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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 101–200 of 407
Cosmic shear analysis of archival HST/ACS data
Schrabback, T., Erben, T., Simon, P., Miralles, J. M., Schneider, P., Heymans, C., Eifler, T. F., Fosbury, R. A. E., Freudling, W., Hetterscheidt, M., et al. (2007) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20065898 · Cited by 82
“This is of particular concern if the redshift distribution is constrained from external fields (seee.g. van Waerbeke et al. 2006; Huterer et al. 2006).”
BackgroundNOISY WEAK-LENSING CONVERGENCE PEAK STATISTICS NEAR CLUSTERS OF GALAXIES AND BEYOND
Fan, Z.-H., Shan, H., & Liu, J.-Y. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/719/2/1408 · Cited by 53
“Considerable efforts have been paid to understand these effects and their influences on cosmological studies (e.g., Tang & Fan 2005; Heymans et al. 2006; Ma et al. 2006; Huterer et al. 2006; Bridle & King 2007; Fan 2007; Amara & Refregier 2008; Sun et al. 2009).”
BackgroundSystematic effects on dark energy from 3D weak shear
Kitching, T., Taylor, A. N., & Heavens, A. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13419.x · Cited by 79
“The effect of systematic errors on weak lensing tomography has also been extensively studied by for example Ma, Hu & Huterer (2006), Huterer et al. (2006), Ishak (2005), King & Schneider (2002), Bridle & King (2007), Amara & Refregier (2007).”
BackgroundGaBoDS: The Garching-Bonn deep survey
Hetterscheidt, M., Simon, P., Schirmer, M., Hildebrandt, H., Schrabback, T., Erben, T., & Schneider, P. (2007) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20065885 · Cited by 79
“See Huterer et al. (2006) and van Waerbeke et al. (2006) for recent studies of photometric redshift errors and their influence on cosmic shear analyses.”
BackgroundTakada, M., & Bridle, S. (n.d.) · UCL Discovery (University College London) · Cited by 78
Self-citationGAZTAÑAGA, E., Eriksen, M., Crocce, M., Castander, F. J., Fosalba, P., Martí, P., Miquel, R., & Cabré, A. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.20613.x · Cited by 77
“Note that this formalism for degradation is more general (for narrow bins) than the one based on the uncertainties in the centroid position of the photo-z source distribution (eg Huterer et al 2006).”
BackgroundMethodConstraining neutrino mass with the tomographic weak lensing bispectrum
Coulton, W., Liu, J., Madhavacheril, M., Böhm, V., & Spergel, D. (2018) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2019/05/043 · Cited by 63
Mitigating Shear-dependent Object Detection Biases with Metacalibration
Sheldon, E. S., Becker, M. R., MacCrann, N., & Jarvis, M. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abb595 · Cited by 75
General requirements on matter power spectrum predictions for cosmology with weak lensing tomography
Hearin, A. P., Zentner, A. R., & Ma, Z. (2012) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2012/04/034 · Cited by 75
“Another potentially dominant source of error for dark energy parameter estimators arises from the necessity of using approximate redshifts determined from photometric data rather than spectroscopic redshifts [43, 44, 45, 46, 47, 48, 49, 50, 51, 52].”
BackgroundHearin, A. P., Zentner, A. R., Ma, Z., & Dragan Huterer, A. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/720/2/1351 · Cited by 73
“…influence of uncertain photometric redshifts (photo-z hereafter) on the dark energy program has been studied by a number of authors (Ma et al. 2006; Huterer et al. 2006; Lima & Hu 2007; Kitching et al. 2008; Ma & Bernstein 2008; Sun et al. 2009; Zentner & Bhattacharya 2009; Bernstein & Huterer…”
BackgroundCosmology with the Large Synoptic Survey Telescope: an overview
Zhan, H., & Tyson, T. (2018) · Reports on Progress in Physics · doi:10.1088/1361-6633/aab1bd · Cited by 73
“It is recognized that the uncertainties in the mean and the width of the true-redshift distribution of galaxies in each photo-z bin should not exceed a few 10−3(1 + z) for the LSST [174, 260, 266].”
BackgroundAn accurate and practical method for inference of weak gravitational lensing from galaxy images
Bernstein, G. M., Armstrong, R., Krawiec, C., & March, M. C. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw879 · Cited by 72
“10−3.5 in order to keep shear-measurement errors from degrading the accuracy of cosmological inferences (Huterer et al. 2006; Amara & Réfrégier 2008).”
BackgroundInfluentialSelf-citationCosmological forecasts for combined and next-generation peculiar velocity surveys
Howlett, C., Staveley‐Smith, L., & Blake, C. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2466 · Cited by 72
An implementation of Bayesian lensing shear measurement
Sheldon, E. S. (2014) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slu104 · Cited by 71
“This multiplicat ve error is significantly larger than the requirements for current and planned surveys, which are∼0.4% and∼0.2%, respectively (Huterer et al. 2006).”
BackgroundInfluentialStar/galaxy separation at faint magnitudes: application to a simulated Dark Energy Survey
Soumagnac, M. T., Abdalla, F. B., Lahav, O., Kirk, D., Sevilla-Noarbe, I., Bertin, E., Rowe, B., Annis, J. T., Busha, M. T., da Costa, L. N., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1410 · Cited by 70
“We use the same formalism as in Amara & Refregier (2008) (see also Kirk et al. 2012 and Huterer et al. 2006), to derive [pα], [pα] = × ∑ β,l,(i,j ),(m,n) (F−1)αβδC sys ij (l)Cov −1[Cgalij (l), C gal mn(l)] ∂Cgalmn(l) ∂pβ , (11) where F−1 is the inverse Fisher matrix.”
Cosmological forecast for non-Gaussian statistics in large-scale weak lensing surveys
Zürcher, D., Fluri, J., Sgier, R., Kacprzak, T., & Réfrégier, A. (2020) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2021/01/028 · Cited by 54
“[46]).”
Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Everett, S., Yanny, B., Kuropatkin, N., Huff, E., Zhang, Y., Myles, J., Masegian, A., Elvin-Poole, J., Allam, S., Bernstein, G. M., et al. (2022) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ac26c1 · Cited by 69
“…the resulting constraints have become so precise that percent-level spatial variations in the survey’s depth can cause biases that dominate over the statistical errors (see for instance Huterer et al. 2006; Blake et al. 2010; Ross et al. 2012; Leistedt et al. 2016; Weaverdyck & Huterer 2020).”
BackgroundSelf-citationHo, S., Agarwal, N., Myers, A. D., Lyons, R., Disbrow, A., Seo, H.-J., Ross, A., Hirata, C., Padmanabhan, N., O’Connell, R., et al. (2015) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2015/05/040 · Cited by 69
Dragan Huterer, A., Cunha, C. E., & Fang, W. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt653 · Cited by 67
The Cosmological Impact of Intrinsic Alignment Model Choice for Cosmic Shear
Kirk, D., Rassat, A., Høst, O., & Bridle, S. (2011) · reroDoc Digital Library · Cited by 65
KiDS-1000: Cosmic shear with enhanced redshift calibration
van den Busch, J. L., Wright, A. H., Hildebrandt, H., Bilicki, M., Asgari, M., Joudaki, S., Blake, C., Heymans, C., Kannawadi, A., Shan, H., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202142083 · Cited by 65
Osato, K., Shirasaki, M., & Yoshida, N. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/806/2/186 · Cited by 52
“The parameter biases of the BA and FE models from fiducial parameters can be computed in the following manner (see, e.g., Huterer et al. 2006): ( ) ( )pp F N N C N p ¯ ¯ , (31) i j i m i ij j1 , 0 1å åd = éëê - ù ûú ¶ ¶a b ab b - - where F is the Fisher matrix given by Equation (27) and N̄i m…”
MethodZhan, H., Knox, L., & Tyson, J. A. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/690/1/923 · Cited by 67
“We extend the additive and multiplicative shear power spectrum errors in Huterer et al. (2006) to include the galaxy power spectrum errors: (CXYℓ )ij =(1 + δ K Xγf X i + δ K Y γf Y j )P XY ij (ℓ) + δKXY [ δKijX 2 rmsn̄ −1 i + ρ XAXi A Y j ( ℓ ℓX ∗ )ηX ] , where ρX determines how strongly the…”
BackgroundInfluentialSánchez, C., & Bernstein, G. M. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty3222 · Cited by 62
“…some selection criterion s, since errors in the characterization of such distributions can lead to biases in the cosmological parameter estimation (Huterer et al. 2006; Cunha et al. 2012; Hildebrandt et al. 2012; Benjamin et al. 2013; Huterer, Cunha & Fang 2013; Bonnett et al. 2016; Hoyle et al.…”
BackgroundSelf-citationShirasaki, M., & Yoshida, N. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/786/1/43 · Cited by 42
“Some of these effects on cosmic-shear power-spectrum analysis have been already studied (e.g., Huterer et al. 2006; Hikage et al. 2011).”
BackgroundNeutrino masses and beyond- ΛCDM cosmology with LSST and future CMB experiments
Mishra-Sharma, S., Alonso, D., & Dunkley, J. (2018) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.97.123544 · Cited by 62
The PAU Survey: an improved photo-zsample in the COSMOS field
Alarcon, A., GAZTAÑAGA, E., Eriksen, M., Baugh, C. M., Cabayol, L., Casas, R., Carretero, J., Castander, F. J., de Vicente, J., Fernandez, E., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3659 · Cited by 61
“A correct description of such redshift distributions is crucial to avoid introducing a bias in the cosmological inference (Huterer et al. 2006; Cunha et al. 2012; Hildebrandt et al. 2012; Benjamin et al. 2013; Huterer, Cunha & Fang 2013; Bonnett et al. 2016; Hildebrandt et al. 2017; Joudaki et al.…”
BackgroundDesigning an inflation galaxy survey: How to measure σ(fNL)∼1 using scale-dependent galaxy bias
de Putter, R., & Doré, O. (2017) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.95.123513 · Cited by 62
“…a large redshift scatter is indeed acceptable, the (photometric) redshift estimator’s distribution , e.g. its scatter and bias, needs to be calibrated to sub-% level precision [45–48], meaning that photo-z calibration is potentially a major limiting systematic for upcoming cosmic shear surveys.”
BackgroundPhotometric Redshift Error Estimators
Oyaizu, H., Lima, M., Cunha, C. E., Lin, H., & Frieman, J. A. (2008) · The Astrophysical Journal · doi:10.1086/592591 · Cited by 62
“…of recent papers have considered the effects of photo-z errors on cosmological probes including baryon acoustic oscillation (Zhan & Knox 2006), weak lensing tomography (Huterer et al. 2006; Ma et al. 2006), supernovae (Huterer et al. 2004) and galaxy clusters (Huterer et al. 2004; Lima & Hu 2007).”
BackgroundImpact of relativistic effects on cosmological parameter estimation
Lorenz, C. S., Alonso, D., & Ferreira, P. G. (2018) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.97.023537 · Cited by 60
Photometric redshift requirements for self-calibration of cluster dark energy studies
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“In addition, we have ignored possiblesystematic errors inherent in weak lensing measurements such as photometric redshift errors and imperfect shape measurement (Huterer et al. 2006; Nishizawa et al. 2010).”
BackgroundSelf-citationCosmic tomographies: baryon acoustic oscillations and weak lensing
Zhan, H. (2006) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2006/08/008 · Cited by 60
Accurate shear measurement with faint sources
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Schneider, P., & Kilbinger, M. (2006) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20065532 · Cited by 57
“Quite a few of those possible systematics have been identified, including the uncertainties in the overall shear calibration resulting from the correction of image smearing by seeing (e.g., Huterer et al. 2006) and uncertainties in the redshift distribution of source galaxies (e.g., Ma et al. 2006).”
BackgroundMarsh, D. J. E., Macaulay, E., Trebitsch, M., & Ferreira, P. G. (2012) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.85.103514 · Cited by 56
TheXMMCluster Survey: forecasting cosmological and cluster scaling-relation parameter constraints
Sahlén, M., Viana, P. T. P., Liddle, A. R., Romer, A. K., Davidson, M., Hosmer, M., Lloyd-Davies, E. J., Sabirli, K., Collins, C. A., Freeman, P. E., et al. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.14923.x · Cited by 56
“These findings are inagreement with what has already been found by e.g. Huterer et al. (2004, 2006); Lima & Hu (2007).”
BackgroundResultInfluentialA unified analysis of four cosmic shear surveys
Chang, C., Wang, M., Dodelson, S., Eifler, T. F., Heymans, C., Jarvis, M., Jee, M. J., Joudaki, S., Krause, E., Malz, A. I., et al. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2902 · Cited by 56
“We parametrize this uncertainty following the approach used in DLS, CFHTLenS, and DES-SV (also see Huterer et al. 2006).”
MethodRedshift and shear calibration: Impact on cosmic shear studies and survey design
Waerbeke, L. V., White, M. J., Hoekstra, H., & Heymans, C. (2006) · Astroparticle Physics · doi:10.1016/j.astropartphys.2006.05.008 · Cited by 55
Unfolding the matter distribution using three-dimensional weak gravitational lensing
Simon, P., Taylor, A. N., & Hartlap, J. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15246.x · Cited by 54
“The main issue for lensing surveys for extracting cosmological parameters will be the control of systematics at the 1%-level (Huterer et al. 2006).”
BackgroundJoudaki, S., & Kaplinghat, M. (2012) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.86.023526 · Cited by 54
Nonlinear clustering in models with primordial non-Gaussianity: The halo model approach
Smith, R. C., Desjacques, V., & Marian, L. (2011) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.83.043526 · Cited by 54
Bayesian inference from photometric redshift surveys
Jasche, J., & Wandelt, B. D. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21423.x · Cited by 53
“…on the inference of cosmological signals such as the baryon acoustic oscillations, cluster counts or weak lensing has been extensively discussed in the literature (see e.g. Huterer et al. 2004; Bernstein & Jain 2004; Ishak 2005; Huterer et al. 2006; Ma et al. 2006; Zhan & Knox 2006; Zhan 2006).”
BackgroundUSING COSMIC MICROWAVE BACKGROUND LENSING TO CONSTRAIN THE MULTIPLICATIVE BIAS OF COSMIC SHEAR
Vallinotto, A. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/759/1/32 · Cited by 53
Simultaneous modelling of matter power spectrum and bispectrum in the presence of baryons
Aricò, G., Angulo, R. E., Hernández-Monteagudo, C., Contreras, S., & Zennaro, M. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab699 · Cited by 52
QUANTIFYING PHOTOMETRIC REDSHIFT ERRORS IN THE ABSENCE OF SPECTROSCOPIC REDSHIFTS
Quadri, R. F., & Williams, R. J. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/725/1/794 · Cited by 51
“…designed to constrain the cosmological parameters require especially tightlyconstrained photometric redshifts, and significant work has gone in to establishing the photometric redshift accuracy and calibration requirements (e.g. Albrecht et al. 2006; Huterer et al. 2006; Mandelbaum et al. 2008).”
BackgroundSystematic effects on dark energy from 3D weak shearPreprint
Kitching, T., Taylor, A. N., & Heavens, A. F. (2008) · Cited by 51
2dFLenS and KiDS: determining source redshift distributions with cross-correlations
Johnson, A., Blake, C., Amon, A., Erben, T., Glazebrook, K., Harnois-Déraps, J., Heymans, C., Hildebrandt, H., Joudaki, S., Klaes, D., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw3033 · Cited by 50
“Knowledge of the redshift distribution of the source galaxies is a critical component of a weak lensing analysis because it is required to calculate the expected weak lensing signal for a given cosmological model (e.g., Ma et al. 2006; Huterer et al. 2006; Kitching et al. 2008).”
BackgroundInfluentialLaboratory Measurement of the Brighter-fatter Effect in an H2RG Infrared Detector
Plazas, A. A., Shapiro, C., Smith, R. M., Huff, E., & Rhodes, J. D. (2018) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/aab820 · Cited by 50
“In addition, Huterer et al. (2006) show that—for a spaced-based mission—a multiplicative error of ∼0.04 will result in a 60% degradation in the marginalized error of the dark energy equation-of-state parameter w0.”
BackgroundInfluentialZhan, H., & Knox, L. (2006) · The Astrophysical Journal · doi:10.1086/503622 · Cited by 50
“The impact of redshift uncertainties on dark energy constraints has been studied for supernovae (Huterer et al. 2004), cluster number counts (Huterer et al. 2004), and most recently for weak lensing (Bernstein& Jain 2004; Huterer et al. 2006; Ishak& Hirata 2005; Ma et al. 2006).”
BackgroundGaBoDS: The Garching-Bonn Deep Survey: VI. Cosmic shear analysisPreprint
Hetterscheidt, M., Simon, P., Schirmer, M., Hildebrandt, H., Schrabback, T., Erben, T., & Schneider, P. (2006) · arXiv (Cornell University) · doi:10.48550/arxiv.astro-ph/0606571 · Cited by 50
“See Huterer et al. (2006) and van Waerbeke et al. (2006) for recent studies of photometric redshift errors and their influence on cosmic shear analyses.”
