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Systematic errors in future weak-lensing surveys: requirements and prospects for self-calibration
Open accessAbstract
We study the impact of systematic errors on planned weak-lensing surveys and compute the requirements on their contributions so that they are not a dominant source of the cosmological parameter error budget. The generic types of error we consider are multiplicative and additive errors in measurements of shear, as well as photometric redshift errors. In general, more powerful surveys have stronger systematic requirements. For example, for a SuperNova/Acceleration Probe (SNAP)-type survey the multiplicative error in shear needs to be smaller than 1 per cent of the mean shear in any given redshift bin, while the centroids of photometric redshift bins need to be known to be better than 0.003. With about a factor of 2 degradation in cosmological parameter errors, future surveys can enter a self-calibration regime, where the mean systematic biases are self-consistently determined from the survey and only higher order moments of the systematics contribute. Interestingly, once the power-spectrum measurements are combined with the bispectrum, the self-calibration regime in the variation of the equation of state of dark energy wa is attained with only a 20-30 per cent error degradation.
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“Higher-order shear and galaxy statistics and shear peak counts can improve dark energy constraints and provide self-calibration of various systematics ( Takada & Jain 2004; Dolney et al. 2006; Huterer et al. 2006; Petri et al. 2016 ) .”
From LSST: From Science Drivers to Reference Design and Anticipated Data Products (2019) · cites this paper as Huterer et al. 2006
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Items 201–300 of 407
Jones, E., & Singal, J. (2017) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201629558/pdf · Cited by 31
Spurious shear in weak lensing with the Large Synoptic Survey Telescope
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“Since γ = 0 in all our analyses, we can identify the ξγ γ measured in Section 7 to be the ‘additive spurious shear correlation function’ ξ sadd introduced in Huterer et al. (2006).”
BackgroundJoachimi, B., & Schneider, P. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201014482 · Cited by 31
“The bias formalism (e.g. Huterer et al. 2006; Amara & Réfrégier 2008; Joachimi & Schneider 2009) allows us to compute the bias on the intrinsic alignment parametersdue to the residual GG signal in the transformed power spectra via bsys(pµ) = ∑ ν ( F−1 ) µν (33) × ∑ ℓ ∑ i, j Π (i) GG(ℓ) Cov −1 ( Π…”
The impact of galaxy colour gradients on cosmic shear measurement
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Weighing the Universe with Photometric Redshift Surveys and the Impact on Dark Energy Forecasts
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Self-citationSánchez, C., Raveri, M., Alarcon, A., & Bernstein, G. M. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2542 · Cited by 30
“…corresponding galaxy samples, and systematic errors in that characterization may directly lead to biases in the cosmological parameter estimation (Huterer et al. 2006; Cunha et al. 2012; Hildebrandt et al. 2012, 2017; Benjamin et al. 2013; Huterer, Cunha & Fang 2013; Bonnett et al. 2016;…”
BackgroundSelf-citationStatistical uncertainties and systematic errors in weak lensing mass estimates of galaxy clusters
Köhlinger, F., Hoekstra, H., & Eriksen, M. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1852 · Cited by 30
“…shear γobs from the true shear γ c© 2015 RAS, MNRAS 000, 1–14 c© 2015 RAS, MNRAS 000, 1–14 can be written as (Heymans et al. 2006) γobs = (1 +m)γ + c , (27) where m refers to the multiplicative bias and c to the additive bias (e.g. Huterer et al. 2006; Massey et al. 2013 and references therein).”
BackgroundSize of spectroscopic calibration samples for cosmic shear photometric redshiftsPreprint
Bernstein, G. M., & Ma, Z. (2012) · Cited by 30
Self-citationMiyatake, H., Kobayashi, Y., Takada, M., Nishimichi, T., Shirasaki, M., Sugiyama, S., Takahashi, R., Osato, K., More, S., & Park, Y. (2022) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.106.083519 · Cited by 28
Self-citationFang, W., & Haiman, Z. (2007) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.75.043010 · Cited by 28
Exploring Large‐Scale Structure with Billions of Galaxies
Zhan, H., Knox, L., Tyson, J. A., & Margoniner, V. (2006) · The Astrophysical Journal · doi:10.1086/500077 · Cited by 28
“They can also reduce the uncertainties of the photometric redshift bias (Zhan & Knox 2006) and thus prevent the redshift bias from severely degrading the constraining power of the weak-lensing tomography on the dark energy equation-of-state parameters (Huterer et al. 2006;Ma et al. 2006).”
