SIMULATIONS OF THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM WITH ACTIVE GALACTIC NUCLEUS FEEDBACK

By Nicholas Battaglia, J. Richard Bond, C. Pfrommer, Jonathan Sievers, D. Sijacki. 2010

164 citations recorded by the source corpus.

We explore how radiative cooling, supernova feedback, cosmic rays, and a new model of the energetic feedback from active galactic nuclei (AGNs) affect the thermal and kinetic Sunyaev–Zel'dovich (SZ) power spectra. To do this, we use a suite of hydrodynamical TreePM-SPH simulations of the cosmic web in large periodic boxes and tailored higher resolution simulations of individual galaxy clusters. Our AGN feedback simulations match the recent universal pressure profile and cluster mass scaling relations of the REXCESS X-ray cluster sample better than previous analytical or numerical approaches. For multipoles ℓ ≲ 2000, our power spectra with and without enhanced feedback are similar, suggesting that theoretical uncertainties over that range are relatively small, although current analytic and semi-analytic approaches overestimate this SZ power. We find the power at high 2000–10, 000 multipoles in which the Atacama Cosmology Telescope (ACT) and South Pole Telescope (SPT) probe is sensitive to the feedback prescription, and hence can constrain the theory of intracluster gas, in particular for the highly uncertain redshifts >0.8. The apparent tension between σ8 from primary cosmic microwave background power and from analytic SZ spectra inferred using ACT and SPT data is lessened with our AGN feedback spectra.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/ed7e415cc1e7b69eeb3dc6b9fb05416cbeca6a62

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Citations in the corpus

THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGY FROM GALAXY CLUSTERS DETECTED VIA THE SUNYAEV–ZEL'DOVICH EFFECT (2010, background): “These processes have a much larger impact on lower mass clusters and groups where the gravitational potential is not strong enough to tightly bind the cluster gas (e.g., Battaglia et al. 2010; Shaw et al. 2010; Trac et al. 2011).”
The Atacama Cosmology Telescope: likelihood for small-scale CMB data (2013, methodology): “Reionization of the universe is not expected to be instantaneous, as was assumed by Battaglia et al. (2010).”
The BAHAMAS project: Calibrated hydrodynamical simulations for large-scale structure cosmology (2016, result): “…up in groups relative to clusters, which is consistent with the findings of previous studies of X-ray bright systems (e.g., Sun et al. 2009) and the predictions of simulations with efficient AGN feedback (e.g., McCarthy et al. 2010; Battaglia et al. 2010; Planelles et al. 2014; L14).”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS (2012, background): “The 2-point function is a potentially-powerful probe of σ8 (Komatsu & Seljak 2002); however, it is sensitive to the low-mass end of the Y (M) scaling relation for clusters, which is subject to astrophysical corrections (Shaw et al. 2010; Battaglia et al. 2010, 2012a).”
THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGICAL PARAMETERS FROM THE 2008 POWER SPECTRUM (2010, methodology): “In this analysis we consider four thermal SZ templates, from Sehgal et al. (2010a), Trac, Bode, & Ostriker (2010), Battaglia et al. (2010), and Shaw et al. (2010).”
CMB-S4 Science Case, Reference Design, and Project Plan (2019, unknown): “[396, 397], EAGLE [398], and IllustrisTNG-300 [399, 400, 401].”
The Atacama Cosmology Telescope: cosmological parameters from three seasons of data (2013, unknown): “9 μK2 at ` = 3000 using the [11] template.”
The Atacama Cosmology Telescope: two-season ACTPol spectra and parameters (2016, methodology): “Following Dunkley et al. (2013) we use an alternative cosmic infrared background clustering template that differs at large scales, and an alternative thermal SZ template from Battaglia et al. (2010).”
A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS (2011, background): “S11 considered four tSZ models: a model by Sehgal et al. (2010) which predicts high levels of tSZ power and three models which all predicted lower tSZ powers (Battaglia et al. 2010; Shaw et al. 2010; Trac et al. 2011).”
A MEASUREMENT OF THE DAMPING TAIL OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM WITH THE SOUTH POLE TELESCOPE (2011, methodology): “The SZ component uses the thermal SZ template of Sehgal et al. (2010a), which has a shape similar to the templates from more recent models (Trac et al. 2011; Shaw et al. 2010; Battaglia et al. 2010), normalized to D` = 5.5 µK 2 at ` = 3000.”
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, methodology): “This model for AGN feedback is self-regulated (Battaglia et al. 2010) and injects∼ 2/3 of the energy beforez= 1 when the average cluster mass is significantly smaller and the associated potentials are shallower so that a fixed energy injection by AGNs may in principle have a stronger impact2.”
Planck intermediate results: V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect (2012, unknown): “03 for the B04 + N07 + P08, Dolag (in prep.) and Battaglia et al. (2010) simulations, respectively.”