BackgroundSchrabback, T., Erben, T., Simon, P., Miralles, J. M., Schneider, P., Heymans, C., Eifler, T. F., Fosbury, R. A. E., Freudling, W., Hetterscheidt, M., et al. (2006) · arXiv (Cornell University) · doi:10.48550/arxiv.astro-ph/0606611 · Cited by 50
“This is of particular concern if the redshift distribution is constrained from external fields (seee.g. van Waerbeke et al. 2006; Huterer et al. 2006).”
BackgroundSchneider, M., Knox, L., Zhan, H., & Connolly, A. J. (2006) · CERN Document Server (European Organization for Nuclear Research) · Cited by 49
Sample variance in photometric redshift calibration: cosmological biases and survey requirements
Cunha, C. E., Dragan Huterer, A., Busha, M. T., & Wechsler, R. H. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.20927.x · Cited by 48
“Past papers on the effects of photometric redshift errors on dark energy constraints (Ma et al. 2006; Huterer et al. 2006;Amara & Refregier 2007; Abdalla et al. 2008; Ma & Bernstein 2008; Kitching et al. 2008; Bordoloi et al. 2010; Hearin et al. 2010) have studied in detail the distribution of…”
BackgroundMethodMining the SDSS Archive. I. Photometric Redshifts in the Nearby Universe
D’Abrusco, R., Staiano, A., Longo, G., Brescia, M., Paolillo, M., Filippis, E. D., & Tagliaferri, R. (2007) · The Astrophysical Journal · doi:10.1086/518020 · Cited by 48
Neutrino Physics from the Cosmic Microwave Background and Large-Scale Structure
Abazajian, K. N., & Kaplinghat, M. (2016) · Annual Review of Nuclear and Particle Science · doi:10.1146/annurev-nucl-102014-021908 · Cited by 48
Cosmic Ballet III: Halo spin evolution in the cosmic web
Veena, P. G., Cautun, M., van de Weygaert, R., Tempel, E., & Frenk, C. S. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab411 · Cited by 48
MODELING THE TRANSFER FUNCTION FOR THE DARK ENERGY SURVEY
Chang, C., Busha, M. T., Wechsler, R. H., Refregier, A. R., Amara, A., Rykoff, E. S., Becker, M. R., Bruderer, C., Gamper, L., Leistedt, B., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/801/2/73 · Cited by 47
“As the statistical uncertainties are reduced by orders of magnitude in these large datasets, various systematic uncertainties in analysing the data become important (Huterer et al. 2006; Amara & Réfrégier 2008).”
BackgroundDark energy survey year 1 results: Constraining baryonic physics in the Universe
Huang, H.-J., Eifler, T. F., Mandelbaum, R., Bernstein, G. M., Chen, A., Choi, A., García-Bellido, J., Dragan Huterer, A., Krause, E., Rozo, E., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab357 · Cited by 47
“The mi are multiplicative factors, one for each tomographic bin, that account for shear calibration bias (Heymans et al. 2006; Huterer et al. 2006).”
BackgroundSelf-citationCosmological systematics beyond nuisance parameters: form-filling functions
Kitching, T., Amara, A., Abdalla, F. B., Joachimi, B., & Refregier, A. R. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15408.x · Cited by 46
“We note that Huterer et al. (2006) have used Chebyshev polynomials in weak lensing systematic analysis, although they marginalise over a systematic parameterised using Chebyshev polynomials and then investigate the biases introduced if the most likely value of the estimated coefficients were…”
BackgroundMethodSample variance in weak lensing: How many simulations are required?
Petri, A., Haiman, Z., & May, M. (2016) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.93.063524 · Cited by 39
Chung, D., Viero, M., Church, S., Wechsler, R., Alvarez, M. A., Bond, J., Breysse, P., Cleary, K., Eriksen, H., Foss, M. K., et al. (2018) · Astrophysical Journal · doi:10.3847/1538-4357/ab0027 · Cited by 37
“For comparison, when binning populations of galaxies in a photometric survey to gauge cosmological parameters, both bias and scatter in redshift must be characterized within 0.003 to limit significant degradation in error, even using bins of z 0.1D ~ (Huterer et al. 2006; Ma et al. 2006).”
