Constrained Simulations of the Real Universe. II. Observational Signatures of Intergalactic Gas in the Local Supercluster Region

By Andrey V. Kravtsov, Anatoly Klypin, Y. Hoffman. 2001

226 citations recorded by the source corpus.

We present results of gasdynamics+N-body constrained cosmological simulations of the Local Supercluster region (LSC; about 30 h-1 Mpc around the Virgo cluster), which closely mimic the real universe within 100 Mpc, by imposing constraints from the MARK III catalog of galaxy peculiar velocities. The simulations are used to study the properties and possible observational signatures of intergalactic medium in the LSC region. We find that in agreement with previous unconstrained simulations, ≈30% of the gas in this region is in the warm/hot phase at T ~ 105-107 K and ≈40% in the diffuse phase at T < 105 K in low-density regions. The X-ray emission from the warm/hot gas may represent a small (~5%-10%) but important contribution to the X-ray background observed by the ROSAT All-Sky Survey at energies around 1 keV. The best prospects for detection of the warm/hot intergalactic medium of the LSC located in filaments and in the vicinity of virialized regions of groups and clusters are through absorption in resonant lines of O VII and O VIII in soft X-rays and in the O VI doublet in UV. If intergalactic gas in filaments (ρ/⟨ρ⟩ ~ 1-10) is enriched to typical metallicities of ≳0.05, the column densities of O VI, O VII, and O VIII along a random line of sight near the north Galactic pole, especially near the supergalactic plane, have a significant probability to be in the range detectable by current (FUSE, XMM) and future (Constellation-X) instruments.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/051eaab674db17348d380f915bbdd8c18d938de8

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

The Cosmological simulation code GADGET-2 (2005, methodology): “Mesh-based codes include algorithms with a ﬁxed mesh (e.g. Cen & Ostriker, 1992, 1993; Yepes et al., 1995; Pen, 1998), and more recently also with adaptive meshes (e.g. Bryan & Norman, 1997; Norman & Bryan, 1999; Teyssier, 2002; Kravtsov et al., 2002; Quilis, 2004).”
ENVIRONMENTAL DEPENDENCE OF THE KENNICUTT–SCHMIDT RELATION IN GALAXIES (2010, methodology): “The simulation was run with Adaptive Refinement Tree (ART) code (Kravtsov 1999; Kravtsov et al. 2002; Rudd et al. 2008) and follows a Lagrangian region corresponding to five virial radii of a system, which evolves into a typical halo of an L∗ galaxy (M ≈ 1012 M ) at z = 0.”
RESIDUAL GAS MOTIONS IN THE INTRACLUSTER MEDIUM AND BIAS IN HYDROSTATIC MEASUREMENTS OF MASS PROFILES OF CLUSTERS (2009, methodology): “The simulations were done with the Adaptive Refinement Tree (ART)N-body+gasdynamics code (Kravtsov 1999; Kravtsov et al. 2002), a Eulerian code that uses adaptive refinement in space and time, and (non-adaptive) refinement in mass (Klypin et al. 2001) to reach the high dynamic range required to…”
THE VELOCITY FUNCTION IN THE LOCAL ENVIRONMENT FROM ΛCDM AND ΛWDM CONSTRAINED SIMULATIONS (2009, methodology): “This approach follows the CSs performed by Kravtsov et al. (2002) and Klypin et al. (2003).”
Intercluster filaments in a ΛCDM Universe (2004, background): “For the most recent studies see Davé et al. (2001), Kravtsov et al. (2002), and Furlanetto et al. (2003) and references therein.”
X-Ray and Sunyaev-Zel’dovich Effect Measurements of the Gas Mass Fraction in Galaxy Clusters (2006, methodology): “This test is carried out using cosmological simulations of galaxy clusters generated with the Adaptive Refinement Tree (ART) N-body+gasdynamics code (Kravtsov 1999; Kravtsov et al. 2002).”
Bayesian physical reconstruction of initial conditions from large-scale structure surveys (2012, methodology): “These initial density fields may be useful for a variety of scientific projects such as constrained simulations (see e.g. Kravtsov et al. 2002; Klypin et al. 2003; Dolag et al. 2005; Libeskind et al. 2010; MartinezVaquero et al. 2009; Gottloeber et al. 2010; Lavaux 2010; Dolag et al. 2012).”
GRACKLE: a chemistry and cooling library for astrophysics (2016, unknown): “To date, the following codes are known to have Grackle implemented: • AREPO (Springel 2010) • ART-I (Kravtsov 1999; Kravtsov et al. 2002) • ART-II (Rudd et al. 2008) • CHANGA (Wadsley et al. 2004; Stinson et al. 2006) • Cosmos++ (Anninos et al. 2003, 2005) • Enzo (Bryan et al. 2014) • Gadget-3…”
The effects of galaxy formation on the matter power spectrum: a challenge for precision cosmology (2011, methodology): “Rudd et al. (2008) used the art code (Kravtsov 1999) expanded with the Eulerian hydrodynamics solver described in Kravtsov et al. (2002).”
Detecting shock waves in cosmological smoothed particle hydrodynamics simulations (2006, background): “…more recently,adaptive mesh refinement (AMR) algorithms have been developed for cosmological applications (Berger & Colella 1989; Bryan & Norman 1997; Norman & Bryan 1999; Abel et al. 2002; Kravtsov et al. 2002; Refregier & Teyssier 2002), which can adapt to regionsof interest in a flexible way.”
IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM (2010, methodology): “Figure 1 shows the pressure-density phase diagram obtained for 16 clusters simulated using the Eulerian hydrodynamics ART code (Kravtsov et al. 2002), including radiative cooling and star formation (Nagai et al. 2007a).”
MODELING MOLECULAR HYDROGEN AND STAR FORMATION IN COSMOLOGICAL SIMULATIONS (2008, methodology): “…that the simulation was performed with the Eulerian, gas dynamics + N -body Adaptive Refinement Tree (ART) code (Kravtsov et al. 1997; Kravtsov 1999; Kravtsov et al. 2002), which uses adaptive mesh refinement (AMR) in both the gas dynamics and gravity calculations to achieve a needed dynamic range.”
Galaxy formation theory (2010, unknown): “Notes 1“GAlaxies with Dark matter and Gas intEracT” (Springel, 2005); 2Wadsley et al. (2004); 3Hydrodynamic Adaptive Refinement Tree (Kravtsov et al., 2002); 4O’Shea et al. (2004); 5http://flash.uchicago.edu (Fryxell et al., 2000); 6Adaptive Mesh Refinement; 7Particle–mesh; 8Smoothed Particle Hydrod”
Escape of Ionizing Radiation from High-Redshift Galaxies (2007, methodology): “The simulation is performed using the Eulerian, gas dynamics + N-body Adaptive Refinement Tree (ART) code (Kravtsov et al. 1997, 2002).”
Comparing AMR and SPH Cosmological Simulations. I. Dark Matter and Adiabatic Simulations (2003, result): “It is interesting to note that the enclosed gas mass fraction at the virial radius produced by the ART code is higher than that of GADGET by a few percent, and the ART gas mass fraction result would be bracketed by the Enzo and GADGET results, overall.”
A COMPARISON OF METHODS FOR DETERMINING THE MOLECULAR CONTENT OF MODEL GALAXIES (2010, methodology): “Here we only remind a reader that a set of “fixed ISM” simulations was performed with the Adaptive Refinement Tree (ART) code (Kravtsov 1999; Kravtsov et al. 2002; Rudd et al. 2008).”