Search

We investigate the ‘Local Hole’, an anomalous underdensity in the local galaxy environment, by extending our previous galaxy K-band number-redshift and number-magnitude counts to ≈90 per cent of the sky. Our redshift samples are taken from the 2MASS Redshift Survey (2MRS) and the 2M++ catalogues, limited to K < 11.5. We find that both surveys are in good agreement, showing an $\approx 21\!-\!22{{\ \rm per\ cent}}$ underdensity at z < 0.075 when compared to our homogeneous counts model that assumes the same luminosity function (LF) and other parameters as in our earlier papers. Using the Two Micron All Sky Survey (2MASS) for n(K) galaxy counts, we measure an underdensity relative to this model of $20 \pm 2 {{\ \rm per\ cent}}$ at K < 11.5, which is consistent in both form and scale with the observed n(z) underdensity. To examine further the accuracy of the counts model, we compare its prediction for the fainter n(K) counts of the Galaxy and Mass Assembly (GAMA) survey. We further compare these data with a model assuming the parameters of a previous study where little evidence for the Local Hole was found. At 13 < K < 16, we find a significantly better fit for our galaxy counts model, arguing for our higher LF normalization. Although our implied underdensity of $\approx 20{{\ \rm per\ cent}}$ means local measurements of the Hubble Constant have been overestimated by ≈3 per cent, such a scale of underdensity is in tension with a global ΛCDM cosmology at an ≈3σ level.

(ABRIDGED) We present a power spectrum analysis of the 10K catalogue from the 2dF QSO Redshift Survey. We compare the redshift-space power spectra of QSOs to those measured for galaxies and Abell clusters at low redshift and find that they show similar shapes in their overlap range, 50-150h^{-1}Mpc, with P_QSO(k)\propto k^{-1.4}. The amplitude of the QSO power spectrum at z~1.4 is almost comparable to that of galaxies at the present day if Omega_m=0.3 and Omega_Lambda=0.7 (the Lambda cosmology), and a factor of ~3 lower if Omega_m=1 (the EdS cosmology) is assumed. The amplitude of the QSO power spectrum is a factor of ~10 lower than that measured for Abell clusters at the present day. At larger scales, the QSO power spectra continue to rise robustly to ~400 h^{-1}Mpc, implying more power at large scales than in the APM galaxy power spectrum measured by Baugh & Efstathiou. We split the QSO sample into two redshift bins and find little evolution in the amplitude of the power spectrum. The QSO power spectrum may show a spike feature at ~90h^{-1}Mpc assuming the Lambda cosmology or ~65 h^{-1}Mpc assuming an EdS cosmology. Although the spike appears to reproduce in both the North and South strips and in two independent redshift ranges, its statistical significance is still marginal and more data is needed to test further its reality. We compare the QSO power spectra to CDM models to obtain a constraint on the shape parameter, Gamma. For two choices of cosmology (Omega_m=1, Omega_Lambda=0 and Omega_m=0.3, Omega_Lambda=0.7), we find the best fit model has Gamma~0.1 +-0.1., MNRAS Accepted

We describe the scientific motivations, the mission concept and the instrumentation of SPACE, a class-M mission proposed for concept study at the first call of the ESA Cosmic-Vision 2015-2025 planning cycle. SPACE aims to produce the largest three-dimensional evolutionary map of the Universe over the past 10 billion years by taking near-IR spectra and measuring redshifts for more than half a billion galaxies at 0, Comment: 27 pages, Experimental Astronomy, in press. The SPACE team complete list is available at http://urania.bo.astro.it/cimatti/space . The article with full resolution figures is available at http://urania.bo.astro.it/cimatti/space/publications.htm

In 2004, as part of Ascension Health's "Healthcare That Is Safe" initiative, St. Vincent's Medical Center, as an alpha site, was charged with defining best practices to eliminate facility-acquired pressure ulcers. A comprehensive plan, including the "SKIN" (Surfaces, Keep the patients turning, Incontinence management, Nutrition) bundle, was developed.The incidence of pressure ulcers decreased from2% to1% from December 2004 through February 2006. No new Stage III or IV facility-acquired pressure ulcers occurred between August 2004 and February 2006. Weekly SKIN operations meetings and use of the SKIN process tool ensured that all at-risk patients were receiving appropriate interventions. REPORTING AND SPREAD: The alpha site work and SKIN bundle were presented to all 67 Ascension Health acute care facilities at a rapid-design-format Pressure Ulcer Summit in mid 2005. All acute care facilities agreed to a single model of care using the SKIN bundle and common measures of quality and performance.The St. Vincent's alpha site initiative in pressure ulcer prevention, enabled it to identify at-risk populations, implement appropriate actions, and achieve positive, measurable, meaningful results.The SKIN program was adopted and is being implemented throughout Ascension Health.