BackgroundSingal, J., Shmakova, M., Gerke, B. F., Griffith, R. L., & Lotz, J. M. (2011) · Publications of the Astronomical Society of the Pacific · doi:10.1086/660155 · Cited by 27
A roadmap to cosmological parameter analysis with third-order shear statistics
Heydenreich, S., Linke, L., Burger, P., & Schneider, P. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244820 · Cited by 27
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Joudaki, S., Cooray, A. R., & HOLZ, D. E. (2009) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.80.023003 · Cited by 27
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Wavelength-dependent PSFs and their impact on weak lensing measurements
Carlsten, S. G., Strauss, M. A., Lupton, R. H., Meyers, J. E., & Miyazaki, S. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1636 · Cited by 29
“Huterer et al. (2006) and Amara & Réfrégier (2008) estimate that for a weak lensing survey with the coverage of the Large Synoptic Survey Telescope (LSST) (LSST Science Collaboration et al. 2009), the average, uncorrected multiplicative bias to the shear needs to be .”
BackgroundJ-PAS: forecasts on dark energy and modified gravity theories
Resco, M. A., Maroto, A. L., Alcaniz, J. S., Abramo, L. R., Hernández-Monteagudo, C., Benítez, N., Carneiro, S., Cenarro, A. J., Cristòbal-Hornillos, D., Dupke, R. A., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa367 · Cited by 25
Cosmic shear requirements on the wavelength dependence of telescope point spread functions
Cypriano, E. S., Amara, A., Voigt, L. M., Bridle, S., Abdalla, F. B., Refregier, A. R., Seiffert, M. D., & Rhodes, J. D. (2010) · reroDoc Digital Library · doi:10.3929/ethz-b-000018626 · Cited by 26
A unified catalogue-level reanalysis of stage-III cosmic shear surveys
Longley, E. P., Chang, C., Walter, C. W., Zuntz, J., Ishak, M., Mandelbaum, R., Miyatake, H., Nicola, A., Pedersen, E. M., Pereira, M. E. S., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad246 · Cited by 26
The influence of galaxy formation physics on weak lensing tests of general relativity
Hearin, A. P., & Zentner, A. R. (2009) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2009/04/032 · Cited by 26
“To utilize this information at the level that forthcoming observational programs will permit, numerical simulations must be able to predict the nonlinear matter power spectra to better than a percent [36, 37].”
BackgroundCosmic shear as a probe of galaxy formation physics
Foreman, S., Becker, M. R., & Wechsler, R. H. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2189 · Cited by 25
“(11) Such a model was also used in Huterer et al. (2006), who pointed out that other additive systematics such as anisotropies in a telescope’s point-spread function will likely have a similar impact on the angular power spectrum.”
Forecast of neutrino cosmology from the CSST photometric galaxy clustering and cosmic shear surveys
Lin, H., Gong, Y., Chen, X., Chan, K. C., Fan, Z., & Zhan, H. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2126 · Cited by 25
Tidal alignments as a contaminant of the galaxy bispectrum
Krause, E., & Hirata, C. M. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.17638.x · Cited by 25
“To first order it is given by (e.g. Huterer et al. 2006; Amara & Réfrégier 2008) ∆pα = 〈 p̂α〉 − pfidα = ( F −1 ) αβ ~∆Pt Cov−1 ( ~P, ~P ) ∂~P ∂pβ + ~∆Bt Cov−1 ( ~B, ~B ) ∂ ~B ∂pβ , (60) where the data vectors and covariances are evaluated at the fiducial model.”
