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Systematic errors in future weak-lensing surveys: requirements and prospects for self-calibration
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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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Self-citationKiDS-450: cosmological parameter constraints from tomographic weak gravitational lensing
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“Future surveys require the accuracy of calibrated shapes to be on the order of 0.1% (Huterer et al 2006, Cropper et al 2013, Massey et al 2013).”
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Heymans, C., van Waerbeke, L., Bacon, D., Bergé, J., Bernstein, G., Bertin, E., Bridle, S., Brown, M. L., Clowe, D., Dahle, H., et al. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.10198.x · Cited by 377
“…errors, it can only be directly detected through the cosmic shear analysis of image simulations, although see the discussion on self-calibration in Huterer et al. (2006) and Hirata et al. (2004) and Mandelbaum et al. (2005) for model-dependent estimates of shear calibration errors in the Sloan…”
BackgroundSelf-citationBridle, S., & King, L. (2007) · New Journal of Physics · doi:10.1088/1367-2630/9/12/444 · Cited by 492
“This follows previous work (Huterer et al. 2006; Ma et al. 2006; Jain et al. 2007; Amara and Refregier 2006), which has also discussed the numbers of spectroscopic redshifts needed to obtain these priors.”
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Self-citationGalSim: The modular galaxy image simulation toolkit
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Self-citationWeak Gravitational Lensing and Its Cosmological Applications
Hoekstra, H., & Jain, B. (2008) · Annual Review of Nuclear and Particle Science · doi:10.1146/annurev.nucl.58.110707.171151 · Cited by 441
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Self-citationEffects of Baryons and Dissipation on the Matter Power Spectrum
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Dark energy two decades after: observables, probes, consistency tests
Dragan Huterer, A., & Shafer, D. L. (2017) · Reports on Progress in Physics · doi:10.1088/1361-6633/aa997e · Cited by 328
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“This enhancement is due to several advantages of the CSST WL survey, e.g the large survey area (17500 deg2), excellent image quality (2-d Gaussian PSF shape), and accurate photo-z calibration, which can efficiently suppress both statistical and systematical errors.”
BackgroundMethodInfluentialGalaxy Alignments: An Overview
Joachimi, B., Cacciato, M., Kitching, T., Leonard, A., Mandelbaum, R., Schäfer, B. M., Sifón, C., Hoekstra, H., Kiessling, A., Kirk, D., et al. (2015) · Space Science Reviews · doi:10.1007/s11214-015-0177-4 · Cited by 342
“This was re-derived and applied to the case of measurement of the matter power spectrum in Huterer and Takada (2005), and applied to the case of weak lensing systematics in Huterer et al. (2006) and Taylor et al. (2007); the approach was subsequently re-derived in Amara and Réfrégier (2008).”
MethodTroxel, M. A., & Ishak, M. (2014) · Physics Reports · doi:10.1016/j.physrep.2014.11.001 · Cited by 289
“…Ade et al., 2013b,c; Das et al., 2014) have been suggested as a method for calibrating multiplicative biases in galaxy lensing (Vallinotto, 2012; Das et al., 2013), which are difficult to constrain and degenerate with the growth function (e.g., Huterer et al. (2006); Amara and Réfrégier (2008)).”
BackgroundMethodInfluentialCalibrating Redshift Distributions beyond Spectroscopic Limits with Cross‐Correlations
Newman, J. A. (2008) · The Astrophysical Journal · doi:10.1086/589982 · Cited by 285
“…redshift of a bin must be smaller than 2 − 4 × 10−3 in z for dark energy constraints not to be degraded strongly (Huterer et al. 2004; Ma et al. 2006; Huterer et al. 2006); for LSST, it is estimated that the mean redshift in each bin must be known to ∼ 2 × 10−3(1+ z) (Zhan & Knox 2006; Zhan…”
BackgroundHirata, C. M., Mandelbaum, R., Ishak, M., Seljak, U., Nichol, R. C., Pimbblet, K. A., Ross, N. P., & Wake, D. A. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.12312.x · Cited by 285
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Font-Ribera, A., McDonald, P., Mostek, N. J., Reid, B. A., Seo, H.-J., & Slosar, A. (2014) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2014/05/023 · Cited by 322
Hildebrandt, H., Arnouts, S., Capak, P. L., Moustakas, L. A., Wolf, C., Abdalla, F. B., Assef, R. J., Banerji, M., Benítez, N., Brammer, G. B., et al. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201014885 · Cited by 270
“To fully exploit the power of these huge, future data sets, photo-z’s with a very low level of residual systematics are needed (e.g. Huterer et al. 2006).”
