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WL1-DC1-DP1:T1
Determine what simulated data will be necessary for each of the tasks in \deliverableref WL1-DC1-RQ1 .
WL2-DC1-SW5:T2
Develop systematics models for PSF fitting and interpolation residuals for the optics contribution to the PSF.
WL1-DC1-RQ1:T4
Determine tolerances additive shear biases. Include requirements on incorporating PSF uncertainties, noise models, and sensor effects.
WL2-DC1-SW2:T4
Identify systematics that are already negligible without any correction or marginalization.
WL1-DC1-RQ1:T6
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.
WL2-DC1-SW2:T3
Check consistency of the theoretical systematics model with the null test pipeline.
WL2-DC1-SW5:T5
Identify systematics that are already negligible without any correction or marginalization.
WL2-DC1-SW2:T5
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.
WL1-DC1-SW1:T2
Adapt \TJPForecast from \deliverableref TJP1-DC1-SW1 for WL systematics requirements within the framework of \deliverableref D:CI:DC1-WLF
WL1-DC1-RQ1:T2
Determine tolerances related to PSF predictions at galaxy locations.
WL1-DC1-SW2:T5
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.
LSSPScodeDC1_1:T1
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.
WL1-DC1-DP0:T4
Produce high-resolution images of telescope diffraction features that can be convolved with \GalSim images.
WL1-DC1-DP0:T3
Interface available models for brighter-fatter (\deliverableref SABF2 ) and static sensor effects (\deliverableref SAST2 ) with \GalSim.
WL1-DC1-DP0:T2
Validate needs for and use of single-pupil atmosphere simulation tools to predict finite-exposure PSF features.
WL2-DC1-SW3:T1
Develop systematics model for star/galaxy separation errors.
WL1-DC1-SW2:T4
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.)
LSSPScodeDC1_2:T4
Implement covariance estimate that is internal to the data (suitably defined jacknife/bootstrap) and capable of dealing with many bins.
LSSPScodeDC1_1:T2a
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.
WL1-DC1-RQ1:T3
Determine tolerances of galaxy sample selections for cosmic shear measurements.
WL2-DC1-SW5:T6
For each of these systematics, verify that the systematic is adequately tested by at least one of the null tests.
WL2-DC1-SW5:T3
Develop systematics models for sensor effects on galaxy shape measurements.
WL2-DC1-SW4:T3
Define null tests based on the mask information produced by \deliverableref D:CX-DC1-Mask-SW1 .
WL2-DC1-SW5:T4
Develop systematics models for chromatic aspects of the PSF.
WL2-DC1-SW1:T2
Enhance systematics framework for WL specific modeling and analysis.
WL2-DC1-SW4:T4
Enhance and validate the null test pipeline, including automation.
WL1-DC1-RQ1:T5
Determine tolerances on shear calibration (i.e., multiplicative shear biases).
WL2-DC1-SW1:T3
Deploy the systematics software framework on DESC computing resources under the environment developed in \deliverableref CI5 .
WL2-DC1-SW2:T2
Develop parametric systematics model for baryonic mass and galaxy biasing in WL cross-correlations.
LSSPScodeDC2_2:T2
Extend marginalization technique to deal with correlated systematics.
WL1-DC1-SW2:T1
Define the null tests to be automated based on Stage III dark energy survey inputs.
LSSPScodeDC1_1:T0
Investigate existing codes for power-spectra measurements and study if and to what extent they satisfy current requirements.
WL1-DC1-DP1:T2
Build the DC1 WL simulation pipeline using \GalSim.
WL2-DC1-SW4:T1
Evaluate existing software for two-point null tests.
WL1-DC1-SW1:T3
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).
LSSPScodeDC1_1:T3
Investigate template marginalization in pixel space.
WL2-DC1-SW2:T1
Develop parametric systematics model for intrinsic alignments in shear two-point statistics.
LSSPScodeDC2_2:T1
Introduce ability to deal with non-scalar fields, particularly spin-2 fields for shear and intrinsic alignment cross-correlations.
WL1-DC1-DP2:T3
Simulate the DC1 WL data sets.
WL1-DC1-SW2:T3
Validate the null test pipeline with DC1 data and relevant pre-cursor data sets.
WL1-DC1-DP0:T1
Adapt models for the distribution and field-dependence of LSST optics aberrations for the \GalSim API.
WL2-DC1-SW5:T1
Develop systematics models for PSF fitting and interpolation residuals for the atmosphere contribution to the PSF.
WL1-DC1-SW1:T1
Develop a preliminary likelihood module for WL analysis data vector for \deliverableref CX2-WL1-DC1-SW1 to put in \TJPForecast.
WL1-DC1-SW2:T2
Develop the null test pipeline.
WL2-DC1-SW3:T2
Develop systematics model for biases due to blending.
LSSPScodeDC2_2:T0
Extend the code so that any pair of fields can be cross-correlated, regardless if they come as point samples or pixelized maps.
LSSPScodeDC1_2:T5
Investigate methods for dealing with catastrophic redshift-errors.
WL1-DC1-RQ1:T1
Determine tolerance on the accuracy of WCS maps (both Jacobian for each exposures and registration between exposures).
LSSPScodeDC1_1:T2b
Adapt power spectrum code or existing correlation codes so that other 2-point functions are calculable, in particular correlation functions and compensated filters.
WL2-DC1-SW4:T2
Define null tests that can be performed given the LSST cadence, deep drilling fields, colors, and ancillary data sets.
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