Atmospheric Dispersion Effects in Weak Lensing Measurements
Plazas, A. A., & Bernstein, G. M. (2012) · Publications of the Astronomical Society of the Pacific · doi:10.1086/668294 · Cited by 25
“s a function of source redshift, since most of the power of cosmic-shear experiments comes from tomographic analyses of detailed comparison between shear strength on different bins of source redshift. Huterer et al. (2006) (hereafter HTBJ) calculate the degradation of cosmological constraints for the DES and LSST cosmi…”
BackgroundSelf-citationPhotometric Redshift Estimation with Galaxy Morphology Using Self-organizing Maps
Wilson, D., Nayyeri, H., Cooray, A. R., & Häußler, B. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab5a79 · Cited by 24
“Errors in photometric redshifts can significantly affect cosmological parameter measurements in, for example, weak lensing studies (e.g., Huterer et al. 2006; Ma et al. 2006; Bernstein & Huterer 2010) and baryon acoustic oscillation studies (e.g., Zhan & Knox 2006; Chaves-Montero et al. 2018).”
BackgroundHierarchical Probabilistic Inference of Cosmic Shear
Schneider, M. D. H. (2021) · OSTI OAI (U.S. Department of Energy Office of Scientific and Technical Information) · Cited by 24
Consistency of cosmic shear analyses in harmonic and real space
Doux, C., Chang, C., Jain, B., Blazek, J., Camacho, H., Fang, X., Gatti, M., Krause, E., MacCrann, N., Samuroff, S., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab661 · Cited by 24
“To account for uncertainties in shear calibration, we model the observed shear γ iobs in redshift bin i from the true shear γ i by γ iobs = (1 + mi)γ i, (4) where mi is the multiplicative shear bias, constant within each redshift bin i (Heymans et al. 2006; Huterer et al. 2006).”
MethodSelf-citationMatthews, D. J., & Newman, J. A. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/745/2/180 · Cited by 25
“Many of the cosmological measurements to be performed with future photometric surveys will require extremely wellcharacterized redshift distributions (Albrecht et al. 2006; Huterer et al. 2006; Ma et al. 2006).”
BackgroundAbrahamse, A., Knox, L., Schmidt, S., Thorman, P., Tyson, J. A., & Zhan, H. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/734/1/36 · Cited by 24
“Huterer et al. (2006) assume that photo-z errors take the form of a bias that varies with z.”
BackgroundTests of neutrino and dark radiation models from galaxy and CMB surveys
Banerjee, A., Jain, B., Dalal, N., & Shelton, J. (2018) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2018/01/022 · Cited by 24
“See for example the discussion around figure 8 of [78], who show that unless the redshift uncertainty is very large, the two parameters are close to degenerate.”
BackgroundSelf-citationTonegawa, M., Okumura, T., Totani, T., Dalton, G., Glazebrook, K., & Yabe, K. (2018) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psy030 · Cited by 24
“We use a Fisher matrix approach (Huterer et al. 2006; Kirk et al. 2015), and the bias on α-th parameter ∆pα is evaluated as: ∆pα = ∑ β F−1αβ ∑ ℓ ∑ i≤j;m≤n ∆C (ij) GG (ℓ) ( Cov [ C (ij) GG (ℓ),C (mn) GG (ℓ) ])−1 ∂C(mn)GG (ℓ) ∂pβ , (22) where C (ij) GG (ℓ) is the cross-power spectrum between i-th and…”
Probing cosmology and cluster astrophysics with multiwavelength surveys – I. Correlation statistics
Shirasaki, M., Lau, E. T., & Nagai, D. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz3021 · Cited by 24
Disentangling dark energy and cosmic tests of gravity from weak lensing systematics
Laszlo, I., Bean, R., Kirk, D., & Bridle, S. (2012) · UCL Discovery (University College London) · Cited by 24
Terasawa, R., Li, X., Takada, M., Nishimichi, T., Tanaka, S., Sugiyama, S., Kurita, T., Zhang, T., Shirasaki, M., Takahashi, R., et al. (2025) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.111.063509 · Cited by 23
“The lensing distortion is small and can only be measured statistically using more than millions of galaxies over a sufficiently wide area of the sky and with various systematic errors under control [16, 17].”
