Large-Scale Fluctuations in the Number Density of Galaxies in
  Independent Surveys of Deep Fields
  New arguments supporting the reality of large-scale fluctuations in the
density of the visible matter in deep galaxy surveys are presented. A
statistical analysis of the radial distributions of galaxies in the COSMOS and
HDF-N deep fields is presented. Independent spectral and photometric surveys
exist for each field, carried out in different wavelength ranges and using
different observing methods. Catalogs of photometric redshifts in the optical
(COSMOS-Zphot) and infrared (UltraVISTA) were used for the COSMOS field in the
redshift interval $0.1 < z < 3.5$, as well as the zCOSMOS (10kZ) spectroscopic
survey and the XMM-COSMOS and ALHAMBRA-F4 photometric redshift surveys. The
HDFN-Zphot and ALHAMBRA-F5 catalogs of photometric redshifts were used for the
HDF-N field. The Pearson correlation coefficient for the fluctuations in the
numbers of galaxies obtained for independent surveys of the same deep field
reaches $R = 0.70 \pm 0.16$. The presence of this positive correlation supports
the reality of fluctuations in the density of visible matter with sizes of up
to 1 000 Mpc and amplitudes of up to 20% at redshifts $z \sim 2$. The absence
of correlations between the fluctuations in different fields (the correlation
coefficient between COSMOS and HDF-N is $R = -0.20 \pm 0.31$) testifies to the
independence of structures visible in different directions on the celestial
sphere. This also indicates an absence of any influence from universal
systematic errors (such as "spectral voids"), which could imitate the detection
of correlated structures.