The results of radioecological investigations in the Syrdarya river basin in the Republic of Kazakhstan are presented. The work was carried out under the International Navruz Project. Nuclear activation analysis, X-ray fluorescence, and g-spectrometry were used to measure the element and radionuclide ( 137 Cs, 40 K and 238 U, 235 U, and 232 Th families) compositions of soil, water, bottom sediments and vegetation. Samples were collected at 15 control points in Kazakhstan along the Syrdarya river and its inflows during four expeditions (autumn 2000 and 2001, spring 2001 and 2002).

We have cross-correlated the WMAP data with several surveys of extragalactic sources and find evidence for temperature decrements associated with galaxy clusters and groups detected in the APM Galaxy Survey survey and the ACO catalogue. We interpret this as evidence for the thermal Sunyaev-Zeldovich (SZ) effect from the clusters. Most interestingly, the signal may extend to �1 deg (� 5h −1 Mpc) around both groups and clusters and we suggest that this may be due to hot ‘supercluster’ gas. We have further cross-correlated the WMAP data with clusters identified in the 2MASS galaxy catalogue and also find evidence for temperature decrements there. From the APM group data we estimate the mean Compton parameter as y(z 10 and then could seriously affect the WMAP cosmological fits.

X-ray luminous narrow emision-line galaxies (NELG) have been previously identified and proposed as an important class of extragalactic X-ray sources, with a potentially significant contribution to the total extragalactic X-ray flux at energies below $\sim$ 10 keV. In order to investigate and clarify this possibility, we have used a sample of NELG found in 5 deep ROSAT fields and similar samples belonging to the Cambridge-Cambridge ROSAT Serendipity Survey and to the {\it Einstein} Observatory Extended Medium Sensitivity Survey sample. The principal results of this investigation are as follows: a) for a given optical luminosity, the typical X-ray luminosity of NELGs is about one or two orders of magnitude higher than that of normal galaxies; b) the ratio of the surface density of NELGs compared with BLAGN increases from about 0.04 at fx >= 6 x 10^{-13} erg cm^{-2} s^{-1} to about 0.1 at fx >= 10^{-14} erg cm^{-2} s^{-1}, suggesting that the surface density of NL galaxies might be very close to that of BLAGN at fx ~ 10^{-15} erg cm^{-2} s^{-1}; c) we find that these objects are described by a cosmological evolution rate similar to that of soft X-ray selected BLAGN; d) the de-evolved (z=0) XLF of NELGs in the luminosity range 10^{41} - 5 x 10^{43} erg s^{-1} is steeper than the BLAGN (z=0) XLF in the same luminosity interval. Their spatial density is significantly lower than the spatial density of X-ray selected BLAGN at Lx(z=0) ~ 5 x 10^{43} erg s^{-1}, but this difference decreases at lower luminosities such that at Lx(z=0) < 10^{42} erg s^{-1} the spatial density of NELGs is very close to that of BLAGN. The implications of these results for the contribution of this class of objects to the cosmic X-ray background are discussed., To be published in M.N.R.A.S., 10 pages, 2 Tables. Figures are available in the anonymous ftp account on ftp://mds.pha.jhu.edu/pub/nl_paper

Observers studying the cosmology and evolutionary history of our Universe through the statistical properties of ‘normal’ galaxies have four main tools at their disposal. (1) The number-redshift relation. Although a very powerful diagnostic, spectroscopic surveys are currently limited to B < 24m and significantly incomplete in the range, 23m< B < 24m. (2) Galaxy number-magnitude counts. Although by themselves, they cannot constrain models as tightly as spectroscopy, they can be measured ∼ 4m fainter, where cosmological effects are expected to be significant. (3) Galaxy colours over a wide wavelength range, which provide additional constraints. (4) The dependence of galaxy clustering with magnitude. ω(θ) can be measured to the limit of the counts.Here we report on the latest Durham count and clustering work.

