Redefine LATISS focalPlane plots to decrease nBins

The choice of nBins = 80 gives about 10 bins per amplifier (along the
short axis).  This seems a nice compromise for highlighting any patterns
on the "focal plane" (single detector) for LATISS while not washing any
potentially discernable structure out.

This also omits the KPM metrics defined on scales much larger than the
current observing strategy for AuxTel/LATISS covers.

pipelines/LATISS/DRP.yaml

@@ -3,18 +3,17 @@ instrument: lsst.obs.lsst.Latiss
 imports:
   - location: $DRP_PIPE_DIR/pipelines/_ingredients/DRP-full.yaml
   - location: $ANALYSIS_TOOLS_DIR/pipelines/coaddColumnValidate.yaml
-  - location: $ANALYSIS_TOOLS_DIR/pipelines/matchedVisitQualityCore.yaml
   - location: $ANALYSIS_TOOLS_DIR/pipelines/coaddQualityCore.yaml
     exclude:
       - analyzeObjectTableCore
+  # The following are from analysis_drp
+  # TODO: remove once they have all been ported to analysis_tools (DM-39081)
   - location: $ANALYSIS_DRP_DIR/pipelines/analysis_drp_plots.yaml
     include:
       - plot_ri_gr_psf
       - plot_ri_gr_cmodel
       - plot_wFit_PSF
       - plot_xFit_PSF
-  # The following are from analysis_drp
-  # TODO: remove once they have all been ported to analysis_tools (DM-39081)
   - location: $ANALYSIS_DRP_DIR/pipelines/coaddQAPlots_tier2_3.yaml
     include:
       - plot_ri_gr_contour_psf
@@ -46,8 +45,8 @@ tasks:
       # psf kernel size.
       maxPsfFwhm: 1.9
 
-  # Importing and defining analyzeObjectTableCore here to omit plots that
-  # require z and/or y band data.
+  # Defining analyzeObjectTableCore here to omit plots that require z and/or
+  # y band data.
   analyzeObjectTableCore:
     class: lsst.analysis.tools.tasks.ObjectTableTractAnalysisTask
     config:
@@ -67,6 +66,35 @@ tasks:
         from lsst.analysis.tools.atools import *
         from lsst.analysis.tools.contexts import *
 
+  # Defining analyzematchedVisitCore here to change the nBins config and omit
+  # plots currently not relevant for LATISS imaging.
+  analyzeMatchedVisitCore:
+    class: lsst.analysis.tools.tasks.AssociatedSourcesTractAnalysisTask
+    config:
+      connections.outputName: matchedVisitCore
+      atools.stellarPhotometricRepeatability: StellarPhotometricRepeatability
+      atools.stellarPhotometricResiduals: StellarPhotometricResidualsFocalPlane
+      atools.stellarPhotometricResiduals.produce.plot.nBins: 80
+      atools.stellarAstrometricResidualsRA: StellarAstrometricResidualsRAFocalPlanePlot
+      atools.stellarAstrometricResidualsRA.produce.nBins: 80
+      atools.stellarAstrometricResidualsDec: StellarAstrometricResidualsDecFocalPlanePlot
+      atools.stellarAstrometricResidualsDec.produce.nBins: 80
+      atools.stellarAstrometricResidualStdDevRA: StellarAstrometricResidualStdDevRAFocalPlanePlot
+      atools.stellarAstrometricResidualStdDevRA.produce.nBins: 80
+      atools.stellarAstrometricResidualStdDevDec: StellarAstrometricResidualStdDevDecFocalPlanePlot
+      atools.stellarAstrometricResidualStdDevDec.produce.nBins: 80
+      # The following are the AMX metrics: median relative astrometric measurement
+      # error on N arc minute scales from single visit images shall be less than
+      # this value, where N = 5, 20, 200 arcmin for X = 1, 2, 3, respectivley.
+      # Given the current distribution of visits/field, one X = 1 is included for
+      # now (the others just pollute the repo with empty plots). The others can/should
+      # be added if the observing strategy changes to warrant it.
+      atools.stellarAstrometricRepeatability1: AstrometricRelativeRepeatability
+      atools.stellarAstrometricRepeatability1.xValue: 1
+      atools.stellarAstrometricRepeatability1.process.calculateActions.rms.annulus: 5
+      python: |
+        from lsst.analysis.tools.atools import *
+
 subsets:
   step1:
     subset: