Strong Gravitational Lensing and Velocity Function as Tools to Probe Cosmological Parameters: Current Constraints and Future Predictions

Nakamura, T.; Suto, Yasushi

doi:10.1143/ptp.97.49

Cited by 125 publications

(74 citation statements)

References 70 publications

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“…with Δ vir (z) being the critical overdensity for virialisation at redshift z (Kitayama & Suto 1996;Nakamura & Suto 1997;Henry 2000). We take the fitting formula from Weinberg & Kamionkowski (2003) …”

Section: Appendix A: the Halo Modelmentioning

confidence: 99%

Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes sincez ~ 1.2

Coupon

Kilbinger

McCracken

et al. 2012

A&A

172

245

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It has become increasingly apparent that studying how dark matter haloes are populated by galaxies can provide new insights into galaxy formation and evolution. In this paper, we present a detailed investigation of the changing relationship between galaxies and the dark matter haloes they inhabit from z ∼ 1.2 to the present day. We do this by comparing precise galaxy clustering measurements over 133 deg 2 of the "Wide" component of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) with predictions of an analytic halo occupation distribution (HOD) model where the number of galaxies in each halo depends only on the halo mass. Starting from a parent catalogue of ∼3 × 10 6 galaxies at i AB < 22.5 we use accurate photometric redshifts calibrated using ∼10 4 spectroscopic redshifts to create a series of type-selected volume-limited samples covering 0.2 < z < 1.2. Our principal result, based on clustering measurements in these samples, is a robust determination of the luminosity-to-halo mass ratio and its dependence on redshift and galaxy type. For the full sample, this reaches a peak at low redshifts of M peak h = 4.5 × 10 11 h −1 M and moves towards higher halo masses at higher redshifts. For redder galaxies the peak is at higher halo masses and does not evolve significantly over the entire redshift range of our survey. We also consider the evolution of bias, average halo mass and the fraction of satellites as a function of redshift and luminosity. Our observed growth of a factor of ∼2 in satellite fraction between z ∼ 1 and z ∼ 0 is testament to the limited role that galaxy merging plays in galaxy evolution for ∼10 12 h −1 M mass haloes at z < 1. Qualitatively, our observations are consistent with a picture in which red galaxies in massive haloes have already accumulated most of their stellar mass by z ∼ 1 and subsequently undergo little evolution until the present day. The observed movement of the peak location for the full galaxy population is consistent with the bulk of star-formation activity migrating from higher mass haloes at high redshifts to lower mass haloes at lower redshifts.

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Section: Appendix A: the Halo Modelmentioning

confidence: 99%

Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes sincez ~ 1.2

Coupon

Kilbinger

McCracken

et al. 2012

A&A

172

245

View full text Add to dashboard Cite

show abstract

“…This means that shocks in the inner regions of clusters may not be fully reproduced. However, those shocks in high-density regions are expected to be weak with low 8 The relation between r 200 and r vir is rather complicated and depends on cosmological parameters (e.g., Nakamura & Suto 1997;Bryan & Norman 1998;Eke et al 1998 Mach numbers of M s 2-3 (e.g., Vazza et al 2011), so their contribution to the production of CRs would not be significant (see the discussion in Section 2.3). Since this paper focuses on relatively strong, CR-producing shocks in the outskirts, having an uniform resolution throughout the entire simulation volume should be actually an advantage.…”

Section: Cluster Samplementioning

confidence: 99%

Shock Waves and Cosmic Ray Acceleration in the Outskirts of Galaxy Clusters

Hong

Ryu

Kang

et al. 2014

ApJ

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The outskirts of galaxy clusters are continuously disturbed by mergers and gas infall along filaments, which in turn induce turbulent flow motions and shock waves. We examine the properties of shocks that form within r 200 in sample galaxy clusters from structure formation simulations. While most of these shocks are weak and inefficient accelerators of cosmic rays (CRs), there are a number of strong, energetic shocks which can produce large amounts of CR protons via diffusive shock acceleration. We show that the energetic shocks reside mostly in the outskirts and a substantial fraction of them are induced by infall of the warm-hot intergalactic medium from filaments. As a result, the radial profile of the CR pressure in the intracluster medium is expected to be broad, dropping off more slowly than that of the gas pressure, and might be even temporarily inverted, peaking in the outskirts. The volume-integrated momentum spectrum of CR protons inside r 200 has the power-law slope of 4.25-4.5, indicating that the average Mach number of the shocks of main CR production is in the range of M s CR ≈ 3-4. We suggest that some radio relics with relatively flat radio spectrum could be explained by primary electrons accelerated by energetic infall shocks with M s 3 induced in the cluster outskirts.

