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Determine what simulated data will be necessary for each of the tasks in \deliverableref WL1-DC1-RQ1 .

Develop systematics models for PSF fitting and interpolation residuals for the optics contribution to the PSF.

Determine tolerances additive shear biases. Include requirements on incorporating PSF uncertainties, noise models, and sensor effects.

Identify systematics that are already negligible without any correction or marginalization.

Collect a set of standard assumptions, based on the first year of LSST data, to be used in setting requirements, such as number density, sky fraction, and redshift/angular bins. Share these with the collaboration.

Check consistency of the theoretical systematics model with the null test pipeline.

Identify systematics that are already negligible without any correction or marginalization.

For each of these systematics, verify that the systematic is adequately tested by at least one of the null tests. i.e. Does a catalog with a significant systematic trigger a failure of at least one null test. If not, this means we either need to add another null test or find some other way to set a prior on the level of the systematic.

Adapt \TJPForecast from \deliverableref TJP1-DC1-SW1 for WL systematics requirements within the framework of \deliverableref D:CI:DC1-WLF

Determine tolerances related to PSF predictions at galaxy locations.

Define the range of values for each null test that would be considered ``null '' . i.e. for a systematics-free catalog with appropriate noise properties, what range of values could be obtained from each null test.

Define a suitable data compression for the power spectrum measurement, including choices of how to bin input catalogs in photo-z, redshift-errors, object-types, and luminosities.

Produce high-resolution images of telescope diffraction features that can be convolved with \GalSim images.

Interface available models for brighter-fatter (\deliverableref SABF2 ) and static sensor effects (\deliverableref SAST2 ) with \GalSim.

Validate needs for and use of single-pupil atmosphere simulation tools to predict finite-exposure PSF features.

Develop systematics model for star/galaxy separation errors.

Confirm that DM will be providing all the necessary metadata that we need for our null tests. e.g. various temperatures, wind speed and direction, etc. (This may be a very quick task, since I think they are already planning to provide all of these things and much more.)

Implement covariance estimate that is internal to the data (suitably defined jacknife/bootstrap) and capable of dealing with many bins.

Implement a basic code capable of measuring power spectra over numerous slices using parametrization defined in \autoref LSSPScodeDC1_1:T1 and approximating data covariance matrix as diagonal.

Determine tolerances of galaxy sample selections for cosmic shear measurements.

For each of these systematics, verify that the systematic is adequately tested by at least one of the null tests.

Develop systematics models for sensor effects on galaxy shape measurements.

Define null tests based on the mask information produced by \deliverableref D:CX-DC1-Mask-SW1 .

Develop systematics models for chromatic aspects of the PSF.

Enhance systematics framework for WL specific modeling and analysis.

Enhance and validate the null test pipeline, including automation.

Determine tolerances on shear calibration (i.e., multiplicative shear biases).

Deploy the systematics software framework on DESC computing resources under the environment developed in \deliverableref CI5 .

Develop parametric systematics model for baryonic mass and galaxy biasing in WL cross-correlations.

Extend marginalization technique to deal with correlated systematics.

Define the null tests to be automated based on Stage III dark energy survey inputs.

Investigate existing codes for power-spectra measurements and study if and to what extent they satisfy current requirements.

Build the DC1 WL simulation pipeline using \GalSim.

Evaluate existing software for two-point null tests.

Develop an approximate framework to propagate image-level systematics to shear two-point function biases via shear calibration errors using the \WLImSim code. This pipeline should accomodate sensor effects, PSF inference errors, and source extraction errors (including deblending), but in a fast and flexible implementation (trading physical fidelity for speed of development and execution).

Investigate template marginalization in pixel space.

Develop parametric systematics model for intrinsic alignments in shear two-point statistics.

Introduce ability to deal with non-scalar fields, particularly spin-2 fields for shear and intrinsic alignment cross-correlations.

Simulate the DC1 WL data sets.

Validate the null test pipeline with DC1 data and relevant pre-cursor data sets.

Adapt models for the distribution and field-dependence of LSST optics aberrations for the \GalSim API.

Develop systematics models for PSF fitting and interpolation residuals for the atmosphere contribution to the PSF.

Develop a preliminary likelihood module for WL analysis data vector for \deliverableref CX2-WL1-DC1-SW1 to put in \TJPForecast.

Develop the null test pipeline.

Develop systematics model for biases due to blending.

Extend the code so that any pair of fields can be cross-correlated, regardless if they come as point samples or pixelized maps.

Investigate methods for dealing with catastrophic redshift-errors.

Determine tolerance on the accuracy of WCS maps (both Jacobian for each exposures and registration between exposures).

Adapt power spectrum code or existing correlation codes so that other 2-point functions are calculable, in particular correlation functions and compensated filters.

Define null tests that can be performed given the LSST cadence, deep drilling fields, colors, and ancillary data sets.