BackgroundPractical Weak-lensing Shear Measurement with Metacalibration
Sheldon, E. S., & Huff, E. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa704b · Cited by 268
“We would like to measure this percent level signal to approximately a part in a thousand in upcoming imaging surveys (Huterer et al. 2006).”
BackgroundSearching for modified growth patterns with tomographic surveys
Zhao, G., Pogosian, L., Silvestri, A., & Zylberberg, J. (2009) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.79.083513 · Cited by 281
Ultrahigh precision cosmology from gravitational waves
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CFHTLenS revisited: assessing concordance with Planck including astrophysical systematics
Joudaki, S., Blake, C., Heymans, C., Choi, A., Harnois-Déraps, J., Hildebrandt, H., Joachimi, B., Johnson, A., Mead, A., Parkinson, D., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2665 · Cited by 258
“On the observational front, there are photometric redshift uncertainties (also denoted as ‘photo-z’; e.g. Huterer et al. 2006; Ma, Hu & Huterer 2006; Bernstein & Huterer 2010; Bonnett et al. 2016) and intrinsic alignments (IA) of galaxies (e.g. Hirata & Seljak 2004; Bridle & King 2007; Joachimi et…”
BackgroundDESI and other Dark Energy experiments in the era of neutrino mass measurements
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Constraints on intrinsic alignment contamination of weak lensing surveys using the MegaZ-LRG sample
Joachimi, B., Mandelbaum, R., Abdalla, F., & Bridle, S. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201015621 · Cited by 217
“With the Fisher matrix, one can calculate the bias on a cosmological parameter via (e.g. Kim et al. 2004; Huterer & Takada 2005; Huterer et al. 2006; Taylor et al. 2007; Amara & Réfrégier 2008; Kitching et al. 2009; Joachimi & Schneider 2009) b(pµ) = ∑ ν ( F−1 ) µν ∑ ℓ,i≤ j,k≤l [ C(i j)II (ℓ) +C (i…”
MethodTroxel, M. A., & Ishak, M. (2016) · Cited by 243
Constraints on intrinsic alignment contamination of weak lensing surveys using the MegaZ-LRG sample
Joachimi, B., Mandelbaum, R., Abdalla, F. B., & Bridle, S. (2011) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201015621/pdf · Cited by 219
Bridle, S., & King, L. J. (n.d.) · UCL Discovery (University College London) · Cited by 213
Putting the precision in precision cosmology: How accurate should your data covariance matrix be?
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Angulo, R. E., & White, S. D. M. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16459.x · Cited by 221
“…amplitude of dark matter haloes (Seljak 2008; Matarrese & Verde 2008; Carbone et al. 2008) and the evolution of gravitational lensing signals (Huterer et al. 2006; Hoekstra et al. 2006; Berge et al. 2009; Debono et al. 2009) have been proposed to explore, for instance, the nature of the…”
BackgroundMasters, D., Capak, P., Stern, D., Ilbert, O., Salvato, M., Schmidt, S., Longo, G., Rhodes, J., Paltani, S., Mobasher, B., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/813/1/53 · Cited by 113
“In particular, cosmological parameters derived from weak lensing are sensitive to small, systematic errors in the photo-z estimates (Ma et al. 2006; Huterer et al. 2006).”
BackgroundMassey, R. J., Hoekstra, H., Kitching, T., Rhodes, J. D., Cropper, M. S., Amiaux, J., Harvey, D., Mellier, Y., Meneghetti, M., Miller, L., et al. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sts371 · Cited by 201
Lima, M., Cunha, C., Oyaizu, H., Frieman, J., Lin, H., & Sheldon, E. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13510.x · Cited by 256
“The power of these surveys to constrain cosmological parameters will be limited in part by the accuracy with which the galaxy redshift distributions can be deter- ⋆ mvlima@uchicago.edu mined (Huterer et al. 2004, 2006; Zhan & Knox 2006; Zhan 2006; Ma et al. 2006; Lima & Hu 2007).”
