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Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-13587

D'Onghia, E; Mapelli, M; Moore, B (2008). Merger and ring galaxy formation rates at z <= 2. Monthly Notices of the Royal Astronomical Society, 389(3):1275-1283.

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Abstract

We compare the observed merger rate of galaxies over cosmic time and the frequency of collisional ring galaxies (CRGs), with analytic models and halo merger and collision rates from a large cosmological simulation. In the Λ cold dark matter (ΛCDM) model, we find that the cosmic merger fraction does not evolve strongly between 0.2 ≤z≤ 2, implying that the observed decrease in the cosmic star formation rate since z∼ 1 might not be tied to a disappearing population of major mergers. Haloes hosting massive galaxies undergo on average ∼2 mergers from z≤ 2 up to present day, reflecting the late assembly time for the massive systems and the related down-sizing problem. The cosmic merger rate declines with redshift: at the present time, it is of a factor of 10 lower than at z∼ 2 in reasonable agreement with the current available data. The rate of CRG formation derived from the interactions between halo progenitors up to z= 2 is found to be a good tracer of the cosmic merger rate. In the ΛCDM model, the rate of CRGs as well as the merger rate do not scale as (1 +z)m as suggested by previous models. Our predictions of cosmic merger and CRG rates may be applied to forthcoming surveys such as GOODS and zCOSMOS

Item Type:Journal Article, refereed, original work
Communities & Collections:07 Faculty of Science > Institute for Computational Science
DDC:530 Physics
Uncontrolled Keywords:methods: N-body simulations; galaxies: interactions; galaxies: peculiar; cosmology: theory
Language:English
Date:September 2008
Deposited On:17 Feb 2009 16:13
Last Modified:28 Nov 2013 00:44
Publisher:Wiley-Blackwell
ISSN:0035-8711
Additional Information:The definitive version is available at www.blackwell-synergy.com
Publisher DOI:10.1111/j.1365-2966.2008.13625.x
Related URLs:http://arxiv.org/abs/0803.0545
Citations:Web of Science®. Times Cited: 7
Google Scholar™
Scopus®. Citation Count: 9

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