MethodInfluentialAlarcon, A., Sánchez, C., Bernstein, G. M., & GAZTAÑAGA, E. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2478 · Cited by 44
“…corresponding galaxy samples, and unaccounted errors in such characterization will directly lead to biases in the cosmological parameter estimation (Huterer et al. 2006; Hildebrandt et al. 2012; Cunha et al. 2012; Benjamin et al. 2013; Huterer et al. 2013; Bonnett et al. 2016; Hoyle et al. 2018;…”
BackgroundSelf-citationMiyatake, H., Sugiyama, S., Takada, M., Nishimichi, T., Shirasaki, M., Kobayashi, Y., Mandelbaum, R., More, S., Oguri, M., Osato, K., et al. (2022) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.106.083520 · Cited by 44
Self-citationThe impact of galaxy colour gradients on cosmic shear measurement
Voigt, L. M., Bridle, S., Amara, A., Cropper, M. S., Kitching, T., Massey, R., Rhodes, J., & Schrabback, T. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.20395.x · Cited by 43
“…al. 2007; Bridle et al. 2009, 2010; Kitching et al. 2010, and references therein), requirements on measurement and calibration of galaxy redshifts (Huterer et al. 2006; Ma, Hu & Huterer 2006; Bridle & King 2007; Abdalla et al. 2008; Jouvel et al. 2009; Bernstein & Huterer 2010; Joachimi & Bridle…”
BackgroundSize of Spectroscopic Calibration Samples for Cosmic Shear Photometric Redshifts
Ma, Z., & Bernstein, G. (2008) · The Astrophysical Journal · doi:10.1086/588214 · Cited by 43
“The effect of photo-z calibration on weak lensing is studied by Ma et al. (2006); Huterer et al. (2006); Jain et al. (2007); Abdalla et al. (2007); and Bridle & King (2007).”
BackgroundSelf-citationCALIBRATED ULTRA FAST IMAGE SIMULATIONS FOR THE DARK ENERGY SURVEY
Bruderer, C., Chang, C., Refregier, A. R., Amara, A., Bergé, J., & Gamper, L. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/817/1/25 · Cited by 43
“Therefore, galaxy shapes need to be measured to a very high accuracy (e.g., Huterer et al. 2006; Amara & Réfrégier 2008, henceforth AR08).”
BackgroundSelf-calibration of photometric redshift scatter in weak-lensing surveys
Zhang, P., Pen, U., & Bernstein, G. M. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16445.x · Cited by 42
“…f to ≈1 per cent levels with potentially larger redshift or size dependence (Massey et al. 2007); but, cosmic shear analysis of future large surveys will require |f | 0.1 per cent if induced systematics are to be subdominant to statistical errors (Huterer et al. 2006; Amara & Réfrégier 2008).”
BackgroundMethodResultInfluentialSelf-citationYoo, J., & Seljak, U. (2012) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.86.083504 · Cited by 29
Photometric redshifts with the quasi Newton algorithm (MLPQNA) Results in the PHAT1 contest
Cavuoti, S., Brescia, M., Longo, G., & Mercurio, A. (2012) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201219755 · Cited by 45
“The possibility to achieve a very low level of residual systematics (Huterer et al., 2006; D’Abrusco et al., 2007), is in fact strongly influenced by many factors: the observing strategy, the accuracyof the photometric calibration, the different point-spread-function in different bands, the adopted…”
DiPompeo, M. A., Hickox, R. C., & Myers, A. D. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2681 · Cited by 41
“…are handled — samples selected, regions discarded/weighted, etc. — can shift results in important ways (e.g. Scranton et al. 2002; Myers et al. 2006; Huterer et al. 2006; Ross et al. 2011; Ho et al. 2012, 2015; Agarwal, Ho & Shandera 2014; Leistedt & Peiris 2014) Quasars, the luminous accreting…”
BackgroundDipole anisotropy of galaxy distribution: Does the CMB rest frame exist in the local universe?
Itoh, Y., Yahata, K., & Takada, M. (2010) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.82.043530 · Cited by 41
Self-citationCONSTRAINING COSMOLOGY WITH HIGH-CONVERGENCE REGIONS IN WEAK LENSING SURVEYS
Wang, S., Haiman, Z., & May, M. (2008) · The Astrophysical Journal · doi:10.1088/0004-637x/691/1/547 · Cited by 31
“As illustrated by Huterer et al. (2006), the prior information of the intrinsic ellipticity noise can help to restore the dark energy constraints.”
