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Results 1 - 10
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3,595
The Galaxy–Absorber Cross-Correlation Function
, 1997
"... Abstract. We describe an analysis of the galaxy–absorber cross-correlation function ξga(v, ρ) as a function of velocity separation v, impact parameter separation ρ, and absorber Lyα equivalent width W on impact parameter scales that extend up to ≈ 1 h −1 Mpc. 1 ..."
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Abstract. We describe an analysis of the galaxy–absorber cross-correlation function ξga(v, ρ) as a function of velocity separation v, impact parameter separation ρ, and absorber Lyα equivalent width W on impact parameter scales that extend up to ≈ 1 h −1 Mpc. 1
Long-range time dependence in the cross-correlation function
"... Detection of a long-range time dependence in the radial cross-correlation function is normally difficult because of the oscillatory behavior of the cross-correlation tail, its low level of coherence, and noise contamination. This problem persists, even with large statistical samples. In this paper, ..."
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Detection of a long-range time dependence in the radial cross-correlation function is normally difficult because of the oscillatory behavior of the cross-correlation tail, its low level of coherence, and noise contamination. This problem persists, even with large statistical samples. In this paper
Computing Energy Levels by Inversion of Imaginary-Time Cross-Correlation Functions†
"... As proposed by Ceperley and Bernu, the excited-state energies can be obtained from imaginary-time cross-correlation functions (rather than autocorrelation functions) generated by quantum Monte Carlo (QMC) simulations. We show that, when processed by the filter diagonalization method (FDM), the same ..."
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As proposed by Ceperley and Bernu, the excited-state energies can be obtained from imaginary-time cross-correlation functions (rather than autocorrelation functions) generated by quantum Monte Carlo (QMC) simulations. We show that, when processed by the filter diagonalization method (FDM), the same
Two-dimensional sensitivity kernels for cross-correlation functions of background surface waves
- Comp. Rend. Geosci
, 2011
"... Abstract Ambient noise tomography has now been applied at scales ranging from local to global. To discuss the theoretical background of the technique, a simple form of a two-dimensional (2-D) Born sensitivity kernel was developed at a finite frequency for a cross-correlation function (CCF) of backg ..."
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Cited by 1 (0 self)
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Abstract Ambient noise tomography has now been applied at scales ranging from local to global. To discuss the theoretical background of the technique, a simple form of a two-dimensional (2-D) Born sensitivity kernel was developed at a finite frequency for a cross-correlation function (CCF
QSO-LRG 2-Point Cross-Correlation Function and Redshift-Space Distortions
, 2007
"... We have measured the bias of QSOs as a function of QSO luminosity at fixed redshift (z < 1) by cross-correlating them with Luminous Red Galaxies (LRGs) in the same spatial volume, hence breaking the degeneracy between QSO luminosity and redshift. We use three QSO samples from 2SLAQ, 2QZ and SDSS ..."
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We have measured the bias of QSOs as a function of QSO luminosity at fixed redshift (z < 1) by cross-correlating them with Luminous Red Galaxies (LRGs) in the same spatial volume, hence breaking the degeneracy between QSO luminosity and redshift. We use three QSO samples from 2SLAQ, 2QZ and SDSS
The APM cluster-galaxy cross-correlation function: Constraints on Ω and galaxy bias.
, 2008
"... We estimate the cluster-galaxy cross-correlation function (ξcg), from the APM galaxy and galaxy cluster surveys. We obtain estimates both in real space from the inversion of projected statistics and in redshift space using the galaxy and cluster redshift samples. The amplitude of ξcg is found to be ..."
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We estimate the cluster-galaxy cross-correlation function (ξcg), from the APM galaxy and galaxy cluster surveys. We obtain estimates both in real space from the inversion of projected statistics and in redshift space using the galaxy and cluster redshift samples. The amplitude of ξcg is found
The Comparison of cylindricity profiles using normalized cross-correlation function
- In Proc. of 5 th International Conference Measurement 2005, Smolenice (SK
, 2005
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Understanding the shape of the halo-mass and galaxy-mass cross-correlation functions
, 709
"... Weak gravitational lensing has opened a new window onto the large scale distribution of matter. Gravitational lensing by foreground mass induces correlated distortions, or shear, in the observed shapes of distant ..."
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Cited by 2 (0 self)
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Weak gravitational lensing has opened a new window onto the large scale distribution of matter. Gravitational lensing by foreground mass induces correlated distortions, or shear, in the observed shapes of distant
The galaxy cross-correlation function as a probe of the spatial distribution of galactic satellites
- Astronomy & Astrophysics
, 2009
"... ar ..."
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