@misc{Kashlinsky1998,
  abstract = {  It is shown how data on the cluster correlation function can be used in order
to reconstruct the density of the pregalactic density field on the cluster mass
scale. The method is applied to the data on the cluster correlation amplitude
-- richness dependence. The spectrum of the recovered density field has the
same shape as the density field derived from data on the galaxy correlation
function which is measured as function of linear scales. Matching the two
amplitudes relates the mass to the comoving scale it contains and thereby leads
to a direct determination of $\Omega$. The resultant density parameter turns
out to be $\Omega$=0.25.
},
  added-at = {2011-04-23T19:03:01.000+0200},
  author = {Kashlinsky, A.},
  biburl = {https://www.bibsonomy.org/bibtex/2ad416aa019f26b305b83486785c4c4a2/ad4},
  description = {Determining $\Omega$ from cluster correlation function},
  interhash = {0ff12b8becf7d683414e4b0f79433659},
  intrahash = {ad416aa019f26b305b83486785c4c4a2},
  keywords = {Clusters Dark Galaxy Matter},
  note = {cite arxiv:astro-ph/9806236
Comment: to appear in Physics Reports, "Dark Matter 98", vol.306},
  timestamp = {2011-04-23T19:03:01.000+0200},
  title = {Determining $\Omega$ from cluster correlation function},
  url = {http://arxiv.org/abs/astro-ph/9806236},
  year = 1998
}

@misc{Bahcall1998,
  abstract = {  The existence of the three most massive clusters of galaxies observed so far
at z>0.5 is used to constrain the mass density parameter of the universe,
Omega, and the amplitude of mass fluctuations, sigma_8. We find Omega=0.2
(+0.3,-0.1), and sigma_8=1.2 (+0.5,-0.4) (95 %). We show that the existence of
even the single most distant cluster at z=0.83, MS1054-03, with its large
gravitational lensing mass, high temperature, and large velocity dispersion, is
sufficient to establish powerful constraints. High-density, Omega=1 (sigma_8 ~
0.5-0.6) Gaussian models are ruled out by these data (< 10^{-6} probability);
the Omega=1 models predict only ~10^{-5} massive clusters at z > 0.65 (~10^{-3}
at z > 0.5) instead of the 1 (3) clusters observed.
},
  added-at = {2011-04-23T18:53:30.000+0200},
  author = {Bahcall, Neta A. and Fan, Xiaohui},
  biburl = {https://www.bibsonomy.org/bibtex/25959653151ba0e18905ddb068b6cef31/ad4},
  description = {The Most Massive Distant Clusters: Determining Omega and sigma_8},
  interhash = {c9a74267791af8c038f5685d5aebd6a0},
  intrahash = {5959653151ba0e18905ddb068b6cef31},
  keywords = {Clusters Dark Galaxy Matter},
  note = {cite arxiv:astro-ph/9803277
Comment: 14 pages, 4 Postscript figures, ApJ in press},
  timestamp = {2011-04-23T18:53:30.000+0200},
  title = {The Most Massive Distant Clusters: Determining Omega and sigma_8},
  url = {http://arxiv.org/abs/astro-ph/9803277},
  year = 1998
}

@misc{Brownstein2005,
  abstract = {  We apply the modified acceleration law obtained from Einstein gravity coupled
explaining galaxy rotation curves without exotic dark matter. Our sample of
galaxies includes low surface brightness (LSB) and high surface brightness
(HSB) galaxies, and an elliptical galaxy. In those cases where photometric data
are available, a best fit via the single parameter (M/L)_{stars} to the
luminosity of the gaseous (HI plus He) and luminous stellar disks is obtained.
Additionally, a best fit to the rotation curves of galaxies is obtained in
terms of a parametric mass distribution (independent of luminosity
observations) -- a two parameter fit to the total galactic mass, (or
mass-to-light ratio M/L), and a core radius associated with a model of the
galaxy cores using a nonlinear least-squares fitting routine including
estimated errors. The fits are compared to those obtained using Milgrom's
phenomenological MOND model and to the predictions of the Newtonian-Kepler
acceleration law.
},
  added-at = {2009-09-02T16:20:17.000+0200},
  author = {{Brownstein}, J. R. and {Moffat}, J. W.},
  biburl = {https://www.bibsonomy.org/bibtex/22fe140028deb9adf99b0e22c31f1e77f/ad4},
  description = {Galaxy Rotation Curves Without Non-Baryonic Dark Matter},
  interhash = {b9e1901cafaf1524723079fcc00a2013},
  intrahash = {2fe140028deb9adf99b0e22c31f1e77f},
  keywords = {Curve Dark Galaxy Matter Rotation},
  note = {cite arxiv:astro-ph/0506370
Comment: 43 pages, 7 figures, 4 tables, 101 galaxies. Submitted to ApJ, June
  20, 2005. Accepted for publication in ApJ, September 21, 2005. To be published
  in ApJ 636 (January 10, 2006)},
  timestamp = {2009-09-02T16:20:18.000+0200},
  title = {{G}alaxy {R}otation {C}urves {W}ithout {N}on-{B}aryonic {D}ark {M}atter},
  url = {http://arxiv.org/abs/astro-ph/0506370},
  year = 2005
}