We provide a new observational test for a key prediction of the Lambda CDM cosmological model: the contributions of mergers with different halo-to-main-cluster mass ratios to cluster-sized halo growth. We perform this test by dynamically analyzing 7 galaxy clusters, spanning the redshift range 0.13 < z(c) < 0.45 and caustic mass range 0.4-1.5 10(15) h(0.73)(-1) M-circle dot, with an average of 293 spectroscopically confirmed bound galaxies to each cluster. The large radial coverage (a few virial radii), which covers the whole infall region, with a high number of spectroscopically identified galaxies enables this new study. For each cluster, we identify bound galaxies. Out of these galaxies, we identify infalling and accreted halos and estimate their masses and their dynamical states. Using the estimated masses, we derive the contribution of different mass ratios to cluster-sized halo growth. For mass ratios between similar to 0.2 and 0.7, we find a similar to 1 sigma agreement with Lambda CDM expectations based on the Millennium simulations I and II. At low mass ratios, less than or similar to 0.2, our derived contribution is underestimated since the detection efficiency decreases at low masses, similar to 2 x 10(14) h(0.73)(-1) M-circle dot. At large mass ratios, greater than or similar to 0.7, we do not detect halos probably because our sample, which was chosen to be quite X-ray relaxed, is biased against large mass ratios. Therefore, at large mass ratios, the derived contribution is also underestimated.
THE CONTRIBUTION OF HALOS WITH DIFFERENT MASS RATIOS TO THE OVERALL GROWTH OF CLUSTER-SIZED HALOS
Mercurio A;
2013-01-01
Abstract
We provide a new observational test for a key prediction of the Lambda CDM cosmological model: the contributions of mergers with different halo-to-main-cluster mass ratios to cluster-sized halo growth. We perform this test by dynamically analyzing 7 galaxy clusters, spanning the redshift range 0.13 < z(c) < 0.45 and caustic mass range 0.4-1.5 10(15) h(0.73)(-1) M-circle dot, with an average of 293 spectroscopically confirmed bound galaxies to each cluster. The large radial coverage (a few virial radii), which covers the whole infall region, with a high number of spectroscopically identified galaxies enables this new study. For each cluster, we identify bound galaxies. Out of these galaxies, we identify infalling and accreted halos and estimate their masses and their dynamical states. Using the estimated masses, we derive the contribution of different mass ratios to cluster-sized halo growth. For mass ratios between similar to 0.2 and 0.7, we find a similar to 1 sigma agreement with Lambda CDM expectations based on the Millennium simulations I and II. At low mass ratios, less than or similar to 0.2, our derived contribution is underestimated since the detection efficiency decreases at low masses, similar to 2 x 10(14) h(0.73)(-1) M-circle dot. At large mass ratios, greater than or similar to 0.7, we do not detect halos probably because our sample, which was chosen to be quite X-ray relaxed, is biased against large mass ratios. Therefore, at large mass ratios, the derived contribution is also underestimated.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
