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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 301–400 of 407
Nishizawa, A. J., Takada, M., Hamana, T., & Furusawa, H. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/718/2/1252 · Cited by 11
“Instead, a precise knowledge of the mean redshift in each tomographic bin is required not to have any significant biases in best-fit parameters compared to the statistical errors, as studied by Huterer et al. (2006).”
BackgroundInfluentialSelf-citationA weak lensing view on primordial non-Gaussianities
Schäfer, B. M., Grassi, A., Gerstenlauer, M., & Byrnes, C. T. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.20357.x · Cited by 11
THE SOURCE-LENS CLUSTERING EFFECT IN THE CONTEXT OF LENSING TOMOGRAPHY AND ITS SELF-CALIBRATION
Yu, Y., Zhang, P., Lin, W., & Cui, W. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/803/1/46 · Cited by 11
“This puts stringent requirements on the accuracy of observational measurement and theoretical modeling (Huterer et al. 2006).”
BackgroundDesigning future dark energy space missions
Jouvel, S., Kneib, J., Bernstein, G. M., Ilbert, O., Jelinsky, P., Milliard, B., Ealet, A., Schimd, C., Dahlén, T., & Arnouts, S. (2011) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201014734 · Cited by 11
“Ma & Bernstein (2008), Huterer et al. (2006), and Bernstein & Huterer (2010) showed that the photoz scatter does not significantly degrade the estimated DE parameters.”
BackgroundSelf-citationBerlfein, F., Mandelbaum, R., Li, X., Zhang, T., Dodelson, S., & Markovic, K. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf1255 · Cited by 10
The power spectrum of systematics in cosmic shear tomography and the bias on cosmological parameters
Cardone, V. F., Martinelli, M., Calabrese, E., Galli, S., Huang, Z., Maoli, R., MELCHIORRI, A., & Scaramella, R. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt2357 · Cited by 10
“…such an issue has then been carefully addressed in the literature under different assumptions about the systematics considered and about their modelling (Huterer et al. 2006; Taylor, Kitching & Heavens 2007; Kitching, Taylor & Heavens 2008a; Kitching et al. 2009; Bernstein & Huterer 2010).”
BackgroundA differentiable perturbation-based weak lensing shear estimator
Li, X., Mandelbaum, R., Jarvis, M., Li, Y., Park, A., & Zhang, T. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3895 · Cited by 10
Cross-correlating Sunyaev–Zel'dovich and weak lensing maps
Munshi, D., Joudaki, S., Coles, P., Smidt, J., & Kay, S. T. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu794 · Cited by 10
“However, the optimism associated with lensing is predicated on overcoming the vast systematic uncertainties in both measurement and in theory (Cooray & Hu 2002; Hirata & Seljak 2003, 2004; White 2004; Ma, Hu & Huterer 2005; Huterer et al. 2006; McDonald, Trac & Contaldi 2006).”
BackgroundTesting the statistical isotropy of large scale structure with multipole vectors
Zunckel, C., Dragan Huterer, A., & Starkman, G. D. (2011) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.84.043005 · Cited by 10
The bispectrum covariance beyond Gaussianity
Martín, S., Schneider, P., & Simon, P. (2012) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201118020/pdf · Cited by 10
Pujol, A., Sureau, F. C., Bobin, J., Courbin, F., Gentile, M., & Kilbinger, M. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038657 · Cited by 10
“…we can describe the relation between the mean observed ellipticity and shear as: 〈 i,obs〉 = gi,obs = ci + (1 + mi)gi, (5) where i = 1, 2,+,×, and now ci,mi are the additive and multiplicative shear biases (see Huterer et al. 2006 and Heymans et al. 2006 for their Taylor expansion notation).”
BackgroundHoyle, B., & Rau, M. M. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz502 · Cited by 10
“…correlation function in a cosmological context, this systematic may lead to biased cosmological parameters which may highlight unphysical tension between data sets, or preference for some cosmological models over others (see e.g. Huterer et al. 2006; Cunha et al. 2014; Rau et al. 2015, 2017).”