A number of 9-(hydroxyalkoxy) derivatives of guanine (27a-h and 27l-n) and of 8-methylguanine (27i-k) have been synthesized and evaluated as antiviral agents against herpes viruses (HSV-1, HSV-2, VZV) and visna virus, a lentivirus. The synthesis Involved reaction of hydroxyl-protected derivatives of hydroxyalkoxy-amines (6a-m) with 4,6-dichloro-2,5-diformamidopy-rimidine (24) followed by cyclization of the resultant 6-alkoxyaminopyrimidines (25a-m) to either guanine derivatives (27a-h and 27l-n) or 8-methylguanine derivatives (27i-k). Modest antiviral activity was seen with 27b, 27c, 27f, 27i and 271 against the herpesvirus and with 27e and 27m against visna virus. Only 27e showed any cytotoxicity in MRC-5 cells at concentrations ≤400μM.

Future short take-off and vertical landing (STOVL) concepts present unique design challenges. The flight control system designer must consider several issues including the control response type, the appropriate cockpit displays, and the control strategy for the flight and propulsion controls. Advanced STOVL concepts will have many force and moment generators. To be operationally effective such configurations need to have precise handling and control properties such that the pilot is not faced with an unacceptably high workload. The vectored thrust aircraft advanced flight control (VAAC) is a research programme which is addressing these issues. Its primary objective is to develop flight control and handling concepts which, when applied to future STOVL configurations, will provide good handling qualities with a low pilot workload. Four potential methods of controlling future STOVL aircraft are described and assessed with manned simulation and with the VAAC Harrier aircraft.

The angular two-point correlation function, ω(θ), for galaxies can be used as a probe of their redshift distribution N(z) and, therefore, of galaxy luminosity evolution. Without redshift data, we can still observe the projection onto the two-dimensional sky of the three-dimensional clustering of galaxies. The autocorrelation of this projected distribution is described by ω(θ). Observations have indicated that ω(θ) follows a θ−0.8 power-law (Peebles 1980) and that the index of the power-law remains approximately constant to the faintest limits of photographic surveys (Jones, Shanks & Fong 1987).

XMS is a multi-channel wide-field spectrograph designed for the prime focus of the 3.5m Calar-Alto telescope. The instrument is composed by four quadrants, each of which contains a spectrograph channel. An innovative mechanical design -at concept/preliminary stage- has been implemented to: 1) Minimize the separation between the channels to achieve maximal filling factor; 2) Cope with the very constraining space and mass overall requirements; 3) Achieve very tight alignment tolerances; 4) Provide lens self-centering under large temperature excursions; 5) Provide masks including 4000 slits (edges thinner than 100μ). An overview of this very challenging mechanical design is here presented.

In this review we first discuss the various ingredients of the non-evolving models for galaxy count observations. These ingredients include the K-corrections, the galaxy luminosity function and its dependence on galaxy colour, the local space density of galaxies and the cosmological deceleration parameter. Comparing the updated count model with the most recent galaxy count observations, the conclusion is still that at B>22m the B (and the R) counts require very significant amounts of evolution to fit the observed, steep n(m) relations. We review models of galaxy luminosity evolution and also discuss the current debate as to whether B≈23m galaxies have z ≈1 or z ≈3.We also consider recent suggestions that the form of Tyson's counts at B=27m may constrain the cosmological deceleration parameter; contrary to the suggestion of Koo (1989), it is proposed here that if the turnover seen in Tyson's B counts is real then this argues for high values of qo and/or low galaxy formation redshifts. Finally, we consider the implications of these results for observations of the extragalactic background light (EBL) and conclude that in the ultraviolet (UV) and in the optical the contribution of faint galaxies to the EBL is likely to be small if the turnover in Tyson's counts is real. The galaxy count evidence gives less clear indications about the contribution of galaxies to the infrared EBL.

Observations that radio-quiet QSOs exist in average galaxy cluster environments (Smith et al. 1995 and references therein) demonstrate that QSOs can be used to derive important information on the structure of the Universe at the largest scales. Previous studies of QSO clustering have been frustrated by the lack of large QSO redshift surveys. Although QSO clustering is detected in the largest existing QSO catalogues (see Shanks & Boyle 1994), it is difficult to place strong limits on the cosmological evolution of QSO clustering or the level of clustering at large scales (> 10h–1 Mpc) with current QSO catalogues.