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Hoyle, B., Gruen, D., Bernstein, G. M., Rau, M. M., de Vicente, J., Hartley, W. G., GAZTAÑAGA, E., DeRose, J., Troxel, M. A., Davis, C. P., et al. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty957 · Cited by 199
Self-citationJoachimi, B., & Bridle, S. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200913657 · Cited by 194
“…are well known from theory, the probability distribution of galaxiesp(i)(χ) has to be measured by using additional spectroscopic redshift information (e.g. Huterer et al. 2006; Ma et al. 2006; Abdalla et al. 2007; Bridle & King 2007; Bernstein & Huterer 2010) with a certain level of uncertainty.”
BackgroundSystematic bias in cosmic shear: extending the Fisher matrix
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“In an earlier work, Huterer et al. (2006) considered the impact of photometric calibration errors and power law shape systematics using the Fisher matrix formalism.”
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“The covariance matrix for the angular power spectrum can be written as follows (Hu & Jain 2004; Cohn 2006; Huterer et al. 2006; Yamamoto et al. 2007): ≡ Cov[C̃ (i, j ) C̃ ′ (m, n)] = Cov (ij )(mn) = δ ′ (2 + 1)fsky [ C̃ (i, m) C̃ (j, n) + C̃ (i, n) C̃ (j, m) ] .”
The impact of non-Gaussian errors on weak lensing surveys
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“To do this we model the systematic errors following the method in Huterer et al. (2006): we introduce parameters to describe the systematic errors and include them as nuisance parameters into the Fisher analysis.”
BackgroundMethodSelf-citationCosmic discordance: are Planck CMB and CFHTLenS weak lensing measurements out of tune?
MacCrann, N., Zuntz, J., Bridle, S., Jain, B., & Becker, M. R. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1154 · Cited by 177
“As a rule of thumb, equation 24 from Huterer et al. (2006) tells us that the lensing power spectrum (at l = 1000 and assuming all source galaxies are at zs = 1) has dependence Pκ ∝ σ2.”
BackgroundSelf-citationGalaxy Alignments: Observations and Impact on Cosmology
Kirk, D., Brown, M. D., Hoekstra, H., Joachimi, B., Kitching, T., Mandelbaum, R., Sifón, C., Cacciato, M., Choi, A., Kiessling, A., et al. (2015) · Space Science Reviews · doi:10.1007/s11214-015-0213-4 · Cited by 177
“…matrix approach can be extended to make an estimate of the bias on cosmological parameters, Δpα , when an incorrect cosmological model is assumed (Huterer et al. 2006; see also Amara and Réfrégier 2008 and Appendix A of Joachimi et al. 2011): Δpα = ∑ β F−1αβ ∑ ∑ i≤j ;m≤n ΔC(ij) ( ) ( Cov […”
CARS: the CFHTLS-Archive-Research Survey
Erben, T., Hildebrandt, H., Lerchster, M., Hudelot, P., Benjamin, J., Waerbeke, L. V., Schrabback, T., Brimioulle, F., Cordes, O., Dietrich, J. P., et al. (2008) · Astronomy and Astrophysics · doi:10.1051/0004-6361:200810426 · Cited by 175
“However, we need to reliably separate galaxies into redshift bins and we require a precise understanding ofour errors concerning redshift misidentifications and inter-bin contamination factors (see e.g. Huterer et al. 2006).”
BackgroundDark Energy Survey Year 3 results: redshift calibration of the weak lensing source galaxies
Myles, J., Alarcon, A., Amon, A., Sánchez, C., Everett, S., DeRose, J., McCullough, J., Gruen, D., Bernstein, G. M., Troxel, M. A., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1515 · Cited by 173
Self-citationA halo model for intrinsic alignments of galaxy ellipticities
Schneider, M. D., & Bridle, S. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15956.x · Cited by 171
Oguri, M., & Takada, M. (2011) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.83.023008 · Cited by 171
Self-citationMandelbaum, R., Blake, C., Bridle, S., Abdalla, F. B., Brough, S., Colless, M., Couch, W. J., Croom, S. M., Davis, T. M., Drinkwater, M. J., et al. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.17485.x · Cited by 164
“…to solving the technical problems in measuring the weak lensing signal, primarily related to unbiased shear estimation (Heymans et al. 2006b; Massey et al. 2007a; Bridle et al. 2009) and to photometric redshifts (Bernstein & Jain 2004; Ishak & Hirata 2005; Huterer et al. 2006; Abdalla et al. 2008).”