BackgroundEuclid and KiDS-1000: Quantifying the impact of source-lens clustering on cosmic shear analyses
Linke, L., Unruh, S., Wittje, A., Schrabback, T., Grandis, S., Asgari, M., Dvornik, A., Hildebrandt, H., Hoekstra, H., Joachimi, B., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202451494 · Cited by 9
A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Gris, P., Awan, H., Becker, M. R., Lin, H., Gawiser, E., & Jha, S. W. (2024) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ad79f5 · Cited by 9
“Shear signals are to be measured with systematic errors lower than ∼ 10 − 3 to minimize the degradation in cosmological parameter accuracies (Huterer et al. 2006).”
BackgroundCosmic shear E/B-mode estimation with binned correlation function data
Becker, M. R. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt1396 · Cited by 9
“…of Dark Energy or modifications to GR from future surveys (e.g., Hirata & Seljak 2003, 2004; Guzik & Bernstein 2005; Huterer & Takada 2005; Huterer et al. 2006; Mandelbaum et al. 2006a; Ma et al. 2006; Bridle & King 2007; Hirata et al. 2007; Hearin & Zentner 2009; Sun et al. 2009;…”
BackgroundThe bispectrum covariance beyond Gaussianity
Martin, S., Schneider, P., & Simon, P. (2012) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201118020 · Cited by 9
“Nevertheless, this Gaussian approximation has been employed in nearly all studies of parameter forcasts from third-order cosmic shear (e.g., Takada & Jain 2004; Huterer et al. 2006; Shi et al. 2010).”
BackgroundMethodCosmic shear calibration with forward modeling
Bruderer, C., Nicola, A., Amara, A., Refregier, A. R., Herbel, J., & Kacprzak, T. (2018) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2018/08/007 · Cited by 9
Photometric Redshifts and Photometry Errors
Wittman, D., Riechers, P. M., & Margoniner, V. E. (2007) · The Astrophysical Journal · doi:10.1086/525020 · Cited by 9
“Second, to control systematic errors in the downstream science, one must be able to know, in some cases rather stringently, the accuracy and precision of the photometric redshifts in the actual survey (Ma et al. 2006, Huterer et al. 2006).”
BackgroundHow well do third-order aperture mass statistics separate E- and B-modes?
Shi, X., Joachimi, B., & Schneider, P. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201322605 · Cited by 9
“Moreover, adding third-order statistics to the weak lensing a alysis may substantially improve the self-calibration of systematic effects (Huterer et al. 2006).”
BackgroundGiga- z : A 100,000 OBJECT SUPERCONDUCTING SPECTROPHOTOMETER FOR LSST FOLLOW-UP
Marsden, D. W., Mazin, B. A., O’Brien, K., & Hirata, C. (2013) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/208/1/8 · Cited by 9
“Very accurate photo-z’s are required to optimally exploit the expected data sets of Dark Energy surveys such as DES, LSST and EUCLID (e.g., Huterer et al. 2006).”
MethodForecasting super-sample covariance in future weak lensing surveys with SuperSCRAM
Digman, M. C., McEwen, J. E., & Hirata, C. M. (2019) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2019/10/004 · Cited by 9
“However, future weak lensing surveys will also suffer from many sources of observational and astrophysical systematic errors, which will need to be properly understood to avoid systematic biases in the results [27–30].”
BackgroundCosmological Studies from Tomographic Weak Lensing Peak Abundances and Impacts of Photo-z Errors
Yuan, S., Pan, C., Liu, X., Wang, Q., & Fan, Z. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab40a5 · Cited by 9
“From these studies, we can also set requirements for the accuracy of photo-z estimates and the subsequent calibrations (Ma et al. 2006; Huterer et al. 2006; Ma & Bernstein 2008; Amara & Réfrégier 2008; Sun et al. 2009; Bernstein & Huterer 2010; Hearin et al. 2010, 2012; Yao et al. 2017; Cao et al.…”
BackgroundMethodInfluentialCosmic Visions Dark Energy: Small Projects Portfolio
Fermi National Accelerator Lab. (FNAL), B., Dawson, K., High Energy Physics (HEP) USDOE Office of Science (SC), Frieman, J. A., Heitmann, K., Jain, B., Kahn, S., Mandelbaum, R., Perlmutter, S., & Slosar, A. (2018) · doi:10.2172/1437393 · Cited by 9
Self-citationSchäfer, B. M., Douspis, M., & Aghanim, N. (2009) · Cited by 12
Xiong, Q., Gong, Y., Zhou, X., Lin, H., Deng, F., Li, Z., Ibitoye, A., Chen, X., Fan, Z., Guo, Q., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adcb44 · Cited by 8
“…considering intrinsic alignments and systematics, the measured shear power spectrum for the i th and j th tomographic bins can be expressed as ( D. Huterer et al. 2006 ) where m i is the shear calibration bias or multiplicative error and the second term accounts for the contribution from the…”
Zhang, Z., Sheldon, E. S., & Becker, M. R. (2023) · The Open Journal of Astrophysics · doi:10.21105/astro.2206.07683 · Cited by 8
Chromatic CCD effects on weak lensing measurements for LSST
Meyers, J. M., & Burchat, P. R. (2015) · Journal of Instrumentation · doi:10.1088/1748-0221/10/06/c06004 · Cited by 8
“Requirements on how well one needs to know m and c have been derived by several authors for surveys similar to and including LSST [5, 6, 7, 8].”