BackgroundMethodInfluentialMiao, H., Gong, Y., Chen, X., Huang, Z., Li, X.-D., & Zhan, H. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3583 · Cited by 40
“Here, we just simply assume 𝑁𝜅𝜅 = 10−9 and 𝑁𝑔𝑔 = 10−8 (Zhan 2006; Huterer et al. 2006; Gong et al. 2019), and 𝜎𝜖 = 0.3 in our analysis.”
BackgroundInfluentialRau, M. M., Dalal, R., Zhang, T., Li, X., Nishizawa, A. J., More, S., Mandelbaum, R., Miyatake, H., Strauss, M. A., & Takada, M. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1962 · Cited by 40
Self-citationClustering-based redshift estimation: application to VIPERS/CFHTLS
Scottez, V., Mellier, Y., Granett, B. R., Moutard, T., Kilbinger, M., Scodeggio, M., Garilli, B., Bolzonella, M., de la Torre, S., Guzzo, L., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1500 · Cited by 40
“Many of the cosmological measurements to be performed with these surveys – e.g. tomographic weak lensing, tomographic clustering – will require extremely wellcharacterized redshift distributions (Albrecht et al. 2006; Huterer et al. 2006; Ma, Hu & Huterer 2006; Thomas et al. 2011).”
BackgroundJones, E., & Singal, J. (2017) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201629558 · Cited by 40
“An important challenge for the current and coming era of large multi-band extragalactic surveys is obtaining sufficiently accurate photometric redshift estimates and understanding theerror properties of these estimates (see e.g. Huterer et al. (2006) for a review).”
BackgroundPhotometric redshifts with the quasi Newton algorithm (MLPQNA) Results in the PHAT1 contest
Cavuoti, S., Brescia, M., Longo, G., & Mercurio, A. (2012) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201219755/pdf · Cited by 40
IMPACT OF ATMOSPHERIC CHROMATIC EFFECTS ON WEAK LENSING MEASUREMENTS
Meyers, J. M., & Burchat, P. R. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/807/2/182 · Cited by 39
“Following PB12, we list requirements on m based on Huterer et al. (2006), who compute the fractional increase in the uncertainty on the (constant) dark energy equation of state parameter w as a function of the prior uncertainty in m for both DES and LSST.”
MethodCunha, C. E., Dragan Huterer, A., Lin, H., Busha, M. T., & Wechsler, R. H. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1424 · Cited by 39
“As shownby many authors (e.g. Ma et al. 2006; Huterer et al. 2006; Amara & Refregier 2007; Abdalla et al. 2008; Ma & Bernstein 2008; Kitching et al. 2008; Hearin et al. 2010) the photo-z calibration requires exquisite knowledge of the photo-z error distribution.”
BackgroundThiele, L., Hill, J. C., & Smith, K. M. (2020) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.102.123545 · Cited by 39
SKA weak lensing – III. Added value of multiwavelength synergies for the mitigation of systematics
Camera, S., Harrison, I., Bonaldi, A., & Brown, M. D. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2688 · Cited by 46
“As also discussed by Huterer et al. (2006), a calibration systematic error in the estimate of the shear γ leads to a multiplicative spurious term represented by the term in square brackets in Eq.”
BackgroundNonlinearity and pixel shifting effects in HXRG infrared detectors
Plazas, A. A., Shapiro, C., Smith, R., Rhodes, J., & Huff, E. (2017) · Journal of Instrumentation · doi:10.1088/1748-0221/12/04/c04009 · Cited by 38
Bernal, J. L., Bellomo, N., Raccanelli, A., & Verde, L. (2020) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2020/10/017 · Cited by 38
“Others investigated the bias arising from an incorrect modeling of the target observable for several specific cases, including the impact of inhomogeneous reionization on CMB anisotropies [26], the effect on weak lensing measurements from incorrect modeling of the non linear power spectrum and galaxy redshift distribu…”
BackgroundStanford, S. A., Masters, D. C., Darvish, B., Stern, D. K., Cohen, J. G., Capak, P. L., Hernitschek, N., Davidzon, I., Rhodes, J. D., Sanders, D. B., et al. (2021) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ac0833 · Cited by 38
Abdalla, E., Abellán, G. F., Aboubrahim, A., Agnello, A., Akarsu, Ö., Akrami, Y., Alestas, G., Aloni, D., Amendola, L., Anchordoqui, L. A., et al. (2022) · Journal of High Energy Astrophysics · doi:10.1016/j.jheap.2022.04.002 · Cited by 37
Observational constraints on cosmic neutrinos and dark energy revisited
Wang, X., Meng, X.-L., Zhang, T.-J., Shan, H., Gong, Y., TAO, C., Chen, X., & Huang, Y. F. (2012) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2012/11/018 · Cited by 36
“[124].”
