Characterizing strong lensing galaxy clusters using the Millennium-XXL and moka simulations

Giocoli, Carlo; Bonamigo, Mario; Limousin, M.; Meneghetti, M.; Moscardini, L.; Angulo, Raúl E.; Despali, Giulia; Jullo, Eric

doi:10.1093/mnras/stw1651

Cited by 12 publications

(8 citation statements)

References 113 publications

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“…Not only do the line-of-sight structures introduce a systematic error in the strong lensing modelling (eg. Bayliss et al 2014;Giocoli et al 2016) but also distant massive structures in the lens plane have a considerable impact in the position of multiple images (Tu et al 2008;Limousin et al 2010) and thus on the mass constraints. Indeed, in Mahler et al (2017) the authors evaluate the impact of the presence of mass clumps in the outskirts of the cluster core of Abell 2744 (Jauzac et al 2016) to change the mass profile by ∼ 6% at 200kpc.…”

Section: Estimation Of ω M and Wmentioning

confidence: 99%

Hubble Frontier Fields: systematic errors in strong lensing models of galaxy clusters – implications for cosmography

Acebrón

Jullo

Limousin

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Strong gravitational lensing by galaxy clusters is a fundamental tool to study dark matter and constrain the geometry of the Universe. Recently, the HST Frontier Fields program has allowed a significant improvement of mass and magnification measurements but lensing models still have a residual RMS between 0.2" and few arcseconds, not yet completely understood. Systematic errors have to be better understood and treated in order to use strong lensing clusters as reliable cosmological probes. We have analysed two simulated Hubble Frontier Fields-like clusters from the Hubble Frontier Fields Comparison Challenge, Ares and Hera. We use several estimators (relative bias on magnification, density profiles, ellipticity and orientation) to quantify the goodness of our reconstructions by comparing our multiple models, optimized with the parametric software Lenstool, with the input models. We have quantified the impact of systematic errors arising, first, from the choice of different density profiles and configurations and, secondly, from the availability of constraints (spectroscopic or photometric redshifts, redshift ranges of the background sources) in the parametric modelling of strong lensing galaxy clusters and therefore on the retrieval of cosmological parameters. We find that substructures in the outskirts have a significant impact on the position of the multiple images, yielding tighter cosmological contours. The need for wide-field imaging around massive clusters is thus reinforced. We show that competitive cosmological constraints can be obtained also with complex multimodal clusters and that photometric redshifts improve the constraints on cosmological parameters when considering a narrow range of (spectroscopic) redshifts for the sources.

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Section: Estimation Of ω M and Wmentioning

confidence: 99%

Hubble Frontier Fields: systematic errors in strong lensing models of galaxy clusters – implications for cosmography

Acebrón

Jullo

Limousin

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…(2014, see also Giocoli et al 2016) discuss how selection effects may bias the measured concentration−mass relation at cluster scales, yielding up to 30% higher concentrations than what predicted by N-body simulations (see also Auger et al 2013;Sereno et al 2015;Lieu et al 2017). Several studies have also highlighted the possibility of biases arising from halo triaxiality (e.g., Foëx et al 2014).…”

Section: Dependence On Host Halo Massmentioning

confidence: 99%

Revisiting the Bulge–Halo Conspiracy. I. Dependence on Galaxy Properties and Halo Mass

Shankar

Sonnenfeld

Mamon

et al. 2017

ApJ

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We carry out a systematic investigation of the total mass density profile of massive (log M star /M ⊙ 11.3) early-type galaxies and its dependence on galactic properties and host halo mass with the aid of a variety of lensing/dynamical data and large mock galaxy catalogs. The latter are produced via semi-empirical models that, by design, are based on just a few basic input assumptions. Galaxies, with measured stellar masses, effective radii and Sérsic indices, are assigned, via abundance matching relations, host dark matter halos characterized by a typical ΛCDM profile. Our main results are as follows: (i) In line with observational evidence, our semi-empirical models naturally predict that the total, mass-weighted density slope at the effective radius γ ′ is not universal, steepening for more compact and/or massive galaxies, but flattening with increasing host halo mass. (ii) Models characterized by a Salpeter or variable initial mass function and uncontracted dark matter profiles are in good agreement with the data, while a Chabrier initial mass function and/or adiabatic contractions/expansions of the dark matter halos are highly disfavored. (iii) Currently available data on the mass density profiles of very massive galaxies (log M star /M ⊙ 12), with M halo 3 × 10 14 M ⊙ , favor instead models with a stellar profile flatter than a Sérsic one in the very inner regions (r 3 − 5 kpc), and a cored NFW or Einasto dark matter profile with median halo concentration a factor of ∼ 2 or 1.3, respectively, higher than those typically predicted by N-body numerical simulations.

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“…We find from Fig. 7 that SIS profile can still match the SQLS observations well, whilst NFW predicts the lensing probabilities that are about an order of magnitude lower than the observations (Giocoli et al 2016). The usually employed standard model SIS+NFW breaks down for large image separations.…”

Section: Lensing Probabilitiesmentioning

confidence: 66%

Baryon effects on the dark matter haloes constrained from strong gravitational lensing

Wang¹,

Chen²,

Li³

2017

Monthly Notices of the Royal Astronomical Society

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Simulations are expected to be the powerful tool to investigate the baryon effects on dark matter (DM) halos. Recent high resolution, cosmological hydrodynamic simulations (Di Cintio et al. 2014, DC14) predict that the inner density profiles of DM halos depend systematically on the ratio of stellar to DM mass (M * /M halo ) which is thought to be able to provide good fits to the observed rotation curves of galaxies. The DC14 profile is fitted from the simulations which are confined to M halo ≤ 10 12 M ⊙ , in order to investigate the physical processes that may affect all halos, we extrapolate it to much larger halo mass, including that of galaxy clusters. The inner slope of DC14 profile is flat for low halo mass, it approaches 1 when the halo mass increases towards 10 12 M ⊙ and decreases rapidly after that mass. We use DC14 profile for lenses and find that it predicts too few lenses compared with the most recent strong lensing observations SQLS (Inada et al. 2012). We also calculate the strong lensing probabilities for a simulated density profile which continues the halo mass from the mass end of DC14 (∼ 10 12 M ⊙ ) to the mass that covers the galaxy clusters (Schaller et al. 2015, Schaller15), and find that this Schaller15 model predict too many lenses compared with other models and SQLS observations. Interestingly, Schaller15 profile has no core, however, like DC14, the rotation curves of the simulated halos are in excellent agreement with observational data. Furthermore, we show that the standard two-population model SIS+NFW cannot match the most recent SQLS observations for large image separations.

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Characterizing strong lensing galaxy clusters using the Millennium-XXL and moka simulations

Cited by 12 publications

References 113 publications

Hubble Frontier Fields: systematic errors in strong lensing models of galaxy clusters – implications for cosmography

Hubble Frontier Fields: systematic errors in strong lensing models of galaxy clusters – implications for cosmography

Revisiting the Bulge–Halo Conspiracy. I. Dependence on Galaxy Properties and Halo Mass

Baryon effects on the dark matter haloes constrained from strong gravitational lensing

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