Methodd'Assignies, W., Manera, M., Aranda, C. P., Ilbert, O., Hildebrandt, H., Reynolds, L., Chaves-Montero, J., Wright, A. H., Tallada-Crespí, P., Eriksen, M., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202555551 · Cited by 7
The impact of photometric redshift errors on lensing statistics in ray-tracing simulations
Abruzzo, M. W., & Haiman, Z. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1016 · Cited by 7
“Because photo-z bias bph = zph − z has the leading order effect on biases in p̂ for Pκκ (Ma et al. 2006; Huterer et al. 2006), we only account for the impact of bias in our assessment of uncalibrated errors; we assume that there is no scatter MNRAS 000, 1–24 (2018) Impact of Photo-z Errors on…”
BackgroundMethodResultInfluentialProbing quintessence potential with future cosmological surveys
Takeuchi, Y., Ichiki, K., Takahashi, T., & Yamaguchi, M. (2014) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2014/03/045 · Cited by 6
“They make crucial systematics for constraints on dark energy and/or other parameters [62, 63].”
BackgroundCosmic shear bias and calibration in dark energy studies
Taylor, A. N., & Kitching, T. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty700 · Cited by 7
“…et al. 2013; Cardone et al. 2013; Kitching et al. 2015) The effect of scale-dependent systematic biases on cosmic shear power was first discussed by Huterer et al. (2006) who studied the impact of scaledependent additive image distortions and a constant multiplicative bias on a range of…”
BackgroundPhotometric Redshift Biases from Galaxy EvolutionPreprint
Macdonald, C. J., & Bernstein, G. M. (2010) · Cited by 7
Self-citationThe removal of shear-ellipticity correlations from the cosmic shear signal
Joachimi, B., & Schneider, P. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200912420 · Cited by 77
“To assess the eff ct of the systematic, we also calculate the bias on every parameter by means of the bias formalism (Kim et al. 2004; Huterer & Takada 2005; Huterer et al. 2006; Taylor et al. 2007; Amara & Refregier 2008; Kitching et al. 2008).”
MethodCragg, C., Duncan, C. A. J., Miller, L., & Alonso, D. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3324 · Cited by 6
Analytical noise bias correction for precise weak lensing shear inference
Li, X., & Mandelbaum, R. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae2764 · Cited by 6
Reconstructing the thermal Sunyaev–Zel'dovich effect in 3D
Pratten, G., & Munshi, D. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu807 · Cited by 6
Nonparametric Methods in Astronomy: Think, Regress, Observe—Pick Any Three
Steinhardt, C. L., & Jermyn, A. S. (2018) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/aaa22a · Cited by 6
“However, some problems, including using redshift distributions to constrain cosmology via weak lensing (Laureijs et al. 2011; Huterer et al. 2006; Masters et al. 2015), instead place their most stringent constraints on the bias.”
BackgroundThawing k-essence dark energy in the PAge space
Huang, Z. (2022) · Communications in Theoretical Physics · doi:10.1088/1572-9494/ac80ed · Cited by 6
“The reader is referred to [ 113, 115 – 119 ] for a more detailed discussion about the calibration of these systematics.”
