The LSST Dark Energy Science Collaboration (DESC) Science Requirements Document

Collaboration, The LSST Dark Energy Science; Mandelbaum, Rachel; Eifler, T. F.; Hložek, Renée; Collett, Thomas S; Gawiser, Eric; Scolnic, D.; Alonso, David; Awan, Humna; Biswas, R.; Blazek, Jonathan; Burchat, P. R.; Chisari, Nora Elisa; Dell’Antonio, Ian; Digel, S. W.; Frieman, J.; Goldstein, Daniel A.; Hook, I. M.; Ivezić, Željko; Kahn, S. M.; Kamath, S. Sowmya; Kirkby, D.; Kitching, Thomas D.; Krause, E.; Léget, P. F.; Marshall, Phil; Meyers, J.; Miyatake, Hironao; Newman, Jeffrey A.; Nichol, R. C.; Rykoff, E. S.; Sánchez, Flora; Slosar, Anže; Sullivan, M.; Troxel, M. A.

doi:10.48550/arxiv.1809.01669

Cited by 99 publications

(177 citation statements)

References 0 publications

Supporting

Mentioning

169

Contrasting

Order By: Relevance

“…(1) with an upper limit of max ∼ 3000. Following the Dark Energy Science Collaboration (DESC) requirements for the LSST Y10 weak lensing analysis (Mandelbaum et al 2018), we consider 20 equally spaced logarithmic angular bins ranging from 20 ∼ 3000, for each tomographic spectra.…”

Section: Modelling the Theoretical Error Covariancementioning

confidence: 99%

“…In order to compute the convergence angular power spectrum one needs to project the 3D power spectrum into different tomographic redshift bins. For the galaxy number distribution, we again DESC requirements for the LSST Y10 weak lensing analysis (Mandelbaum et al 2018). Hence, we use the following parametric form for the source redshift distribution n(z):…”

Section: Modelling the Theoretical Error Covariancementioning

confidence: 99%

See 1 more Smart Citation

Mitigating baryonic effects with a theoretical error covariance

Moreira,

Andrade-Oliveira,

Fang

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

One of the primary sources of uncertainties in modeling the cosmic-shear power spectrum on small scales is the effect of baryonic physics. Accurate cosmology for Stage-IV surveys requires knowledge of the matter power spectrum deep in the nonlinear regime at the percent level. Therefore, it is important to develop reliable mitigation techniques to take into account baryonic uncertainties if information from small scales is to be considered in the cosmological analysis. In this work, we develop a new mitigation method for dealing with baryonic physics for the case of the shear angular power spectrum. The method is based on an extended covariance matrix that incorporates baryonic uncertainties informed by hydrodynamical simulations. We use the results from 13 hydrodynamical simulations and the residual errors arising from a fit to a ΛCDM model using the extended halo model code HMCode to account for baryonic physics. These residual errors are used to model a so-called theoretical error covariance matrix that is added to the original covariance matrix. In order to assess the performance of the method, we use the 2D tomographic shear from four hydrodynamical simulations that have different extremes of baryonic parameters as mock data and run a likelihood analysis comparing the residual bias on Ω m and σ 8 of our method and the HMCode for an LSST-like survey. We use different modelling of the theoretical error covariance matrix to test the robustness of the method. We show that it is possible to reduce the bias in the determination of the tested cosmological parameters at the price of a modest decrease in the precision.

show abstract

Section: Modelling the Theoretical Error Covariancementioning

confidence: 99%

Section: Modelling the Theoretical Error Covariancementioning

confidence: 99%

Mitigating baryonic effects with a theoretical error covariance

Moreira,

Andrade-Oliveira,

Fang

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…The linear bias parameter estimates from the fiducial model fits in our analysis are 1.394±0.001, 1.649±0.001 and 1.880±0.002 for m i < 24.43, m i < 22.87 and m i < 21.80 samples, respectively. The LSST DESC Science Requirements Document (SRD) [61] assumed the form…”

Section: Comparison With Measurementsmentioning

confidence: 99%

“…FIG.12. Comparison of our linear bias parameter estimates with observations of HSC galaxy clustering[60], as well as the LSST DESC SRD[61].…”

mentioning

confidence: 99%

Perturbation theory models for LSST-era galaxy clustering: tests with sub-percent mock catalog measurements in Fourier and configuration space

Goldstein,

Pandey,

Slosar

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

We analyze the clustering of galaxies using the z = 1.006 snapshot of the CosmoDC2 simulation, a high-fidelity synthetic galaxy catalog designed to validate analysis methods for the Large Synoptic Survey Telescope (LSST). We present sub-percent measurements of the galaxy auto-correlation and galaxy-dark matter cross correlations in Fourier space and configuration space for a magnitudelimited galaxy sample. At these levels of precision, the statistical errors of the measurement are comparable to the systematic effects present in the simulation and measurement procedure; nevertheless, using a hybrid-PT model, we are able to model non-linear galaxy bias with 0.5% precision up to scales of kmax = 0.5 h/Mpc and rmin = 4 Mpc/h. While the linear bias parameter is measured with 0.01% precision, other bias parameters are determined with considerably weaker constraints and sometimes bimodal posterior distributions. We compare our fiducial model with lower dimensional models where the higher-order bias parameters are fixed at their co-evolution values and find that leaving these parameters free provides significant improvements in our ability to model small scale information. We also compare bias parameters for galaxy samples defined using different magnitude bands and find agreement between samples containing equal numbers of galaxies. Finally, we compare bias parameters between Fourier space and configuration space and find moderate tension between the two approaches. Although our model is often unable to fit the CosmoDC2 galaxy samples within the 0.1% precision of our measurements, our results suggest that the hybrid-PT model used in this analysis is capable of modeling non-linear galaxy bias within the percent level precision needed for upcoming galaxy surveys.

show abstract

“…We con-sider three LSS experiments: DESI, Vera Rubin Observatory Year 1 (VROY1) and Year 10 (VROY10). The parameters for VRO are based on [43,44] and those for DESI are based on [45]. For DESI, we take a 116 Gpc 3 box with galaxy survey density n g = 1.4 × 10 −4 /Mpc 3 and σ z = 0.…”

Section: B Redshift Space Distortionsmentioning

confidence: 99%

Transverse Velocities with the Moving Lens Effect

et al. 2019

View full text Add to dashboard Cite

Gravitational potentials which change in time induce fluctuations in the observed cosmic microwave background (CMB) temperature. Cosmological structure moving transverse to our line of sight provides a specific example known as the moving lens effect. Here we explore how the observed CMB temperature fluctuations combined with the observed matter over-density can be used to infer the transverse velocity of cosmological structure on large scales. We show that near-future CMB surveys and galaxy surveys will have the statistical power to make a first detection of the moving lens effect, and we discuss applications for the reconstructed transverse velocity.

show abstract

The LSST Dark Energy Science Collaboration (DESC) Science Requirements Document

Cited by 99 publications

References 0 publications

Mitigating baryonic effects with a theoretical error covariance

Mitigating baryonic effects with a theoretical error covariance

Perturbation theory models for LSST-era galaxy clustering: tests with sub-percent mock catalog measurements in Fourier and configuration space

Transverse Velocities with the Moving Lens Effect

Contact Info

Product

Resources

About