Self-citationde Putter, R., Doré, O., & Das, S. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/780/2/185 · Cited by 23
Laszlo, I., Bean, R., Kirk, D., & Bridle, S. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.20994.x · Cited by 25
THE SYNERGY BETWEEN THE DARK ENERGY SURVEY AND THE SOUTH POLE TELESCOPE
Vallinotto, A. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/778/2/108 · Cited by 22
“…of the multiplicative bias, a systematic introduced in the shear measurement by the algorithms correcting for atmospheric seeing and for the instrumental distortions of the telescope’s point spread function (Heymans et al. 2006; Huterer et al. 2006; Amara & Refregier 2008).”
BackgroundMethodGalaxy–galaxy weak gravitational lensing in f(R) gravity
Li, B., & Shirasaki, M. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx3006 · Cited by 22
“The multiplicative bias is one of the most important systematics in cosmic shear analysis and can make the amplitude of lensing power spectrum uncertain (e.g. Huterer et al. 2006).”
BackgroundTowards a full wCDM map-based analysis for weak lensing surveys
Zürcher, D., Fluri, J., Ajani, V., Fischbacher, S., Refregier, A. R., & Kacprzak, T. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2212 · Cited by 24
“Since inaccuracies in these distributions can lead to biases in the inferred cosmological constraints it is vital to take the uncertainty of the redshift distributions into account (see e.g. Huterer et al. 2006; Choi et al. 2016; Hildebrandt et al. 2020b).”
BackgroundWeak lensing tomography with orthogonal polynomials
Schäfer, B. M., & Heisenberg, L. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21137.x · Cited by 22
“…chosen initial cosmology on the construction of polynomials and that systematics control plays a very important role in parameter estimation from weak lensing (among others, see King & Schneider 2002; Huterer et al. 2006; Bridle & King 2007; Semboloni et al. 2011), which we are not touching here.”
BackgroundZhang, J. (2011) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2011/11/041 · Cited by 22
PSF Anisotropy and Systematic Errors in Weak Lensing SurveysPreprint
Jain, B., Jarvis, M., & Bernstein, G. (2005) · Cited by 22
Self-citationThiele, L., Marques, G. A., Liu, J., & Shirasaki, M. (2023) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.108.123526 · Cited by 21
Sugiyama, S., Takada, M., Miyatake, H., Nishimichi, T., Shirasaki, M., Kobayashi, Y., Mandelbaum, R., More, S., Takahashi, R., Osato, K., et al. (2022) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.105.123537 · Cited by 21
Self-citationAnalytical weak-lensing shear responses of galaxy properties and galaxy detection
Li, X., & Mandelbaum, R. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad890 · Cited by 21
Controlling intrinsic-shear alignment in three-point weak lensing statistics
Shi, X., Joachimi, B., & Schneider, P. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201014191 · Cited by 21
“But the ultimate performance of these future surveys still largely depends on the how well the systematic errors can be controlled (e.g. Huterer et al. 2006).”
BackgroundMethodPhotometric redshifts with surface brightness priors
Stabenau, H. F., Connolly, A. J., & Jain, B. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13317.x · Cited by 21
“In some applications, such as WL tomography (Huterer et al. 2006; Ma et al. 2005), it is important for the measured redshifts to be as unbiased as possible, while others, such as Baryon Oscillations, are more sensitive to the scatter in the measurement.”
MethodInfluentialSelf-citationSources of contamination to weak lensing tomography: redshift-dependent shear measurement bias
Semboloni, E., Tereno, I., Waerbeke, L. V., & Heymans, C. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.14926.x · Cited by 21
“This is in agreement with Huterer et al. (2006) where itwas found that an additive bias larger than∼ 10−4 would degrade the cosmological constraints of future weak lensing probes.”