Assessing theoretical uncertainties for cosmological constraints from weak lensing surveys
Tan, T., Zürcher, D., Fluri, J., Refregier, A. R., Tarsitano, F., & Kacprzak, T. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1142 · Cited by 6
Jouvel, S., Kneib, J., Bernstein, G. M., Ilbert, O., Jelinsky, P., Milliard, B., Ealet, A., Schimd, C., Dahlén, T., & Arnouts, S. (2010) · arXiv (Cornell University) · doi:10.48550/arxiv.1003.4294 · Cited by 6
“Ma & Bernstein (2008), Huterer et al. (2006), and Bernstein & Huterer (2010) showed that the photoz scatter does not significantly degrade the estimated DE parameters.”
BackgroundSelf-citationResampling images in Fourier domainPreprint
Bernstein, G. M., & Gruen, D. (2014) · Cited by 6
Self-citationSu, P., Gong, Y., Xiong, Q., Hu, D., Lin, H., Deng, F., & Chen, X. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae4a1e · Cited by 5
“In weak lensing analyses, it typically manifests as a smoothing of the cross-bin correlations and a slight degradation in cosmological parameter constraints ( D. Huterer et al. 2006; Z. Ma et al. 2006; J. Myles et al. 2021 ) .”
Lin, Q., Ruan, H., Fouchez, D., Chen, S., Li, R., Montero-Camacho, P., Napolitano, N. R., Ting, Y.-S., & Zhang, W. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202349113 · Cited by 5
Johnston, H., Chisari, N. E., Joudaki, S., Reischke, R., Stölzner, B., Loureiro, A., Mahony, C., Unruh, S., Wright, A. H., Asgari, M., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202452466 · Cited by 5
“…remains too expensive to provide an accurate redshift for every observed object, the modelling of lensing statistics only requires accurate knowledge of the redshift distributions of source galaxy samples (Bernardeau et al. 1997; Huterer et al. 2006), rather than redshift point-estimates.”
The quest for an accurate measurement of cosmic shear
Zhang, J. (2016) · National Science Review · doi:10.1093/nsr/nww017 · Cited by 5
Dash, C. B. V., Sarkar, T. G., & Sarkar, A. K. (2023) · Journal of Astrophysics and Astronomy · doi:10.1007/s12036-022-09885-w · Cited by 5
“We have assumed that the source galaxies are distributed as (Huterer et al. 2006): n(z) = n0 ( z z0 )α exp [ − ( z z0 )]β .”
MethodEuclid : Photometric redshift calibration with self-organising maps
Roster, W., Wright, A. H., Hildebrandt, H., Reischke, R., Ilbert, O., d'Assignies, W., Manera, M., Bolzonella, M., Masters, D. C., Paltani, S., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202556848 · Cited by 8
Optimizing the shape of photometric redshift distributions with clustering cross-correlations
Stölzner, B., Joachimi, B., & Korn, A. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3630 · Cited by 4
Hang, Q., Joachimi, B., Charles, E., Crenshaw, J. F., Larsen, P., Malz, A. I., Schmidt, S., Yan, Z., Zhang, T., Leistedt, B., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae2519 · Cited by 4
DIAGNOSING MULTIPLICATIVE ERROR WITH LENSING MAGNIFICATION OF TYPE Ia SUPERNOVAE
Zhang, P. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/806/1/45 · Cited by 4
“1%, the minimum requirement for stage IV weak lensing surveys (Huterer et al. 2006).”
BackgroundResultInfluentialGravitational lensing in cosmology
Futamase, T. (2015) · International Journal of Modern Physics D · doi:10.1142/s0218271815300116 · Cited by 4
The effects of calibration on the bias of shear measurements
Gillis, B. R., & Taylor, A. N. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2637 · Cited by 4
“…is minimized, the effects of measurement bias will begin to dominate the measured values, and this bias can carry through to affect the estimates of cosmological parameters (Huterer et al. 2006; Amara & Réfrégier 2008; Kitching et al. 2008; Massey et al. 2013; Taylor & Kitching 2016).”
BackgroundA framework for measuring weak-lensing magnification using the Fundamental Plane
Freudenburg, J. K. C., Huff, E., & Hirata, C. M. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1505 · Cited by 4
“…Hirata & Seljak 2003; Heymans et al. 2006; Massey et al. 2007; Mandelbaum et al. 2012, 2015; Huff & Mandelbaum 2017; Sheldon & Huff 2017) and photometric redshift estimation (Huterer et al. 2006; Newman 2008; Hildebrandt et al. 2010; Sánchez et al. 2014; Masters et al. 2017; Tanaka et al. 2018).”