We are currently carrying out a major redshift survey of 30000 QSOs using the 2dF facility on the Anglo-Australian Telescope. As of January 1998, over 1000 QSO redshifts have been obtained for the survey, making this the largest single homogeneous sample of QSOs yet compiled. When complete the survey will be used to provide important information on the large-scale structure of the Universe.

The transboundary nature of water resources demands a transboundary approach to their monitoring and management. However, transboundary water projects raise a challenging set of problems related to communication issues, and standardization of sampling, analysis and data management methods. This manual addresses those challenges and provides the information and guidance needed to perform the Navruz Project, a cooperative, transboundary, river monitoring project involving rivers and institutions in Kazakhstan, Kyrgyzstan, Tajikistan, and Uzbekistan facilitated by Sandia National Laboratories in the U.S. The Navruz Project focuses on waterborne radionuclides and metals because of their importance to public health and nuclear materials proliferation concerns in the region. This manual provides guidelines for participants on sample and data collection, field equipment operations and procedures, sample handling, laboratory analysis, and data management. Also included are descriptions of rivers, sampling sites and parameters on which data are collected. Data obtained in this project are shared among all participating countries and the public through an internet web site and are available for use in further studies and in regional transboundary water resource management efforts. Overall, the project addresses three main goals: to help increase capabilities in Central Asian nations for sustainable water resources management; to provide a scientific basis for supporting nuclear transparency and non-proliferation in the region; and to help reduce the threat of conflict in Central Asia over water resources, proliferation concerns, or other factors.

We present results from two new near-infrared imaging surveys. One survey covers 47.2 arcmin2 to K(3σ) = 20 mag whilst a second, deeper catalogue covers a subarea of 1.8 arcmin2 to K(3σ) = 22.75 mag. Over the entire area we have extremely deep optical photometry in four bandpasses (UBRI), allowing us to track the colour evolution of galaxies to very faint magnitude limits. Our K-band number counts are consistent with the predictions of non-evolving models with 0 ≤ q0 ≤ 0.5. The K-selected (B - K) galaxy colour distributions from our surveys move sharply bluewards fainter than K∼20. At brighter magnitudes (K < 20 mag) our K-selected (B - K) distributions indicate a deficiency of red, early-type galaxies at z ∼ 1 compared with the predictions of passively evolving models, which implies either a pure luminosity evolution (PLE) model, where star formation continues at a low level after an initial burst, or dynamical merging. At fainter magnitudes, the continuing bluewards trend observed in (B - K) can be explained purely in terms of passively evolving PLE models. We detect 0.5 ± 0.1 galaxy arcmin-2 with (I - K) > 4 and 19 < K < 20 mag. Although this is a factor of ∼3 (2σ) more objects than in the recent survey of Berger et al., this is still lower than the predictions of standard passively evolving models and more consistent with PLE models containing small amounts of ongoing star formation. Our observed numbers of (I - K) > 4 galaxies at K ∼ 20 are lower than the predictions of passively evolving models or PLE models with a low level of continuing star formation, suggesting that at least part of the larger deficiency observed in (B - K) at K ∼ 20 may be caused by star formation rather than dynamical merging. As we and others have noted, the number redshift distribution at 18 < K < 19 of recent, deep K-selected redshift surveys is well fitted by non-evolving models, and passively evolving models with a Salpeter or Scalo initial mass functions predict too many galaxies with z > 1. Dynamical merging is one possible solution to reduce the numbers of these galaxies but (as we have suggested previously) a dwarf-dominated initial mass function for early-type galaxies could offer an alternative explanation; we show here that such a model reproduces well the optical-infrared colour distributions and K-band galaxy counts.

The syntheses of the first amphotericin B derivatives to be modified solely at the C-13 hemiketal position are described. Selective functionalisation at this position is facilitated by use of the allyl ester as a C-16 carboxylate protecting group on the amphotericin B nucleus. In in vitro tests all compounds showed markedly reduced haemolytic activity against mammalian erythrocytes while two of the novel 13-alkoxy derivatives retained good antifungal activity.

The organisation and the workload of the anaesthetic department of a Field Hospital deployed during the Gulf war were described. Suggestions are made as to how the problems encountered might be overcome in the future.

