Merging History as a Function of Halo Environment

By Stefan Gottloeber, Anatoly Klypin, Andrey V. Kravtsov. 2000

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According to the hierarchical scenario, galaxies form via merging and accretion of small objects. Using N-body simulations, we study the frequency of merging events in the history of the halos. We find that at z ≲ 2 the merging rate of the overall halo population can be described by a simple power law, (1 + z)3. The main emphasis of this paper is on the effects of environment of halos at the present epoch (z = 0). We find that the halos located inside clusters have formed earlier (Δz ≈ 1) than isolated halos of the same mass. At low redshifts (z < 1), the merger rate of cluster halos is 3 times lower than that of isolated halos and twice as low as that of halos that end up in groups by z = 0. At higher redshifts (z ~ 1-4), progenitors of cluster and group halos have 3-5 times higher merger rates than isolated halos. We briefly discuss the implications of our results for galaxy evolution in different environments.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ac0072666a5fec60aad189e8af8c3ef2b0607d7b

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Citations in the corpus

HISTORY OF GALAXY INTERACTIONS AND THEIR IMPACT ON STAR FORMATION OVER THE LAST 7 Gyr FROM GEMS (2009, methodology): “…mergers per comoving volume and per unit time between isolated dark matter (DM) halos within a ΛCDM model is relatively straightforward via semi-analytic methods or Nbody simulations (e.g. Lacey & Cole 1993; Gottlöber et al. 2001; Fakhouri & Ma 2008; Neistein & Dekel 2008; D’Onghia et al. 2008).”
MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, background): “Another is found in Gottlöber et al. (2001) (see also Kravtsov et al. 2004; Zentner et al. 2005); they quantify the fit separately to field, group, and cluster environments.”
Luminous Infrared Galaxies with the Submillimeter Array. I. Survey Overview and the Central Gas to Dust Ratio (2008, background): “Since galaxy merger rates are substantially higher in the early universe (Le Fèvre et al. 2000; Gottlöber et al. 2001), understanding the physical and dynamical properties of nearby ULIRGs is also important for understanding the processes in the early universe which give rise to the very luminous…”
The Rest-Frame Far-Ultraviolet Morphologies of Star-Forming Galaxies at z ~ 1.5 and 4 (2006, background): “The observed major-merger fraction and large number of minor-merger candidates are consistent with current numerical (Gottlöber et al. 2001) and semianalytic model predictions (Somerville et al. 2001) for high-redshift galaxies.”
ON THE CLUSTER PHYSICS OF SUNYAEV–ZEL'DOVICH AND X-RAY SURVEYS. I. THE INFLUENCE OF FEEDBACK, NON-THERMAL PRESSURE, AND CLUSTER SHAPES ON Y–M SCALING RELATIONS (2011, background): “In particular, the relative mass accretion rates increase fromz = 0 to z = 2 by a factor 3 for clusters (M200 = 1015M⊙) and 10 for groups (M200 = 1013M⊙) (see Pfrommer et al. 2011; Gottlöber et al. 2001).”
The role of minor mergers in the recent star formation history of early-type galaxies (2007, background): “The merger fraction increases with look-back time because the merger rate in the Universe increases at higher redshift (see also e.g. Gottlöber et al. 2001; Le Fèvre et al. 2000).”
Early and Rapid Merging as a Formation Mechanism of Massive Galaxies: Empirical Constraints (2005, methodology): “…its extension (Bond et al. 1991; Bower 1991; Lacey & Cole 1993), agree well with Nbody models of the hierarchical galaxy formation process (e.g., Gottlober et al. 2001), and has been used as the basis for all semi-analytic CDM models, some of which have published these merger histories (Kolatt…”
The nearly universal merger rate of dark matter haloes in ΛCDM cosmology (2007, methodology): “Gottlöber et al. (2001) studied the rate of major mergers (defined to be ξ > 1/3 in our notation) in N-body simulations and found a steeper power law dependence of ∝ (1+z)3 (at z .”
The realm of the galaxy protoclusters (2016, background): “Galaxies in present-day clusters experienced more major mergers compared to galaxies of a similar mass outside clusters (Gottlöber et al., 2001; Fakhouri & Ma, 2009).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. I. Galaxy Mergers and Quasar Activity (2007, background): “…which are not well defined (even when extracted directly from cosmological simulations) and depend sensitively on a number of definitions (see, e.g., Gottlöber et al. 2001;Maller et al. 2006), but instead wework from the robust (and well-defined) subhalo mass function (see Gao et al. 2004 and…”
DUSTY INFRARED GALAXIES: Sources of the Cosmic Infrared Background (2005, background): “The latter dominates the infrared and submillimeter energy density of the Universe at high z. Consistently, cold dark matter N-body simulations show that halo merger rates increase with redshift as (1+z)m with 2.5≤ m ≤3.5 (Gottlober et al. 2001).”
A systematic study of X-ray substructure of galaxy clusters detected in the ROSAT All-Sky Survey ? (2001, unknown): “High-resolution N -body simulations of, e.g., Gottlöber et al. (2001) suggest an increase of major merger rates by a factor of about 2 between redshift z = 0 and 0.25.”
CHANDRA CLUSTER COSMOLOGY PROJECT. II. SAMPLES AND X-RAY DATA REDUCTION (2008, result): “…offset can lead to departures from selfsimilar evolution in the Mtot–TX relation for the entire cluster population, because the fraction of merging clusters is expected to increase at high redshifts (e.g., Gottlöber et al. 2001; Cohn & White 2005), as we indeed observe in our sample (Figure 8).”
The merger rates and mass assembly histories of dark matter haloes in the two Millennium simulations (2010, background): “Halo mergers have also been studied in a handful of papers by others (e.g., Governato et al. 1999; Gottlöber et al. 2001; Berrier et al. 2006; Maller et al. 2006; Guo & White 2008; Genel et al. 2009; Stewart et al. 2009).”
Formation of Globular Clusters in Hierarchical Cosmology (2003, background): “Statistically, the CDM halo merger rate at zP 4 decreases rapidly as (1þ z) 2:5 (Gottlöber et al. 2001).”