BackgroundA demonstration of position angle-only weak lensing shear estimators on the GREAT3 simulations
Whittaker, L., Brown, M. D., & Battye, R. A. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2085 · Cited by 4
“Let m′i and c ′ i respectively denote the multiplicative and additive biases on the components of the zeroth-order shear estimates (Heymans et al. 2006; Huterer et al. 2006; Massey et al. 2007).”
BackgroundProbing Quintessence Potential with Future Cosmological SurveysPreprint
Takeuchi, Y., Ichiki, K., Takahashi, T., & Yamaguchi, M. (2016) · Cited by 4
HOW FUTURE SPACE-BASED WEAK LENSING SURVEYS MIGHT OBTAIN PHOTOMETRIC REDSHIFTS INDEPENDENTLYPreprint
Sorba, R., & Sawicki, M. (2016) · Cited by 4
Forecast of Joint Analysis of Cosmic Shear and Supernovae Magnification from the CSST and LSST
Ye, C., Hu, B., Yao, J., & Zhan, H. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad4d96 · Cited by 3
“The covariance matrix of the power spectra can be estimated by (Hu & Jain 2004; Huterer et al. 2006; Joachimi et al. 2008) where 𝑋 , 𝑌 , 𝑋 ′ and 𝑌 ′ are either the SNIa magnification 𝜇 or the galaxy shear 𝛾 .”
MethodZhang, T., Almoubayyed, H., Mandelbaum, R., Rau, M. M., Šarčević, N., Leonard, C. D., Newman, J. A., Andrews, B. H., & Liang, S. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf1829 · Cited by 3
Taking the weight off: mitigating parameter bias from catastrophic outliers in 3×2pt analysis
Mill, C. M., Leonard, C. D., Rau, M. M., Uhlemann, C., & Joudaki, S. (2025) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2025/12/037 · Cited by 3
“However, as the precision of our data improves, the dominant source of error shifts from statistical uncertainties to systematic errors, i.e., those arising from our modelling [13–17].”
How well do third-order aperture mass statistics separate E- and B-modes?
Shi, X., Joachimi, B., & Schneider, P. (2014) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201322605/pdf · Cited by 3
Mapping variations of redshift distributions with probability integral transforms
Myles, J., Gruen, D., Amon, A., Alarcon, A., DeRose, J., Everett, S., Dodelson, S., Bernstein, G. M., Campos, A., Harrison, I., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3585 · Cited by 3
“See also Huterer et al. 2006; Hildebrandt et al. 2012; Benjamin et al. 2013; Huterer et al. 2013; Samuroff et al. 2017; Hoyle & Gruen et al., 2018; Wright et al. 2020a,b; Joudaki et al. 2020; Tessore & Harrison 2020 Myles & Alarcon et al., 2021; Gatti & Giannini et al., 2022; Sánchez & Prat et al.,…”
BackgroundSelf-citationHow Future Space-Based Weak-Lensing Surveys Might Obtain Photometric Redshifts Independently
Sorba, R., & Sawicki, M. (2011) · Publications of the Astronomical Society of the Pacific · doi:10.1086/660843 · Cited by 3
Testing the origin of the CMB large-angle correlation deficit with a galaxy imaging survey
Hearin, A. P., Gibelyou, C., & Zentner, A. R. (2011) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2011/10/012 · Cited by 3
“As the effect of photo-z uncertainty on the dark energy constraints is much more profound [35, 42, 43, 44, 45, 46, 47, 48], the photo-z calibration effort leading up to future wide-area imaging surveys will very likely achieve the precision required to reach the constraining power illustrated in Figs.”
BackgroundSuperMOS: a new class of low resolution multiobject spectrographs
Mazin, B. A., Marsden, D. W., & O’Brien, K. (2012) · Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE · doi:10.1117/12.926398 · Cited by 3
Analysis of two-point statistics of cosmic shear: III. Covariances of shear measures made easyPreprint
Joachimi, B., Schneider, P., & Eifler, T. F. (2007) · arXiv (Cornell University) · doi:10.48550/arxiv.0708.0387 · Cited by 3
“(53) This result is in agreement with the covariance derived for instance in Takada & Jain (2004), Ma et al. (2006) and Huterer et al. (2006).”
