophysical Journal Pub Date: December 1994 DOI: 10.1086/174918 arXiv: arXiv:astro-ph/9401012 Bibcode: 1994ApJ...436..423B Keywords: Background Radiation; Cosmology; Extraterrestrial Radio Waves; Microwaves; Radio Astronomy; Spaceborne Astronomy; Temperature Distribution; Universe; Anisotropy; Computerized Simulation; Cosmic Background Explorer Satellite; Microwave Radiometers; Monte Carlo Method; Astronomy; COSMOLOGY: COSMIC MICROWAVE BACKGROUND; COSMOLOGY: LARGE-SCALE STRUCTURE OF UNIVERSE; COSMOLOGY: OBSERVATIONS; Astrophysics E-Print: Accepted by the Astrophysical Journal. Modifications include the addition of a quadrupole- removed correlation function and an analysis of the technique bias on the power spectral index, n. The most likely, de-biased, estimate of n is between 1.1 and 1.3. 57 pages of uu-encoded postscript (incl 3 b&amp full text sources arXiv | ADS |