TY - JOUR
T1 - The contribution of halos with different mass ratios to the overall growth of cluster-sized halos
AU - Lemze, Doron
AU - Postman, Marc
AU - Genel, Shy
AU - Ford, Holland C.
AU - Balestra, Italo
AU - Donahue, Megan
AU - Kelson, Daniel
AU - Nonino, Mario
AU - Mercurio, Amata
AU - Biviano, Andrea
AU - Rosati, Piero
AU - Umetsu, Keiichi
AU - Sand, David
AU - Koekemoer, Anton
AU - Meneghetti, Massimo
AU - Melchior, Peter
AU - Newman, Andrew B.
AU - Bhatti, Waqas A.
AU - Voit, G. Mark
AU - Medezinski, Elinor
AU - Zitrin, Adi
AU - Zheng, Wei
AU - Broadhurst, Tom
AU - Bartelmann, Matthias
AU - Benitez, Narciso
AU - Bouwens, Rychard
AU - Bradley, Larry
AU - Coe, Dan
AU - Graves, Genevieve
AU - Grillo, Claudio
AU - Infante, Leopoldo
AU - Jimenez-Teja, Yolanda
AU - Jouvel, Stephanie
AU - Lahav, Ofer
AU - Maoz, Dan
AU - Merten, Julian
AU - Molino, Alberto
AU - Moustakas, John
AU - Moustakas, Leonidas
AU - Ogaz, Sara
AU - Scodeggio, Marco
AU - Seitz, Stella
PY - 2013/10/20
Y1 - 2013/10/20
N2 - We provide a new observational test for a key prediction of the ΛCDM 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 M ⊙, 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 ∼1σ agreement with ΛCDM 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 × 1014 M ⊙. 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.
AB - We provide a new observational test for a key prediction of the ΛCDM 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 M ⊙, 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 ∼1σ agreement with ΛCDM 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 × 1014 M ⊙. 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.
KW - dark matter
KW - galaxies: kinematics and dynamics
UR - http://www.scopus.com/inward/record.url?scp=84886001084&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84886001084&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/776/2/91
DO - 10.1088/0004-637X/776/2/91
M3 - Article
AN - SCOPUS:84886001084
SN - 0004-637X
VL - 776
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 91
ER -