We consider whether photometric errors may have induced the apparent large-scale, ≥10h -1 Mpc (where h is the Hubble constant in units of 100 km s-1 Mpc-1), power in the angular correlation function ω(θ) estimated from the APM galaxy catalogue. Using the galaxy CCD sequences on 39 of the plates in this catalogue we have made an independent estimate of the random and systematic errors in the APM magnitude scale. In particular we have found that the rms error in the plate zero-points is 0.m084, a factor of ∼2 larger than the estimate found by Maddox et al. (1990b). Further, the distribution of the zero-point residuals over the APM survey area suggests that much of this extra error could arise from large-scale magnitude correlations. Thus, taking these observations into account in the estimate of ω(θ), it is shown that the excess power in the galaxy correlation function may be due to photometric calibration errors and that the standard CDM galaxy formation model may not be in contradiction with the observations.

Novel purine nucleoside analogues in which the N-9 ribosyl moiety is replaced by a 2,3-dihydroxy-1-methoxypropyl or 3-hydroxy- 1-methoxy-propyl substituent and their N-7 substituted isomers have been synthesized and tested for antiviral activity.

Although aflatoxicosis in Coturnix coturnix japonica has been described, the histochemical localization of liver chemicals and the occurrence of ingested aflatoxins within blood, feces, and liver have not been described. Six to 8-week-old quail, which were intubated with a carrier with or without .3 mg mixed aflatoxins (AFB1, AFB2, AFG1, AFG2)/kg body weight were sacrificed within .25 to 5 days of intubation. Deparaffinized sections of livers were stained for lipids, nucleic acids, polysaccharides, and proteins. Other livers and excrement were homogenized and filtered homogenates as well as blood partitioned against chloroform. The aqueous phase was treated with pepsin and then partitioned, but the organic phase was analyzed directly. Organic phases of .25 to 5 day blood, feces, and liver lacked aflatoxins. Pepsin digesta of blood from males and females dosed 6 hr appeared to contain aflatoxicol (disappeared by 24 hr) and an unknown fluorescent compound, respectively. Whereas an unidentified fluorescent compound was observed within excrement of males dosed 6 hr, female excrement contained a fluorescent compound with an AFB1 Rf (disappeared by 24 hr). Although the liver of males dosed 6 hr had three fluorescent compounds (Rfs for AFB1 and AFB2a), only one was seen within dosed females. Ultra violet absorption spectra of presumed AFB2a and aflatoxicol failed to yield their reported absorption maxima. Livers from dosed quail exhibited bile duct proliferation, cellular necrosis, vacuolization, congestion, fatty changes and mild hepatitis. Sinusoidal membranes were thickened and contained abundant periodic acid-Schiff's (PAS)-positive substances. Although livers of nondosed quail abounded with regularly shaped and uniformly distributed, Sudan IV-positive droplets, livers of dosed quail accommodated few, irregularly-shaped and positioned droplets. Hepatocyte nuclei and nucleoli of dosed quail displayed marked affinities for the Feulgen reagent and toluidine blue O, respectively. Lobules of dosed quail possessed concentrations of cells in which their entire cytoplasm was PAS positive. Treatment of sections with alpha-amylase reduced staining suggesting the presence of glycogen. Ninhydrin-positive substances were distributed throughout the liver in both DQ and non DQ with no apparent difference in intensities between the two livers. Generally the DQ showed mild hepatitis due to aflatoxicosis and the toxin altered liver histochemistry for the major classes of cellular chemicals.

Recent results from studies of galaxy clustering in galaxy redshift surveys have tentatively suggested the existence of ‘spike’ features in the galaxy 2-point correlation function at large spatial scales. These features are most straightforwardly predicted in a dense, baryon dominated world model with initial adiabatic fluctuations. Here we discuss the prospects for such a model assuming a Friedmann cosmology with the density parameter, Ω , equal to the critical value of unity. We conclude that the lower the value of Hubble's constant, H 0 , the more likely it is that the above model may be consistent with the current observational constraints.

We are in the process of compiling a large catalogue of faint (B < 20.9 mag), UVX selected QSOs with complete spectroscopic identification using the fibre optic (FOCAP) system at the Anglo-Australian Telescope. From the 220 QSOs thus far identified we find that QSO evolution is most simply parameterised by a uniform increase in luminosity towards higher redshifts. We also find evidence for strong QSO clustering at scales < 10h−1 Mpc.

