Scale dependence of galaxy biasing investigated by weak gravitational lensing: An assessment using semi-analytic galaxies and simulated lensing data

Simon, Patrick; Hilbert, Stefan

doi:10.1051/0004-6361/201732248

Cited by 33 publications

(30 citation statements)

References 115 publications

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“…In particular, the galaxygalaxy lensing shear profiles (e.g. Ziour & Hui 2008;Hilbert et al 2009;Simon & Hilbert 2018;Ghosh et al 2018), higherorder moments of the convergence field (Petri et al 2017a) and lensing bispectrum ) may require one to go beyond first order and undeflected light rays (Petri et al 2017b).…”

Section: Weak Gravitational Lensingmentioning

confidence: 99%

The accuracy of weak lensing simulations

Hilbert

Barreira

Fabbian

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We investigate the accuracy of weak lensing simulations by comparing the results of five independently developed lensing simulation codes run on the same input N -body simulation. Our comparison focuses on the lensing convergence maps produced by the codes, and in particular on the corresponding PDFs, power spectra and peak counts. We find that the convergence power spectra of the lensing codes agree to 2% out to scales ≈ 4000. For lensing peak counts, the agreement is better than 5% for peaks with signal-to-noise 6. We also discuss the systematic errors due to the Born approximation, line-of-sight discretization, particle noise and smoothing. The lensing codes tested deal in markedly different ways with these effects, but they nonetheless display a satisfactory level of agreement. Our results thus suggest that systematic errors due to the operation of existing lensing codes should be small. Moreover their impact on the convergence power spectra for a lensing simulation can be predicted given its numerical details, which may then serve as a validation test.

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Section: Weak Gravitational Lensingmentioning

confidence: 99%

The accuracy of weak lensing simulations

Hilbert

Barreira

Fabbian

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…In contrast, the overall tracer bias, which is typically weighted towards the most overdense structures in the Universe, has remained an active topic of research for a long time, due to its complex non-linear behaviour on intermediate and small scales (e.g. Smith et al 2007;Cacciato et al 2012;Dvornik et al 2018;Simon & Hilbert 2018;Springel et al 2018, and references therein). Moreover, recent evidence for additional stochasticity Table 2.…”

Section: O N C L U S I O N Smentioning

confidence: 99%

On the relative bias of void tracers in the Dark Energy Survey

Pollina

Hamaus

Paech

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Luminous tracers of large-scale structure are not entirely representative of the distribution of mass in our Universe. As they arise from the highest peaks in the matter density field, the spatial distribution of luminous objects is biased towards those peaks. On large scales, where density fluctuations are mild, this bias simply amounts to a constant offset in the clustering amplitude of the tracer, known as linear bias. In this work we focus on the relative bias between galaxies and galaxy clusters that are located inside and in the vicinity of cosmic voids, extended regions of relatively low density in the large-scale structure of the Universe. With the help of mock data we verify that the relation between galaxy and cluster overdensity around voids remains linear. Hence, the void-centric density profiles of different tracers can be linked by a single multiplicative constant. This amounts to the same value as the relative linear bias between tracers for the largest voids in the sample. For voids of small sizes, which typically arise in higher density regions, this constant has a higher value, possibly showing an environmental dependence similar to that observed for the linear bias itself. We confirm our findings by analysing data obtained during the first year of observations by the Dark Energy Survey. As a side product, we present the first catalogue of three-dimensional voids extracted from a photometric survey with a controlled photo-z uncertainty. Our results will be relevant in forthcoming analyses that attempt to use voids as cosmological probes.

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“…Hirata & Seljak 2004;Unruh et al 2020). In particular, intrinsic alignments (IA) have to be included in the lensing signal to reach an accuracy of several per cent for b(k) and r(k), as demonstrated in Simon & Hilbert (2018) (hereafter SH18) by using mock galaxy and shear catalogues that are similar to ours here. We apply the SH18 procedure with some improvements to measure the functions in Eqs.…”

Section: Introductionmentioning

confidence: 70%

“…The impact of magnification on N 2 , on other hand, is negligible but nevertheless included here (using Equation 36 in SH18). 4 In Simon & Hilbert (2018) there is a missing minus sign for F ia (χ) in their Eq. (31) and a typo in the pre-factor of P mb nκ ( ) ≡ P (2) nκ ( ) in their Eq.…”

Section: Intrinsic Alignment and Magnification Biasmentioning

confidence: 99%

CFHTLenS: Galaxy bias as function of scale, stellar mass, and colour

Simon

Hilbert

2021

A&A

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Galaxy models predict a tight relation between the clustering of galaxies and dark matter on cosmological scales, but predictions differ notably in the details. We used this opportunity and tested two semi-analytic models by the Munich and Durham groups with data from the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS). For the test we measured the scale-dependent galaxy bias factor b(k) and correlation factor r(k) from linear to non-linear scales of k ≈ 10 h Mpc −1 at two redshiftsz = 0.35, 0.51 for galaxies with stellar mass between 5 × 10 9 and 3 × 10 11 h −2 70 M. Our improved gravitational lensing technique accounts for the intrinsic alignment of sources and the magnification of lens galaxies for better constraints for the galaxy-matter correlation r(k). Galaxy bias in CFHTLenS increases with k and stellar mass; it is colour-dependent, revealing the individual footprints of galaxy types. Despite a reasonable model agreement for the relative change with both scale and galaxy properties, there is a clear conflict for b(k) with no model preference: the model galaxies are too weakly clustered. This may flag a model problem at z 0.3 for all stellar masses. As in the models, however, there is a high correlation r(k) between matter and galaxy density on all scales, and galaxy bias is typically consistent with a deterministic bias on linear scales. Only our blue and low-mass galaxies of about 7 × 10 9 h −2 70 M atz = 0.51 show, contrary to the models, a weak tendency towards a stochastic bias on linear scales where r ls = 0.75 ± 0.14 (stat.) ± 0.06 (sys.). This result is of interest for cosmological probes, such as E G , that rely on a deterministic galaxy bias. We provide Monte Carlo realisations of posterior constraints for b(k) and r(k) in CFHTLenS for every galaxy sample in this paper as online material.

show abstract

Scale dependence of galaxy biasing investigated by weak gravitational lensing: An assessment using semi-analytic galaxies and simulated lensing data

Cited by 33 publications

References 115 publications

The accuracy of weak lensing simulations

The accuracy of weak lensing simulations

On the relative bias of void tracers in the Dark Energy Survey

CFHTLenS: Galaxy bias as function of scale, stellar mass, and colour

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