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Large--Scale Angular Correlations in CDM Models
Astrophysics · Submitted 23 Feb 1993
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Such models are therefore in principle capable of reconciling the lack of large--scale power of the CDM spectrum with the observed clustering of APM galaxies.
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We generate artificial Lick maps using $N$--body simulations and compare the angular correlation function, $w(\vartheta)$, measured from the simulations with the APM correlation. For the Gaussian CDM model, neither the standard biassed model nor a more evolved model (as suggested by the COBE data), reproduce the correlations on large angular scales. We come to a similar conclusion about CDM models with positively skewed initial fluctuation distributions. In contrast, models with initially negatively skewed fluctuations produce a $w(\vartheta)$ that declines much more gently on large scales. Such models are therefore in principle capable of reconciling the lack of large--scale power of the CDM spectrum with the observed clustering of APM galaxies.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We generate artificial Lick maps using $N$--body simulations and compare the angular correlation function, $w(\vartheta)$, measured from the simulations with the APM correlation. | method 0.94 | 0.95 | 0.03 | asserted 0.96 |
| s1 | For the Gaussian CDM model, neither the standard biassed model nor a more evolved model (as suggested by the COBE data), reproduce the correlations on large angular scales. | result 1.00 | 0.83 | 0.26 | asserted 1.00 |
| s2 | We come to a similar conclusion about CDM models with positively skewed initial fluctuation distributions. | result 1.00 | 0.82 | 0.09 | asserted 1.00 |
| s3 | In contrast, models with initially negatively skewed fluctuations produce a $w(\vartheta)$ that declines much more gently on large scales. | result 1.00 | 0.85 | 0.21 | asserted 1.00 |
| s4 | Such models are therefore in principle capable of reconciling the lack of large--scale power of the CDM spectrum with the observed clustering of APM galaxies. | interpretation 1.00 | 0.66 | 0.71 | hedged possibility 0.98 |
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Original abstract
We generate artificial Lick maps using $N$--body simulations and compare the angular correlation function, $w(\vartheta)$, measured from the simulations with the APM correlation. For the Gaussian CDM model, neither the standard biassed model nor a more evolved model (as suggested by the COBE data), reproduce the correlations on large angular scales. We come to a similar conclusion about CDM models with positively skewed initial fluctuation distributions. In contrast, models with initially negatively skewed fluctuations produce a $w(\vartheta)$ that declines much more gently on large scales. Such models are therefore in principle capable of reconciling the lack of large--scale power of the CDM spectrum with the observed clustering of APM galaxies.
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