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“…They also revealed that the concentration parameter of the NFW profile, namely the ratio of the virial radius to the scale radius, c vir = r vir /r s , is much higher than predicted by cosmological N -body simulations (e.g., Bullock et al 2001;Neto et al 2007). We note that the virial radius, r vir , within which the mean interior density is ∆ vir ≃ 110 (Nakamura & Suto 1997) times the critical mass density, ρ cr (z), at a cluster redshift is given by…”

Section: A Joint X-ray and Lensing Analysismentioning

confidence: 99%

SUZAKUOBSERVATION OF A1689: ANISOTROPIC TEMPERATURE AND ENTROPY DISTRIBUTIONS ASSOCIATED WITH THE LARGE-SCALE STRUCTURE

Kawaharada

Okabe

Umetsu

et al. 2010

ApJ

140

189

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We present results of new, deep Suzaku X-ray observations (160 ks) of the intracluster medium (ICM) in Abell 1689 out to its virial radius, combined with complementary data sets of the projected galaxy distribution obtained from the SDSS catalog and the projected mass distribution from our recent comprehensive weak and strong lensing analysis of Subaru/Suprime-Cam and HST/ACS observations. Faint X-ray emission from the ICM around the virial radius (r vir ∼ 15.′ 6) is detected at 4.0σ significance, thanks to low and stable X-ray background of Suzaku. The Suzaku observations reveal anisotropic gas temperature and entropy distributions in cluster outskirts of r 500 < ∼ r < ∼ r vir correlated with large-scale structure of galaxies in a photometric redshift slice around the cluster. The high temperature (∼ 5.4 keV) and entropy region in the northeastern (NE) outskirts is apparently connected to an overdense filamentary structure of galaxies outside the cluster. The gas temperature and entropy profiles in the NE direction are in good agreement, out to the virial radius, with that expected from a recent XMM-Newton statistical study and with an accretion shock heating model of the ICM, respectively. To the contrary, the other outskirt regions in contact with low density void environments have low gas temperatures (∼ 1.7 keV) and entropies, deviating from hydrostatic equilibrium. These anisotropic ICM features associated with large-scale structure environments suggest that the thermalization of the ICM occurs faster along overdense filamentary structures than along low-density void regions. We find that the ICM density distribution is fairly isotropic, with a threedimentional density slope of −2.29 ± 0.18 in the radial range of r 2500 < ∼ r < ∼ r 500 , and with −1.24in r 500 < ∼ r < ∼ r vir , which however is significantly shallower than the Navarro, Frenk, & White universal matter density profile in the outskirts, ρ ∝ r −3 . A joint X-ray and lensing analysis shows that the hydrostatic mass is lower than spherical lensing one (∼ 60 − 90%) but comparable to a triaxial halo mass within errors, at intermediate radii of 0.6r 2500 < ∼ r < ∼ 0.8r 500 . On the other hand, the hydrostatic mass within 0.4r 2500 is significantly biased as low as < ∼ 60%, irrespective of mass models. The thermal gas pressure within r 500 is, at most, ∼ 50-60% of the total pressure to balance fully the gravity of the spherical lensing mass, and ∼ 30-40% around the virial radius. Although these constitute lower limits when one considers the possible halo triaxiality, these small relative contributions of thermal pressure would require additional sources of pressure, such as bulk and/or turbulent motions.

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Strong Gravitational Lensing and Velocity Function as Tools to Probe Cosmological Parameters: Current Constraints and Future Predictions

Cited by 125 publications

References 70 publications

Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes sincez ~ 1.2

Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes sincez ~ 1.2

Shock Waves and Cosmic Ray Acceleration in the Outskirts of Galaxy Clusters

SUZAKUOBSERVATION OF A1689: ANISOTROPIC TEMPERATURE AND ENTROPY DISTRIBUTIONS ASSOCIATED WITH THE LARGE-SCALE STRUCTURE

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