BackgroundKiDS-1000 catalogue: Redshift distributions and their calibration
Hildebrandt, H., van den Busch, J. L., Wright, A. H., Blake, C., Joachimi, B., Kuijken, K. H., Tröster, T., Asgari, M., Bilicki, M., de Jong, J. T. A., et al. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202039018 · Cited by 159
“The accuracy of the cosmological conclusions drawn from modern WL surveys depends directly on the accuracy of the photo-z used to model the WL observables (Huterer et al. 2006).”
BackgroundThe effective number density of galaxies for weak lensing measurements in the LSST project
Chang, C., Jarvis, M., Jain, B., Kahn, S. M., Kirkby, D., Connolly, A., Krughoff, S., Peng, E. H., & Peterson, J. R. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt1156 · Cited by 164
“Huterer et al. (2006) and Paulin-Henriksson et al. (2008), on the other hand, use the number ng ≈ 30 arcmin−2 in their analyses, where ng is the raw number of galaxies instead of the weighted neff .”
BackgroundSelf-citationTHE THIRD GRAVITATIONAL LENSING ACCURACY TESTING (GREAT3) CHALLENGE HANDBOOK
Mandelbaum, R., Rowe, B., Bosch, J., Chang, C.-W. L., Courbin, F., Gill, M., Jarvis, M., Kannawadi, A., Kacprzak, T., Lackner, C., et al. (2013) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/212/1/5 · Cited by 139
“Following a parameterization used in the STEP challenges and elsewhere (Heymans et al. 2006; Huterer et al. 2006; Massey et al. 2007a), we can relate biases in observed shears g obs to an input true shear g true using a linear model in each component: where i = 1 , 2 denotes the component of shear,…”
MethodResults of the GREAT08 Challenge★: an image analysis competition for cosmological lensing
Bridle, S., Balan, S. T., Bethge, M., Gentile, M., Stefan Harmeling, B., Heymans, C., Hirsch, M., Hosseini, R., Jarvis, M., Kirk, D., et al. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16598.x · Cited by 154
“There is now much discussion about obtaining high-quality galaxy distances using spectroscopic redshifts to calibrate approximate methods to solve (i) (Ma, Hu & Huterer 2005; Huterer et al. 2006a; Bernstein & Ma 2008; Kitching, Taylor & Heavens 2008c; Bernstein & Huterer 2010).”
BackgroundMethodSelf-citationOptimal surveys for weak-lensing tomography
Amara, A., & Refregier, A. R. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.12271.x · Cited by 150
“Future lensing surveys have set 0.1% as their target uncertainties on shear measurements (Huterer et al. 2006; van Waerbeke et al. 2006; Réfrégier et al. 2006), γ, which translates into an uncertainty of 0.2% in Cℓ.”
BackgroundInfluentialCunha, C. E., Lima, M., Oyaizu, H., Frieman, J. A., & Lin, H. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.14908.x · Cited by 150
Precision photometric redshift calibration for galaxy–galaxy weak lensing
Mandelbaum, R., Seljak, U., Hirata, C. M., Bardelli, S., Bolzonella, M., Bongiorno, A., Carollo, C. M., Contini, T., Cunha, C. E., Garilli, B., et al. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.12947.x · Cited by 144
“While several theoretical studies have estimated the effects of photoz errors for shear–shear autocorrelations (Huterer et al. 2006; Ma, Hu & Huterer 2006; Abdalla et al. 2007; Bernstein & Ma 2007), we present the first such analysis for galaxy–galaxy lensing, in which we not only offer statistics…”
BackgroundGrowth of cosmic structure: Probing dark energy beyond expansion
Huterer, D., Kirkby, D., Bean, R., Connolly, A., Dawson, K., Dodelson, S., Evrard, A., Jain, B., Jarvis, M., Linder, E., et al. (2015) · Astroparticle Physics · doi:10.1016/j.astropartphys.2014.07.004 · Cited by 143
“1% relative accuracy in order that dark energy constraints not be significantly degraded [131].”
BackgroundSelf-citationPoint spread function calibration requirements for dark energy from cosmic shear
Paulin-Henriksson, S., Amara, A., Voigt, L. M., Refregier, A. R., & Bridle, S. (2008) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20079150 · Cited by 141
“Huterer et al. (2006) have also studied the impact of multiplicative and additive errors.”