ResultDeepShape: Radio weak-lensing shear measurements using deep learning
Tripathi, P., Wang, S., Prunet, S., & Ferrari, A. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202554072 · Cited by 2
Probing decaying dark matter using the post-reionization HI 21-cm signal
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“The observed angular power spectra are given by (D. Huterer et al. 2006 Here, δ ij is the Kronecker delta, which ensures shot noise and shape noise contributes only to auto-correlations within the same tomographic bin, ¯ n ig denotes the mean galaxy number density in the i -th bin, and σ γ…”
d'Assignies, W., Bernstein, G. M., Yin, B., Giannini, G., Alarcon, A., Manera, M., To, C., Yamamoto, M., Weaverdyck, N., Cawthon, R., et al. (2026) · Physical review. D/Physical review. D. · doi:10.1103/6lfl-h6dg · Cited by 2
Self-citationGravitational lensing in cosmology
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Cosmological constraints from HSC Y1 lensing convergence PDFPreprint
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Accurate shear estimation with fourth-order moments
Park, A., Li, X., & Mandelbaum, R. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf053 · Cited by 1
Assessing the growth of structure over cosmic time with cosmic microwave background lensing
Madhavacheril, M. S. (2025) · Philosophical Transactions of the Royal Society A Mathematical Physical and Engineering Sciences · doi:10.1098/rsta.2024.0025 · Cited by 1
“…function n ( z ) for the source galaxies. including Several sources of additional uncertainty are introduced, shear multiplicative biases (e.g. [52,53] or the more recent exploration in [54]), photometric redshift uncertainties (e.g. [55,56]) and intrinsic alignments (e.g. [57] and more…”
Blot, L., Tanidis, K., Cañas-Herrera, G., Carrilho, P., Bonici, M., Camera, S., Cardone, V. F., Casas, S., Davini, S., Domizio, S. D., et al. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202557700 · Cited by 1
Forecasting constraint on primordial black hole properties with the CSST 3×2 pt analysis
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Cid, D. S., Ferté, A., Blazek, J., Samuroff, S., Amon, A., Andrade-Oliveira, F., Coloma-Nadal, J. M., Muir, J., Porredon, A., Prat, J., et al. (2026) · Physical review. D/Physical review. D. · doi:10.1103/8n76-f6ln · Cited by 1
Self-citationCosmology with Gravitational Lensing
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Weak Lensing Morphological Analysis
Shirasaki, M. (2015) · Springer theses · doi:10.1007/978-981-287-796-3_4 · Cited by 1
Development of the FOBOS focal plane positioner
Adams, D., Lawrence, J. S., McGregor, H., O'Brien, E. G., Lacombe, C. S., Lorente, N. P. F., Goodwin, M., Brown, R. A., Thomakos, M., Zafar, T., et al. (2022) · Ground-based and Airborne Instrumentation for Astronomy IX · doi:10.1117/12.2627289 · Cited by 1
“• Nature of Dark Energy Accurate measurements of cosmological distances are important to constrain cosmological results.(1) FOBOS will carry out follow-up spectroscopic surveys of the all-sky panoramic imaging surveys of the upcoming the Vera C.”
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Dark energy survey year 3 results: Cosmology with peaks using an emulator approach
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Self-citationDark Energy Survey Year 3 Results: Three-point shear correlations and mass aperture moments
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“…parameter degeneracies (Bernardeau et al. 2002, Kayo & Takada 2013, Takada & Jain 2003b) and when combined with 2pt functions can additionally constrain astrophysical and systematic nuisance parameters (Huterer et al. 2006, Pyne & Joachimi 2021, Semboloni et al. 2013, Troxel & Ishak 2012).”
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Self-citationWeak gravitational lensing, dark energy and modified gravity
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MEASURING NEUTRINO MASSES AND DARK ENERGY
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Large Synoptic Survey Telescope Town Hall
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The Lsst Data Processing Software Stack
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Introduction to Observational Cosmology
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Multi-probe analysis on harmonic space: Contributions for the Dark Energy Survey
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Neutrino Mass Constraints from Reconstructing the Large-scale Structure: Systematic Uncertainty
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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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