2,3,4,6-Tetra-O-benzyl-D-glucitol (5) reacts with toluene-p-sulphonyl chloride in pyridine at 60 °C to form mainly the furanoid products 2,3,6-tri-O-benzyl-1,4-anhydro-D-glucitol (10) and its 5-toluene-p-sulphonate (11) with loss of the 4-O-benzyl group. The pyranoid product tetra-O-benzyl-1,5-anhydro-D-glucitol preponderates when the intermediate 2,3,4,6-tetra-O-toluene-p-sulphonyl-D-glucitol (6) is converted into its 0–5 oxyanion. Benzyloxy participation has been exploited in a new synthesis of 2,3,5-tri-O-benzyl-α(and β)-D-ribofuranosylethyne, (20) and (4), from 2,3,4,5-tetra-O-benzyl-aldehydo-D-ribose. A synthesis of 2-α-D-ribofuranosylmaleimide, the α-isomer of showdomycin, from (20) is described.

We present correlation function results from galaxy and QSO redshift surveys. The galaxy correlation function shows evidence for a possible ‘shoulder’ feature in ξ(s) at s = 2h−1 Mpc. At scales between 10 and 100h−1Mpc the correlation function remains close to zero and shows no evidence for any large scale galaxy clustering. The QSO correlation function detects strong QSO clustering for scales s < 10h−1 Mpc. At larger scales (10 < s < 1000h−1 Mpc) no evidence of significant QSO clustering is seen.

Recent measurement of UK Schmidt plates have yielded interesting results on the cross-correlation of galaxies with QSOs and ultra-violet excess (UVX) objects. We find that in all Schmidt fields so far analysed there appears to be a significant anti-correlation (at angular scales less than 5') between the positions of galaxies and QSOs and between the positions of galaxies and UVX objects. This anti-correlation appears to be restricted to those galaxies that are found in clusters. These observations can very naturally be explained using a model in which dust within clusters of galaxies obscures the QSOs lying at cosmological distances behind them. This hypothesis may be further corroborated by tentative evidence that the UVX objects and the QSOs appear to be reddened close to clusters of galaxies.

The coverage of this paper, which was presented at an Ordinary Meeting of the Institute held in London on 18 March 1970, includes:(1) A brief review of current aircraft flight control systems.(2) A discussion of the benefits to be gained in terms of manual handling and full automatic pilot modes, in using feedback control techniques in the primary flight controls (Manœuvre Demand Control).(3) A description of the work done on Manœuvre Demand Control at the Royal Aircraft Establishment, Farnborough, in the Avro 707C aircraft and in the Hunter Mk. 12 aircraft.

When the American Civil War began, the Southern dioceses of the Protestant Episcopal Church organized a Confederate Church. Contrary to sentiment in the other popular Protestant denominations, there was in 1861 little hostility between the Confederate and Northern leaders of this Church. As the war progressed, however, bitterness developed until in 1865 at the close of the war many wanted to retain separate church organizations. Despite these animosities, some bold spirits succeeded in bringing about the reconciliation of the dioceses of the Church. The story of this reunion has been told before, but new material recently made available warrants a new analysis.

Showdomycin, 2-β-D-ribofuranosylmaleimide (1), has been prepared in six stages from 2,3,5-tri-O-benzyl-β-D-ribofuranosylethyne (2) in 23% overall yield (8% from D-ribose). Dimethoxycarbonylation of (2) afforded the substituted maleic ester (4) which was converted, in two stages, into the crystalline anhydride (10). Ammonolysis followed by ring-closure gave the crystalline maleimide (13), which was debenzylated with boron trichloride to give showdomycin.

We review the current status of the Edinburgh/Durham southern galaxy catalogue. The aim of this project is to use COSMOS measurements of the UK Schmidt J survey to produce a unique data base of galaxies, complete down to bj ∼ 20.5 mag and covering ∼ 100 survey fields. We have developed the optimum procedures to classify objects as stars or galaxies and calibrate the galaxy magniudes on individual plates. We are confident that residual systematics will be ∼ 5%, thereby ensuring that this catalogue will substantially contribute to our understanding of the Universe at large. One initial finding of the survey is a probable 6 sigma density fluctuation in the galaxy distribution.