BackgroundMeans of confusion: how pixel noise affects shear estimates for weak gravitational lensing
Melchior, P., & Viola, M. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21381.x · Cited by 140
“E-mail: melchior.12@osu.edu 1 http://www.darkenergysurvey.org/ 2 http://kids.strw.leidenuniv.nl/ 3 http://sci.esa.int/euclid 4 http://wfirst.gsfc.nasa.gov/ |m| not larger than some per mille (e.g Huterer et al. 2006; Amara & Refregier 2008).”
BackgroundMasters, D. C., Stern, D. K., Cohen, J. G., Capak, P. L., Rhodes, J. D., Castander, F. J., & Paltani, S. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa6f08 · Cited by 135
“%) redshift biases can easily dominate the overall error budget in the cosmological parameters measured by these surveys (e.g., Huterer et al. 2006).”
BackgroundGalaxy alignments: An overview
Joachimi, B., Cacciato, M., Kitching, T., Leonard, A., Mandelbaum, R., Schuller, B., Sifón, C., Hoekstra, H., Kiessling, A., Kirk, D., et al. (2015) · KiltHub Repository · doi:10.1184/r1/6506831.v1 · Cited by 136
Semboloni, E., Hoekstra, H., & Schaye, J. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt1013 · Cited by 134
“The benefit of combining three- and two-point shear statistics is even larger in the self-calibration regime (Huterer et al. 2006), where one exploits the different sensitivity of the two measurements to the source redshift distribution in order to alleviate the impact of the lack of accurate…”
BackgroundThe Complete Calibration of the Color–Redshift Relation (C3R2) Survey: Analysis and Data Release 2
Masters, D. C., Stern, D. K., Cohen, J. G., Capak, P. L., Stanford, S. A., Hernitschek, N., Galametz, A., Davidzon, I., Rhodes, J. D., Sanders, D. B., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab184d · Cited by 127
“Weak lensing cosmology requires unbiased redshift estimates (Ma et al. 2006; Huterer et al. 2006), at a level which is not possible with classical photo-z estimation techniques such as spectral template fitting.”
BackgroundCOMPREHENSIVE TWO-POINT ANALYSES OF WEAK GRAVITATIONAL LENSING SURVEYS
Bernstein, G. M. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/695/1/652 · Cited by 125
“For example, in the presence of tomographic data, many systematics are readily distinguishable from cosmological signals and can hence be diagnosed and corrected internally to a survey; this approach is called self-calibration (Huterer et al. 2006).”
Self-citationJoachimi, B., & Bridle, S. (2010) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/200913657/pdf · Cited by 123
On using angular cross-correlations to determine source redshift distributions
McQuinn, M., & White, M. J. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt914 · Cited by 122
“…to prevent redshift errors from being the limiting factor for cosmological parameter estimates with the next generation of weak lensing surveys (Huterer et al. 2006; Schneider et al. 2006; Bernstein & Huterer 2010; Zhang et al. 2010; Cunha et al. 2012).1 There are a wide range of surveys to…”
BackgroundHandbook for the GREAT08 Challenge: An image analysis competition for cosmological lensing
Bridle, S., Gill, M. S. S., Heavens, A., Heymans, C., High, F. W., Hoekstra, H., Jarvis, M., Kirk, D., Kitching, T., Kneib, J., et al. (2009) · The Annals of Applied Statistics · doi:10.1214/08-aoas222 · Cited by 122
Self-citationKayo, I., Takada, M., & Jain, B. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sts340 · Cited by 123
“Thus combining the power spectrum and bispectrum measurements can be used to self-calibrate systematic errors and improve cosmological constraints (Huterer et al. 2006).”
BackgroundMethodSelf-citationCatastrophic photometric redshift errors: weak-lensing survey requirements
Bernstein, G. M., & Dragan Huterer, A. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15748.x · Cited by 121
Self-citationTakada, M., & Bridle, S. (2007) · New Journal of Physics · doi:10.1088/1367-2630/9/12/446 · Cited by 117
Self-citationDark Energy Survey year 1 results: Galaxy-galaxy lensing
Prat, J., Sánchez, C., Fang, Y., Gruen, D., Elvin-Poole, J., Kokron, N., Secco, L. F., Jain, B., Miquel, R., MacCrann, N., et al. (2018) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.98.042005 · Cited by 115
Self-citationKocsis, B., Haiman, Z., & Kristen Menou, A. (2008) · The Astrophysical Journal · doi:10.1086/590230 · Cited by 111
“All of the survey instruments listed in Table 1 should be able to observe the field in several bands, and, for example, LSST should be able deliver photometric redshifts of all sources with an accuracy ofδz ∼< 0.05 (see, e.g. Huterer et al. 2006).”