BackgroundResultZhang, T., Rau, M. M., Mandelbaum, R., Li, X., & Moews, B. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3090 · Cited by 20
Gong, Z., Halder, A., Barreira, A., Seitz, S., & Friedrich, O. (2023) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2023/07/040 · Cited by 20
Yao, J., Shan, H., Li, R., Xu, Y., Fan, D., Liu, D., Zhang, P., Yu, Y., Wei, C., Hu, B., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3563 · Cited by 23
SUPERNOVA ACCELERATION PROBE: INVESTIGATING PHOTOMETRIC REDSHIFT OPTIMIZATION
Dahlén, T., Mobasher, B., Jouvel, S., Kneib, J., Ilbert, O., Arnouts, S., Bernstein, G. M., & Rhodes, J. D. (2008) · The Astronomical Journal · doi:10.1088/0004-6256/136/3/1361 · Cited by 20
“(Ma et al., 2006; Huterer et al. 2006).”
Self-citationCharacterizing unknown systematics in large scale structure surveys
Agarwal, N., Ho, S., Myers, A. D., Seo, H., Ross, A. J., Bahcall, N. A., Brinkmann, J. V., Eisenstein, D. J., Muna, D., Palanque‐Delabrouille, N., et al. (2014) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2014/04/007 · Cited by 20
Cosmic shear statistics in cosmologies with non-Gaussian initial conditions
Fedeli, C., & Moscardini, L. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16500.x · Cited by 23
“…above, the covariance matrix for weak lensing tomography hasnz(nz + 1)nl/2 independent elements, wherenl = l2−l1 = 2950, and it can be written as (Huterer et al. 2006; Ma et al. 2006; Sun et al. 2009) Γ ( Ci jl ,C km l′ ) = δll ′ (2l + 1)∆l fsky [( Cikl + δik γ2 n̄i ) ( C jml + δ jm…”
Modelling baryonic effects on galaxy cluster mass profiles
Shirasaki, M., Lau, E. T., & Nagai, D. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty763 · Cited by 20
“The bias δpα for the parameter pα can be expressed as (e.g., Huterer et al. 2006) δpα = ∑ β F−1αβ ∑ i,j C−1ij ∆〈γ+〉(θi) ∂〈γ+〉(θj) ∂pβ , (24) where i and j are the indices for binned lensing profiles, and ∆〈γ+〉 describes the difference between the assumed and true models.”
Photometric Redshifts and Signal‐to‐Noise Ratios
Margoniner, V. E., & Wittman, D. (2008) · The Astrophysical Journal · doi:10.1086/528365 · Cited by 20
“For example, Ma et al. 2006 and Huterer et al. 2006 have examined the required photometric redshift accuracy for surveys which plan to use weak lensing (cosmic shear) to constrain dark energy.”
BackgroundDetectability of large-scale power suppression in the galaxy distribution
Gibelyou, C., Dragan Huterer, A., & Fang, W. (2010) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.82.123009 · Cited by 19
The Effect of Detector Nonlinearity onWFIRSTPSF Profiles for Weak Gravitational Lensing Measurements
Plazas, A. A., Shapiro, C., Kannawadi, A., Mandelbaum, R., Rhodes, J., & Smith, R. (2016) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/128/968/104001 · Cited by 19
“…in Stage IV surveys (in the language of Albrecht et al. 2006), the ellipticity and relative size of the PSF must be known to an accuracy of O(10−3) (Huterer et al. 2006; Amara & Réfrégier 2008; Paulin-Henriksson et al. 2008, 2009; Cropper et al. 2013; Massey et al. 2013) or better (4.7×10−4 for…”
BackgroundInfluentialBayesian photometric redshifts of blended sources
Jones, D. M., & Heavens, A. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty3279 · Cited by 19
“…would require the mean of each redshift bin to be known to a precision of 0.003, though this requirement can be reduced by self-calibration (e.g. Huterer et al. 2006; Sun, Zhan & Tao 2015; Samuroff et al. 2017) and combining weak lensing data with other cosmological probes such as baryonic…”
BackgroundInfluentialA composite likelihood approach for inference under photometric redshift uncertainty
Rau, M. M., Morrison, C., Schmidt, S. J., Wilson, S., Mandelbaum, R., Mao, Y.-Y., Alonso, D., Hartley, W. G., Kirkby, D. P., Kuusela, M., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3290 · Cited by 18
Magnification as a tool in weak lensing
Vallinotto, A., Dodelson, S., & Zhang, P. (2011) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.84.103004 · Cited by 19
Jain, B., Connolly, A. J., & Takada, M. (2007) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2007/03/013 · Cited by 19
Self-citationEFFECT OF MASKED REGIONS ON WEAK-LENSING STATISTICS
Shirasaki, M., Yoshida, N., & Hamana, T. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/774/2/111 · Cited by 14
“Some of these effects on cosmic shear power spectrum analysis have been already studied (e.g. Huterer et al. 2006; Hikage et al. 2011).”
