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Date and Time of the Query: 2018-11-15 T21:23:10 PST
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For refcode 2013ApJ...776...91L:
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2013ApJ...776...91L The Contribution of Halos with Different Mass Ratios to the Overall Growth of Cluster-sized Halos Lemze, Doron; Postman, Marc; Genel, Shy; Ford, Holland C.; Balestra, Italo; Donahue, Megan; Kelson, Daniel; Nonino, Mario; Mercurio, Amata; Biviano, Andrea; Rosati, Piero; Umetsu, Keiichi; Sand, David; Koekemoer, Anton; Meneghetti, Massimo; Melchior, Peter; Newman, Andrew B.; Bhatti, Waqas A.; Voit, G. Mark; Medezinski, Elinor; Zitrin, Adi; Zheng, Wei; Broadhurst, Tom; Bartelmann, Matthias; Benitez, Narciso; Bouwens, Rychard; Bradley, Larry; Coe, Dan; Graves, Genevieve; Grillo, Claudio; Infante, Leopoldo; Jimenez-Teja, Yolanda; Jouvel, Stephanie; Lahav, Ofer; Maoz, Dan; Merten, Julian; Molino, Alberto; Moustakas, John; Moustakas, Leonidas; Ogaz, Sara; Scodeggio, Marco; Seitz, Stella Abstract. We provide a new observational test for a key prediction of the LambdaCDM 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_sun_, 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 ~0.2 and ~0.7, we find a ~1sigma agreement with LambdaCDM expectations based on the Millennium simulations I and II. At low mass ratios, <~ 0.2, our derived contribution is underestimated since the detection efficiency decreases at low masses, ~2 x 10^14^ h_{0.73}_^{-1} M_sun_. At large mass ratios, >~ 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. Key words: dark matter, galaxies: clusters: individual: Abell 611 Abell 963 Abell 1423 Abell 2261 MACS J1206.2--0848 RX J2129.7+0005 CL 2130.4--0000, galaxies: kinematics and dynamics
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