BackgroundInfluentialDefining a weak lensing experiment in space
Cropper, M. S., Hoekstra, H., Kitching, T., Massey, R. J., Amiaux, J., Miller, L., Mellier, Y., Rhodes, J. D., Rowe, B., Pires, S., et al. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt384 · Cited by 112
“The formalism for the critical systematic effects has been developed in a series of papers (Vale et al., 2004, Mandelbaum et al., 2005, Huterer et al., 2006, Stabenau et al., 2007, Amara & Réfrégier, 2007, 2008, Paulin-Henriksson et al., 2008, Kitching, Taylor & Heavens 2008a, Amara, Réfrégier…”
BackgroundEifler, T. F., Krause, E., Dodelson, S., Zentner, A. R., Hearin, A. P., & Gnedin, N. Y. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2000 · Cited by 111
“…with the parameters we aim to infer from the data; however, this same requirement must be met for more commonplace “self-calibration” exercises to be eff ctive (e.g., such as Huterer et al. 2006; Zentner, Rudd & Hu 2008; Bernstein 2009; Semboloni, Hoekstra & Schaye 2013; Zentner et al. 2013).”
MethodBuchs, R., Davis, C. P., Gruen, D., DeRose, J., Alarcon, A., Bernstein, G. M., Sánchez, C., Myles, J., Roodman, A. J., Allen, S. W., et al. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2162 · Cited by 104
“The physical interpretation of the signal is thus sensitive to systematic errors in redshift (Huterer et al. 2006; Ma, Hu & Huterer 2006).”
BackgroundSelf-citationCosmological Tests of General Relativity with Future Tomographic Surveys
Zhao, G., Pogosian, L., Silvestri, A., & Zylberberg, J. (2009) · Physical Review Letters · doi:10.1103/physrevlett.103.241301 · Cited by 105
Cunha, C. E., Lima, M., Oyaizu, H., Frieman, J. A., & Lin, H. (2009) · Cited by 105
Shape measurement biases from underfitting and ellipticity gradients
Bernstein, G. M. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16883.x · Cited by 103
“…errors into cosmological parameter inferences suggests that systematic errors in shear estimation must be held below ≈ 1 part in 1000 of the expected shear to avoid significant degradation of cosmological inferences (Huterer et al. 2006; ⋆ garyb@physics.upenn.edu Amara & Réfrégier 2008).”
BackgroundSelf-citationHannestad, S. (2006) · Annual Review of Nuclear and Particle Science · doi:10.1146/annurev.nucl.56.080805.140548 · Cited by 103
Measuring neutrino masses and dark energy with weak lensing tomography
Hannestad, S., Tu, H., & Wong, Y. Y. Y. (2006) · CERN Document Server (European Organization for Nuclear Research) · Cited by 101
Spectroscopic needs for imaging dark energy experiments
Newman, J. A., Abate, A., Abdalla, F. B., Allam, S., Allen, S. W., Ansari, R., Bailey, S., Barkhouse, W. A., Beers, T. C., Blanton, M. R., et al. (2015) · Astroparticle Physics · doi:10.1016/j.astropartphys.2014.06.007 · Cited by 98
“…of redshift need to be known to better than ∼0.002(1+z) precision in order to not degrade dark energy parameter accuracies from Stage IV surveys by more than 50% (cf. Ma et al. 2006, Huterer et al. 2006, Kitching et al. 2008, Bernstein & Huterer 2010, Hearin et al. 2010, Hearin et al. 2012).”