BackgroundHamana, T., Miyazaki, S., Okura, Y., Okamura, T., & Futamase, T. (2013) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/65.5.104 · Cited by 18
“It should be, however, noted that the full potential of cosmic shear statistics to place a constraint on the cosmological parameters is archived only if systematic errors are reduced down to a required level (Huterer et al. 2006; Cropper et al. 2013; Massey et al. 2013).”
BackgroundCosmic shear requirements on the wavelength dependence of telescope point spread functions
Cypriano, E. S., Amara, A., Voigt, L. M., Bridle, S., Abdalla, F. B., Refregier, A. R., Seiffert, M., & Rhodes, J. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16461.x · Cited by 18
“…presence of a redshift dependent multiplicative bias, the measured lensing power spectrum can be given in terms of the true lensing power spectrum by Ĉκij(ℓ) = C κ ij(ℓ)(1 + m i + mj) (5) where mi is the multiplicative bias for redshift bin i, averaged over all galaxies (Huterer et al. 2006, Eq.”
BackgroundOptimizing cosmic shear surveys to measure modifications to gravity on cosmic scales
Kirk, D., Laszlo, I., Bridle, S., & Bean, R. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sts571 · Cited by 18
“At large values of the prior width we reach a “self-calibration” regime in which the information in the survey is sufficient to constrain the unknown parameters (Huterer et al. 2006).”
BackgroundInfluentialMeasuring the Reduced ShearPreprint
Zhang, J. (2016) · Cited by 18
Constraining extended cosmologies with GW×LSS cross-correlations
Bosi, M., Bellomo, N., & Raccanelli, A. (2023) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2023/11/086 · Cited by 17
“[ 67–69], to treat the error due to poor determination of the GW redshift.”
Exploring Large-scale Structure with Billions of Galaxies
Zhan, H., Knox, L., Tyson, A., & Margoniner, V (2005) · CERN Document Server (European Organization for Nuclear Research) · Cited by 17
Schaefer, B. M., Douspis, M., & Aghanim, N. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.14991.x · Cited by 14
“The question of parameter estimation bias in the presence of systematics was addressed in different contexts: reionisation (Zahn et al. 2005), weak cosmic shear (Huterer et al. 2006; Amara & Refregier 2007) and Sunyaev-Zeldovich contaminations to the CMB spectrum (Taburet et al. 2009).”
BackgroundFinner, K., Lee, B., Chary, R., Jee, M. J., Hirata, C. M., Congedo, G., Taylor, P. L., & HyeongHan, K. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acfafd · Cited by 16
“The contribution of the biases to the measurement of the shear can be separated into a multiplicative bias (m) and an additive bias (c) as follows: gm − gt = mgt + c, (4) where gm is the measured shear and gt is the true shear (Huterer et al. 2006).”
BackgroundInstrumental systematics and weak gravitational lensing
Mandelbaum, R. (2015) · Journal of Instrumentation · doi:10.1088/1748-0221/10/05/c05017 · Cited by 16
“A common description for systematic errors in shear estimates is a linear model [32],”
BackgroundSamuroff, S., Troxel, M. A., Bridle, S., Zuntz, J., MacCrann, N., Krause, E., Eifler, T. F., & Kirk, D. (2016) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slw201 · Cited by 16
“Huterer et al. (2006) show that cosmic shear alone affords a limited capacity for self-calibration.”
BackgroundWeak lensing cosmology beyond ΛCDM
Das, S., de Putter, R., Linder, E. V., & Nakajima, R. (2012) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2012/11/011 · Cited by 16
“[41] finds their results are insensitive to this power law index.”