QUANTIFYING PHOTOMETRIC REDSHIFT ERRORS IN THE ABSENCE OF SPECTROSCOPIC REDSHIFTSPreprint
Quadri, R., & Williams, R. J. (2016) · Cited by 36
Cosmic tomographies: baryon acoustic oscillations and weak lensingPreprint
Zhan, H. (2006) · Cited by 42
A highly precise shear bias estimator independent of the measured shape noise
Pujol, A., Kilbinger, M., Sureau, F. C., & Bobin, J. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833740 · Cited by 35
CosmoPower-JAX: high-dimensional Bayesian inference with differentiable cosmological emulators
Piras, D., & Mancini, A. S. (2023) · The Open Journal of Astrophysics · doi:10.21105/astro.2305.06347 · Cited by 34
Biases on the cosmological parameters and thermal Sunyaev-Zel'dovich residuals
Taburet, N., Aghanim, N., Douspis, M., & Langer, M. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.14105.x · Cited by 34
“While the Serra et al. (2008) analysis was based on Monte Carlo Markov Chains (MCMC), Zahn et al. used an approximate analytic computation of the biases (see also Huterer et al. 2006).”
MethodPhoto-z outlier self-calibration in weak lensing surveys
Schaan, E., Ferraro, S., & Seljak, U. (2020) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2020/12/001 · Cited by 33
“Furthermore, we also include photo-z outliers through a mixing or leakage matrix cij [34].”
BackgroundMethodZhan, H., & Knox, L. (2005) · CERN Document Server (European Organization for Nuclear Research) · Cited by 33
Petri, A., May, M., & Haiman, Z. (2016) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.94.063534 · Cited by 32
Self-calibration of weak lensing systematic effects using combined two- and three-point statistics
Pyne, S., & Joachimi, B. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab413 · Cited by 32
“Of the few studies which did consider systematics in three-point statistics, Huterer et al. (2006) investigated generic multiplicative and additive biases in future surveys such as LSST and found that using the bispectrum as well as the power spectrum could increase the scope for self-calibration…”
BackgroundMethodInfluentialCATASTROPHIC PHOTO-zERRORS AND THE DARK ENERGY PARAMETER ESTIMATES WITH COSMIC SHEAR
Sun, L., Fan, Z.-H., TAO, C., Kneib, J., Jouvel, S., & Tilquin, A. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/699/2/958 · Cited by 32
“As an approximation, a simple extension of the Fisher matrix formalism can be used to compute the bias in cosmological parameters with (see Huterer et al. 2006; Amara & Refregier 2008) δpi = F−1ij ∑ ,α,β [ Cκα ( ) − C̄κα ( ) ] Cov−1 × [Cκα ( ), Cκβ ( )] ∂C̄ κ β ( ) ∂pj , (10) where α and β each…”
BackgroundInfluentialShirasaki, M., Nishimichi, T., Li, B., & Higuchi, Y. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw3254 · Cited by 34
“We estimate the bias in parameter estimation as (Huterer et al. 2006) δpα = ∑ β F−1GR,αβ [O(xi; F6)−O(xi; fid)]C −1 ij ∂O(xj) ∂pβ , (44) where pα = (Ωm0, σ8), O(xi; fid) represents the assumed ΛCDM model, while O(xi;F6) is the true cosmological model, corresponding to the F6 model in this case.”
HIERARCHICAL PROBABILISTIC INFERENCE OF COSMIC SHEAR
Schneider, M. D., Hogg, D. W., Marshall, P. J., Dawson, W. A., Meyers, J. M., Bard, D., & Lang, D. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/807/1/87 · Cited by 31
“…include the uncertainties in the survey redshift distribution (e.g., from photometric redshift errors, see Loh & Spillar 1986; Connolly et al. 1995; Huterer et al. 2006) as well as other astrophysical systematics that are redshift-dependent (such as intrinsic alignments of galaxies, see Catelan et…”
BackgroundProbing dark energy dynamics from current and future cosmological observations
Zhao, G., & Zhang, X. (2010) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.81.043518 · Cited by 31
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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