The Influence of Baryons on the Clustering of Matter and Weak-Lensing Surveys

By Y. Jing, Pengjie Zhang, Weipeng Lin, Liang Gao, Volker Springel. 2005

169 citations recorded by the source corpus.

Future weak-lensing measurements of cosmic shear will reach such high accuracy that second-order effects in weak-lensing modeling, such as the influence of baryons on structure formation, become important. We use a controlled set of high-resolution cosmological simulations to quantify this effect by comparing pure N-body dark matter runs with corresponding hydrodynamic simulations, carried out both in nonradiative form and in dissipative form with cooling and star formation. In both hydrodynamic simulations, the clustering of the gas is suppressed while that of dark matter is boosted at scales k > 1 h Mpc-1. Despite this counterbalance between dark matter and gas, the clustering of the total matter is suppressed by up to 1% at 1 h Mpc-1 ≲ k ≲ 10 h Mpc-1, while for k ≈ 20 h Mpc-1 it is boosted, up to 2% in the nonradiative run and 10% in the run with star formation. The stellar mass formed in the latter is highly biased relative to the dark matter in the pure N-body simulation. Using our power spectrum measurements to predict the effect of baryons on the weak-lensing signal at scales corresponding to multipole moments 100 < l < 10,000, we find that baryons may change the lensing power spectrum by less than 0.5% at l < 1000, but by 1% to 10% at 1000 < l < 10,000. The size of the effect exceeds the predicted accuracy of future lensing power spectrum measurements and will likely be detected. Precise determinations of cosmological parameters with weak lensing, and studies of small-scale fluctuations and clustering, therefore rely on properly including baryonic physics.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9a5177db931067dd424e0a82bac75db34c8385d6

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Citations in the corpus

Neutrino Mass in Cosmology: Status and Prospects (2011, background): “The study of [54] finds that baryon physics can contribute an uncertainty of up to 10% at multipole ` > 1000 corresponding to physical scales k of less than a factor of ten beyond the linear regime.”
The effects of galaxy formation on the matter power spectrum: a challenge for precision cosmology (2011, methodology): “Hence, using the simulation NOZCOOL, we reproduce both the qualitative and quantitative results of Jing et al. (2006), even though baryonic processes such as SN feedback are not implemented in the same way.”
CFHTLenS: combined probe cosmological model comparison using 2D weak gravitational lensing (2012, background): “The resulting bias on cosmological parameters is smaller than the CFHTLenS statistical errors 13 www.icosmo.org Downloaded from https://academic.oup.com/mnras/article-abstract/430/3/2200/981767 by guest on 27 July 2018 (Jing et al. 2006; Rudd, Zentner & Kravtsov 2008; Semboloni et al. 2011).”
A Fitting Formula for the Merger Timescale of Galaxies in Hierarchical Clustering (2007, methodology): “The simulation has the same mass resolution and model parameters as the star formation run of Jing et al. (2006), except that the softening length of the gravitational force is greatly reduced in the current simulation, where we use a spline kernel (Springel 2005), roughly equivalent to a Plummer…”
Strong-lensing optical depths in a ΛCDM universe – II. The influence of the stellar mass in galaxies (2007, background): “The effects of the baryons on the dark-matter profile and their relevance for lensing (see, e.g., Puchwein et al. 2005; Jing et al. 2006; Rozo et al. 2006; Wambsganss et al. 2008) are not the primary focus of this work, so we neglect these effects in the following.”
Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data (2018, methodology): “There are also uncertainties in modeling the matter power spectrum on small scales due to baryonic effects such as star formation and supernovae and AGN feedbacks (White 2004; Zhan & Knox 2004; Huterer & Takada 2005; Jing et al. 2006; Bernstein 2009; Semboloni et al. 2011).”
Cosmological parameter constraints from galaxy-galaxy lensing and galaxy clustering with the SDSS DR7 (2012, background): “…to predict the non-linear power spectrum (e.g., Heitmann et al. 2010) in the absence of modifications due to gas physics, which may be significant on the scales used for typical weak lensing analyses (Zhan & Knox 2004; Jing et al. 2006; Rudd et al. 2008; Zentner et al. 2008; Semboloni et al. 2011).”
REVISING THE HALOFIT MODEL FOR THE NONLINEAR MATTER POWER SPECTRUM (2012, background): “The baryon cooling would enhance the power at small scales by some ten percent at k = 10 h Mpc−1 and the enhancement becomes more significant for smaller scales (e.g., Jing et al. 2006; Rudd et al. 2008; Casarini et al. 2011b, 2012; van Daalen et al. 2011).”
Gravitational lensing (2010, background): “Precise knowledge of the nonlinear power spectrum is important on angular scales smaller than ∼10′ [188], where baryons can also change the dark-matter power spectrum noticeably [233].”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “However, for k > 2 – 3h Mpc−1 neglecting baryon physics is no longer accurate [642, 1023, 207, 1271, 576].”
Formation of Galaxy Clusters (2012, background): “The larger range of radii over which this effect operates makes it a potential worry for the precision constraints from the cosmic shear power spectrum (Jing et al. 2006; Rudd, Zentner & Kravtsov 2008).”
Optimal Surveys for Weak Lensing Tomography (2006, background): “In particular, the role played by baryons is not well understood at present (Zhan and Knox 2004; Jing et al. 2006).”
The Intrinsic Alignment of Galaxies and its Impact on Weak Gravitational Lensing in an Era of Precision Cosmology (2014, methodology): “This kind of marginalization process was shown to be successful by Joachimi and Bridle (2010); Kirk et al.”