Effects of Galaxy Formation on Thermodynamics of the Intracluster Medium

Nagai, Daisuke; Kravtsov, Andrey V.; Vikhlinin, A.

doi:10.1086/521328

Cited by 669 publications

(944 citation statements)

References 93 publications

(199 reference statements)

Supporting

Mentioning

858

Contrasting

Unclassified

Order By: Relevance

“…Our finding that the hydrostatic X-ray masses are larger than the weak lensing masses contradicts the results from many recent numerical simulations, all of which conclude that the hydrostatic assumption underestimates the true mass owing to its neglect of pressure support from gas bulk motions (e.g., Nagai et al 2007;Piffaretti & Valdarnini 2008;Meneghetti et al 2010). If the weak lensing mass is indeed unbiased (or less biased) and thus, on average, more representative of the true mass, then one would expect the weak lensing masses to be larger than the hydrostatic X-ray masses.…”

Section: The Mass Discrepancycontrasting

confidence: 91%

“…We then fitted the pressure profile of each cluster with the generalised Navarro, Frank & White (GNFW) model introduced by Nagai et al (2007), viz.,…”

Section: X-ray Pressure Profilementioning

confidence: 99%

“…Moreover, the majority of mass measurements used to date (e.g., Benson et al 2004;Bonamente et al 2008;Andersson et al 2011;Planck Collaboration 2011f) have relied on X-ray observations that assume hydrostatic equilibrium, which many theoretical studies tell us is likely to result in a mass that is systematically underestimated by about 10-15 percent due to neglect of bulk motions in the intracluster medium (ICM; e.g. Nagai et al 2007;Piffaretti & Valdarnini 2008;Meneghetti et al 2010). This effect is now commonly referred to in the literature as the "hydrostatic mass bias".…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Planckintermediate results

Ade¹,

Aghanim²,

Arnaud³

et al. 2013

A&A

View full text Add to dashboard Cite

We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal D 2 A Y 500 for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data, and the SZ effect signal is measured from Planck all-sky survey data. We find an M WL −D 2 A Y 500 relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R 500 are on average ∼20 percent larger than the corresponding weak lensing masses, which is contrary to expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods and, for the present sample, that the mass discrepancy and difference in mass concentration are especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations.

show abstract

Section: The Mass Discrepancycontrasting

confidence: 91%

“…We then fitted the pressure profile of each cluster with the generalised Navarro, Frank & White (GNFW) model introduced by Nagai et al (2007), viz.,…”

Section: X-ray Pressure Profilementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Planckintermediate results

Ade¹,

Aghanim²,

Arnaud³

et al. 2013

A&A

View full text Add to dashboard Cite

show abstract

“…This quantity reflects the total thermal energy of the ICM and is predicted to be a robust, low scatter mass proxy from simulations (e.g. Kravtsov et al 2006;Nagai et al 2007) which has recently been well confirmed by observations (e.g. Arnaud et al 2007;Vikhlinin et al 2009a;Arnaud et al 2010).…”

Section: Y Xmentioning

confidence: 58%

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

Fassbender

Böhringer

Santos

et al. 2011

A&A

View full text Add to dashboard Cite

Context. Observations of the formation and evolution of massive galaxy clusters and their matter components provide crucial constraints on cosmic structure formation, the thermal history of the intracluster medium (ICM), galaxy evolution, transformation processes, and gravitational and hydrodynamic interaction physics of the subcomponents. Aims. We characterize the global multi-wavelength properties of the X-ray selected galaxy cluster XMMU J1230.3+1339 at z = 0.975, a new system discovered within the XMM-Newton Distant Cluster Project (XDCP). We measure and compare various widely used mass proxies and identify multiple cluster-associated components from the inner core region out to the large-scale structure environment.Methods. We present a comprehensive galaxy cluster study based on a joint analysis of X-ray data, optical imaging and spectroscopy observations, weak lensing results, and radio properties for achieving a detailed multi-component view on a system at z ∼ 1. Results. We find an optically very rich and massive system with M 200 (4.2 ± 0.8) × 10 14 M , T X,2500 5.3 +0.7 −0.6 keV, and L bol X,500 (6.5 ± 0.7) × 10 44 erg s −1 . We have identified a central fly-through group close to core passage and find marginally extended 1.4 GHz radio emission possibly associated with the turbulent wake region of the merging event. On the cluster outskirts we see evidence for an on-axis infalling group with a second brightest cluster galaxy (BCG) and indications for an additional off-axis group accretion event. We trace two galaxy filaments beyond the nominal cluster radius and provide a tentative reconstruction of the 3D-accretion geometry of the system. Conclusions. In terms of total mass, ICM structure, optical richness, and the presence of two dominant BCG-type galaxies, the newly confirmed cluster XMMU J1230.3+1339 is likely the progenitor of a system very similar to the local Coma cluster, differing by 7.6 Gyr of structure evolution. This new system is an ideally suited astrophysical model laboratory for in-depth follow-up studies on the aggregation of baryons in the cold and hot phases.

show abstract

“…Inside this high-pressure tube, we model the pressure with a power-law function that depends only on the radial distance from the Coma centre: P tube (r) = P s (r/r s ) γ , where r is the radial distance, r s is a constant and P s and γ are the model parameters. This pressure tube is placed over a spherically symmetric generalized Navarro-Frenk-White (GNFW) pressure model (Nagai, Kravtsov & Vikhlinin 2007;Arnaud et al 2010) for the Coma cluster, which is constrained from the SZ-data excluding the radio relic wedge. We let the pressure excess terminate at the radio relic position (or any arbitrary position determined by the SZE data alone), beyond which the SZE signal is contributed only from the main cluster's GNFW pressure.…”

Section: Modelsmentioning

confidence: 99%

Evidence for a pressure discontinuity at the position of the Coma relic from Planck Sunyaev–Zel'dovich effect data

Erler

Basu

Trasatti

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Radio relics are Mpc-scale diffuse synchrotron sources found in galaxy cluster outskirts. They are believed to be associated with large-scale shocks propagating through the intracluster medium, although the connection between radio relics and the cluster merger shocks is not yet proven conclusively. We present a first tentative detection of a pressure jump in the well-known relic of the Coma cluster through Sunyaev-Zel'dovich (SZ) effect imaging. The SZE data are extracted from the first public all-sky data release of Planck and we use highfrequency radio data at 2.3 GHz to constrain the shock-front geometry. The SZE data provide evidence for a pressure discontinuity, consistent with the relic position, without requiring any additional prior on the shock-front location. The derived Mach number M = 2.9 +0.8 −0.6 is consistent with X-ray and radio results. A high-pressure "filament" without any pressure discontinuity is disfavoured by X-ray measurements and a "sub-cluster" model based on the infalling group NGC 4839 can be ruled out considering the published mass estimates for this group. These results signify a first attempt towards directly measuring the pressure discontinuity for a radio relic and the first SZ-detected shock feature observed near the virial radius of a galaxy cluster.

show abstract

Effects of Galaxy Formation on Thermodynamics of the Intracluster Medium

Cited by 669 publications

References 93 publications

Planckintermediate results

Planckintermediate results

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

Evidence for a pressure discontinuity at the position of the Coma relic from Planck Sunyaev–Zel'dovich effect data

Contact Info

Product

Resources

About