Scaling relations for galaxy clusters in the Millennium-XXL simulation

By R. Angulo, Volker Springel, Simon D. M. White, Adrian Jenkins, C. Baugh, Carlos S. Frenk. 2012

383 citations recorded by the source corpus.

We present a very large high-resolution cosmological N-body simulation, the Millennium-XXL or MXXL, which uses 303 billion particles to represent the formation of dark matter structures throughout a 4.1 Gpc box in a Λ cold dark matter cosmology. We create sky maps and identify large samples of galaxy clusters using surrogates for four different observables: richness estimated from galaxy surveys, X-ray luminosity, integrated Sunyaev–Zeldovich (SZ) signal and lensing mass. The unprecedented combination of volume and resolution allows us to explore in detail how these observables scale with each other and with cluster mass. The scatter correlates between different mass–observable relations because of common sensitivities to the internal structure, orientation and environment of clusters, as well as to line-of-sight superposition of uncorrelated structure. We show that this can account for the apparent discrepancies uncovered recently between the mean thermal SZ signals measured for optically and X-ray selected clusters by stacking data from the Planck satellite. Related systematics can also affect inferences from extreme clusters detected at high redshift. Our results illustrate that cosmological conclusions from galaxy cluster surveys depend critically on proper modelling, not only of the relevant physics, but also of the full distribution of the observables and of the selection biases induced by cluster identification procedures.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/87971c87c8685b798acdf8c35210ad81faf3eae7

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Citations in the corpus

COLOSSUS: A Python Toolkit for Cosmology, Large-scale Structure, and Dark Matter Halos (2017, methodology): “…on numerical results (FOF, explicit z-dependence) courtin11 Courtin et al. 2011 A calibration based on numerical results (FOF, uses fixed δc = 1.673) angulo12 Angulo et al. 2012 A calibration based on numerical results (FOF, no z-dependence) watson13 Watson et al. 2013 Both FOF and SO fits,…”
The universality of the virial halo mass function and models for non-universality of other halo definitions (2015, background): “In the Cold Dark Matter (CDM) model, structures – up to protogalactic scales – form through the amplification of small density fluctuations via gravitational instability (Longair 1998; Springel et al. 2005; Mo et al. 2010; Angulo et al. 2012).”
The COSMOS2015 galaxy stellar mass function . Thirteen billion years of stellar mass assembly in ten snapshots (2017, neutral): “The code allows us to choose among alternate models (e.g. Sheth et al. 2001; Tinker et al. 2010; Angulo et al. 2012) without any significant impact on our conclusions.”
Modelling baryon acoustic oscillations with perturbation theory and stochastic halo biasing (2013, background): “…needs to cover is extremely large, ranging from varying the cosmological parameters, over modelling different biased tracers, to account for cosmic variance (for large-volume N -body simulations see e.g. Kim et al. 2009; Prada et al. 2012; Angulo et al. 2012; Alimi et al. 2012; Watson et al. 2013).”
Core Cosmology Library: Precision Cosmological Predictions for LSST (2018, methodology): “This basic form is modified for the Angulo et al. (2012) formulation.”
Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe (2014, background): “…although the physical nature of DM and DE remain unknown, their evolution can be followed far into the non-linear regime using collisionless N-body simulations (e.g. Springel et al. 2005b, 2008; Boylan-Kolchin et al. 2009; Klypin, Trujillo-Gomez & Primack 2011; Angulo et al. 2012; Wu et al. 2013).”
The SPTpol Extended Cluster Survey (2019, background): “We note that we expect positive correlation in the scatter between ζ and λ, as both are projected quantities (see, e.g., Angulo et al. 2012).”
Weak Lensing Measurement of the Mass--Richness Relation of SDSS redMaPPer Clusters (2016, background): “Indeed, this effect has been seen in numerical simulations (Angulo et al. 2012; Noh & Cohn 2012).”
Observational probes of cosmic acceleration (2012, background): “Biesiadzinski et al. (2012) have attributed this inconsistency to miscentering, while Angulo et al. (2012) point out the importance of systematics covariance.”
Baryon impact on the halo mass function: Fitting formulae and implications for cluster cosmology (2015, background): “…functions (e.g. Jenkins et al. 2001; Sheth, Mo & Tormen 2001; White, Hernquist & Springel 2002; Reed et al. 2003; Warren et al. 2006; Lukić et al. 2007; Reed et al. 2007; Tinker et al. 2008; Crocce et al. 2010; Bhattacharya et al. 2011; Courtin et al. 2011; Angulo et al. 2012; Watson et al. 2013).”
The halo mass function through the cosmic ages (2012, methodology): “2002) and Jenkins et al. (Jenkins et al. 2001) fits, as well as a number of more recent fits (Reed et al. 2003, 2007; Warren et al. 2006; Crocce et al. 2010; Bhattacharya et al. 2011; Courtin et al. 2011; Angulo et al. 2012).”
First results from the IllustrisTNG simulations: matter and galaxy clustering (2017, methodology): “18 to a similar analysis carried out by Angulo et al. (2014) for the Millennium-XXL simulation (Angulo et al. 2012) on the basis of a semi-analytic galaxy formation model.”
Structure finding in cosmological simulations: the state of affairs (2013, background): “Such an approach obviates the need to frequently save the raw simulation output, instead only requiring the storing of much smaller reduced catalogues of the interesting structures and their properties (Angulo et al. 2012).”
Theoretical Challenges in Galaxy Formation (2016, methodology): “…calculation, but other simulations (Klypin, Trujillo-Gomez & Primack 2011) also of Theoretical Challenges in Galaxy Formation 7 larger volumes (Angulo et al. 2012) or constrained to a certain halo mass scale (Diemand, Kuhlen & Madau 2007; Gao et al. 2012; Springel et al. 2008; Stadel et al.…”
The mass–concentration–redshift relation of cold dark matter haloes (2013, methodology): “(MS-XXL is excluded from our zi = 2 analysis because particle data is unavailable for this redshift.)”
Halo and subhalo demographics with Planck cosmological parameters: Bolshoi–Planck and MultiDark–Planck simulations (2016, background): “…simulations that are particularly useful for studying galaxy hosts include the Millennium simulations (Springel et al. 2005; Boylan-Kolchin et al. 2009; Angulo et al. 2012), Bolshoi (Klypin, Trujillo-Gomez & Primack 2011), MultiDark (Prada et al. 2012; Riebe et al. 2013), Jubilee (Watson et al.…”
The mass profile and accretion history of cold dark matter haloes (2013, methodology): “Symbols of different colors are used for halos in each of the three mass bins, which correspond to different MS. Note that they all delineate the same trend, despite the fact that they span a range of roughly four decades in virial mass. Note as well that parameters corresponding to individual halos”