InfluentialControlling intrinsic-shear alignment in three-point weak lensing statistics
Shi, X., Joachimi, B., & Schneider, P. (2010) · Kölner Universitäts PublikationsServer (Universität zu Köln) · Cited by 16
Spurious Shear from the Atmosphere in Ground-Based Weak Lensing ObservationsPreprint
Wittman, D. (2005) · Cited by 16
Zhang, T., Almoubayyed, H., Mandelbaum, R., Meyers, J. M., Jarvis, M., Kannawadi, A., Schmitz, M. A., & Guinot, A. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3350 · Cited by 15
Jones, E., & Singal, J. (2020) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/ab54ed · Cited by 15
“…with well constrained and understood error properties are critical for the current and coming era of large multi-band extragalactic surveys (e.g. Huterer et al. 2006; Hearin et al. 2010; Bernstein & Huterer 2010), such as the Large Synoptic Survey Telescope (LSST)1, Euclid2, Wide Field Infrared…”
BackgroundInfluentialOn mitigation of the uncertainty in non-linear matter clustering for cosmic shear tomography
Kitching, T., & Taylor, A. N. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18772.x · Cited by 15
“…the uncertainty in the non-linear power spectrum and marginalize over those parameters (Zhang et al., 2009; Rudd et al., 2008; Zenter et al., 2008; Huterer et al., 2006; Jing et al., 2000) or attempt to modify the data to minimise the effect (Huterer & White, 2005), however all these assume…”
BackgroundMerkel, P. M., & Schäfer, B. M. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1044 · Cited by 15
“The Fisher matrix approach may be also used to estimate the bias due to systematic effects that are present in the data but not accounted for in the model used in the analysis from which the bestfitting parameter values are derived (e.g. Huterer et al. 2006; Amara & Réfrégier 2008).”
MethodGreisel, N., Seitz, S., Drory, N., Bender, R., Saglia, R. P., & Snigula, J. M. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1005 · Cited by 15
“However, statistical errors can be accounted for if they are well known (e.g., Huterer et al. 2006).”
BackgroundGiannini, G., Alarcon, A., Gatti, M., Porredon, A., Crocce, M., Bernstein, G. M., Cawthon, R., Sánchez, C., Doux, C., Elvin-Poole, J., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2945 · Cited by 14
Self-citationInvestigating clustering dark energy with 3D weak cosmic shear
Ayaita, Y., Schäfer, B. M., & Weber, M. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.20822.x · Cited by 14
“Further systematic effects have been studied (March et al. 2011) but, in general, do not seem to have a strong impact on parameter estimation (Huterer et al. 2006; Kitching, Taylor & Heavens 2008; Takada & Jain 2009).”
BackgroundTakeuchi, Y., Ichiki, K., & Matsubara, T. (2012) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.85.043518 · Cited by 13
Zhang, L., Yu, Y., & Zhang, P. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa8c72 · Cited by 14
“Following Huterer et al. (2006) and Zhan & Knox (2006), the fiducial galaxy redshift distribution ( )n zP is chosen to have the form = -( ) ( ) ( )n z x x dxexp 2, 13P 2 where ºx z zP 0 with z0=0.45.”
BackgroundMethodInfluentialYamamoto, M., Troxel, M. A., Jarvis, M., Mandelbaum, R., Hirata, C. M., Long, H., Choi, A., & Zhang, T. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2644 · Cited by 14
Probing Dark Energy with the Kunlun Dark Universe Survey Telescope
Zhao, G.-B., Zhan, H., Wang, L., Fan, Z., & Zhang, X. (2011) · Publications of the Astronomical Society of the Pacific · doi:10.1086/660801 · Cited by 14
“At the levels of systematics future surveys aim to achieve, the most important aspect of the (shear) additive error is its amplitude (Huterer et al. 2006), so we simply fix ρX = 1 and ηX = 0.”