BackgroundInfluentialThe cosmological impact of intrinsic alignment model choice for cosmic shear
Kirk, D., Rassat, A., Høst, O., & Bridle, S. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21099.x · Cited by 98
“To this end we employ the cosmological bias formalism of Huterer et al. (2006) (see also Amara & Refregier (2006) and appendix A of Joachimi et al. (2011)). δpα = F −1 αβ ∑ l ∆Cij (Cov [Cij(l), Cmn(l)]) −1 ∂Cmn(l) ∂pβ , (20) where δpα is the cosmological bias on each parameter considered, Cij are…”
Abdalla, F. B., Amara, A., Capak, P. L., Cypriano, E. S., Lahav, O., & Rhodes, J. D. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13151.x · Cited by 98
Optimal surveys for weak-lensing tomographyPreprint
Amara, A., & Refregier, A. R. (2007) · Cited by 96
Measuring neutrino masses and dark energy with weak lensing tomography
Hannestad, S., Tu, H., & Wong, Y. Y. Y. (2006) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2006/06/025 · Cited by 98
Sugiyama, S., Miyatake, H., More, S., Li, X., Shirasaki, M., Takada, M., Kobayashi, Y., Takahashi, R., Nishimichi, T., Nishizawa, A. J., et al. (2023) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.108.123521 · Cited by 95
Self-citationSchneider, M., Knox, L., Zhan, H., & Connolly, A. J. (2006) · The Astrophysical Journal · doi:10.1086/507675 · Cited by 93
Means of confusion: how pixel noise affects shear estimates for weak gravitational lensingPreprint
Melchior, P., & Viola, M. G. (2012) · Cited by 93
Bayesian lensing shear measurement
Bernstein, G. M., & Armstrong, R. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt2326 · Cited by 92
“…errors in shear inference is (using a simplified scalar notation) that the measured shear ĝ is related to the true shear via ĝ = (1 +m)g + c. (1) Huterer et al. (2006) calculate that ambitious weak-shear surveys must obtain multiplicative errors |m| < 10−3 to retain their full statistical…”
BackgroundSelf-citationAnalysis of two-point statistics of cosmic shear
Joachimi, B., Schneider, P., & Eifler, T. F. (2007) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20078400 · Cited by 89
“(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).”
ResultMiyatake, H., Sugiyama, S., Takada, M., Nishimichi, T., Li, X., Shirasaki, M., More, S., Kobayashi, Y., Nishizawa, A. J., Rau, M. M., et al. (2023) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.108.123517 · Cited by 88
“To study the impact of such residual photo-z calibrated uncertainty, we introduce a nuisance parameter, denoted as Δ z ph , to model a systematic shift in the mean source redshift by shifting the posterior distribution of source redshifts, given as [6,14,92].”
MethodSelf-citationWeak lensing, dark matter and dark energy
Huterer, D. (2010) · General Relativity and Gravitation · doi:10.1007/s10714-010-1051-z · Cited by 70
Self-calibration of tomographic weak lensing for the physics of baryons to constrain dark energy
Zentner, A. R., Rudd, D. H., & Hu, W. (2008) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.77.043507 · Cited by 86
Schaan, E., Krause, E., Eifler, T. F., Doré, O., Miyatake, H., Rhodes, J. D., & Spergel, D. N. (2017) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.95.123512 · Cited by 85
THE THIRD GRAVITATIONAL LENSING ACCURACY TESTING (GREAT3) CHALLENGE HANDBOOK
Mandelbaum, R., Rowe, B., Bosch, J., Chang, C., Courbin, F., Gill, M. S., Jarvis, M., Kannawadi, A., Kacprzak, T., Lackner, C., et al. (2014) · UCL Discovery (University College London) · Cited by 85
RECONSTRUCTING REDSHIFT DISTRIBUTIONS WITH CROSS-CORRELATIONS: TESTS AND AN OPTIMIZED RECIPE
Matthews, D. J., & Newman, J. A. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/721/1/456 · Cited by 85
“If future dark energy experiments are to reach their goals, it is necessary to develop a method of calibrating photometric redshifts with high precision (Albrecht et al. 2006; Huterer et al. 2006; Ma et al. 2006).”
MethodCosmological tests of general relativity: A principal component analysis
Hojjati, A., Zhao, G., Pogosian, L., Silvestri, A., Crittenden, R., & Koyama, K. (2012) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.85.043508 · Cited by 83
Gatti, M., Giannini, G., Bernstein, G. M., Alarcon, A., Myles, J., Amon, A., Cawthon, R., Troxel, M. A., DeRose, J., Everett, S., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3311 · Cited by 83
Self-citationMeasuring dark energy properties with 3D cosmic shear
Heavens, A., Kitching, T., & Taylor, A. N. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.11006.x · Cited by 83
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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