BackgroundInfluentialDiagnosing Space Telescope Misalignment and Jitter Using Stellar Images
Ma, Z., Bernstein, G. M., Weinstein, A. J., & Sholl, M. (2008) · Publications of the Astronomical Society of the Pacific · doi:10.1086/595724 · Cited by 14
Self-citationCosmology from cross-correlation of ACT-DR4 CMB lensing and DES-Y3 cosmic shear
Shaikh, S., Harrison, I., van Engelen, A., Marques, G. A., Abbott, T. M. C., Aguena, M., Alves, O., Amon, A., An, R., Bacon, D., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3987 · Cited by 13
Self-citationEuclid: Improving the efficiency of weak lensing shear bias calibration
Jansen, H., Tewes, M., Schrabback, T., Aghanim, N., Amara, A., Andreon, S., Auricchio, N., Baldi, M., Branchini, E., Brescia, M., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347833 · Cited by 13
Simulation-based inference of deep fields: galaxy population model and redshift distributions
Moser, B., Kacprzak, T., Fischbacher, S., Refregier, A. R., Grimm, D., & Tortorelli, L. (2024) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2024/05/049 · Cited by 13
“We create masks of the areas with no data and surrounding bright stars using the bit flags 8 and 9 from the second layer of the fits files.”
Congedo, G., Miller, L., Taylor, A. N., Cross, N. J. G., Duncan, C. A. J., Kitching, T., Martinet, N., Matthew, S. Z., Schrabback, T., Tewes, M., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202450617 · Cited by 13
Degeneracies in parametrized modified gravity models
Hojjati, A. (2013) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2013/01/009 · Cited by 13
“These errors are modeled in [27, 28] and we use their parametrization for our Fisher analysis (see [38] for details).”
Impact of spurious shear on cosmological parameter estimates from weak lensing observables
Petri, A., May, M., Haiman, Z., & Kratochvil, J. M. (2014) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.90.123015 · Cited by 13
Photometric Redshift Biases from Galaxy Evolution
MacDonald, C. J., & Bernstein, G. (2010) · Publications of the Astronomical Society of the Pacific · doi:10.1086/651702 · Cited by 12
“Yet the cosmological measures that weak-lensing surveys have as goals are extremely sensitive to biases or other miscalibrations of the photo-z scale: biases as small as ≈ 10−3(1+ z) will overwhelm the statistical errors on cosmology in these experiments (Huterer et al. 2006).”
BackgroundSelf-citationEuclid: Calibrating photometric redshifts with spectroscopic cross-correlations
Naidoo, K., Johnston, H., Joachimi, B., van den Busch, J. L., Hildebrandt, H., Ilbert, O., Lahav, O., Aghanim, N., Altieri, B., Amara, A., et al. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244795 · Cited by 12
Resampling Images in Fourier Domain
Bernstein, G. M., & Gruen, D. (2014) · Publications of the Astronomical Society of the Pacific · doi:10.1086/675812 · Cited by 11
Self-citationMerkel, P. M., & Schäfer, B. M. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1664 · Cited by 11
“In order to quantify the systematical error ∆θα which is induced by ignoring the biases in the observed power spectra we perturb the Fisher-approximated likelihood and arrive at ∆θα = F−1αβ ∑ ` 2` + 1 2 C−1` ∂C` ∂θβ C−1` ∆C` (21) (Huterer et al. 2006; Amara & Réfrégier 2008).”
Three-point intrinsic alignments of dark matter haloes in the IllustrisTNG simulation
Pyne, S., Tenneti, A., & Joachimi, B. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2351 · Cited by 11
Metadata
- Authors
- Huterer, D., Takada, M., Bernstein, G., & Jain, B.
- Affiliations
- Tohoku University (JP)
- University of Pennsylvania (US)
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2006-02-11
- Volume
- 366
- Issue
- 1
- Pages
- 101-114
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W2102084015
- Cited by
- 409
- References
- 78
- Citations by year
- 2026: 11 · 2025: 13 · 2024: 14 · 2023: 23 · 2022: 25 · 2021: 17 · 2020: 11 · 2019: 13 · 2018: 21 · 2017: 13 · 2016: 24 · 2015: 26 · 2014: 21 · 2013: 16 · 2012: 34
- FWCI
- 14.56
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Dark Matter and Cosmic Phenomena
- Keywords
- weak gravitational lensing, systematic errors, photometric redshift errors, self-calibration, dark energy equation of state, power spectrum, bispectrum
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