From eff6418246517840fa6e13f8106083165b9bfa5c Mon Sep 17 00:00:00 2001 From: Paul Tiede Date: Mon, 23 Sep 2024 13:46:52 -0400 Subject: [PATCH] Add missing docstring and fix example in cphase --- docs/src/api.md | 1 + examples/intermediate/ClosureImaging/main.jl | 2 +- 2 files changed, 2 insertions(+), 1 deletion(-) diff --git a/docs/src/api.md b/docs/src/api.md index 5aa2dd90..95814721 100644 --- a/docs/src/api.md +++ b/docs/src/api.md @@ -127,6 +127,7 @@ Comrade.loglikelihood Comrade.dataproducts Comrade.skymodel Comrade.instrumentmodel(::Comrade.AbstractVLBIPosterior) +Comrade.instrumentmodel(::Comrade.AbstractVLBIPosterior, ::Any) Comrade.forward_model Comrade.prior_sample Comrade.likelihood diff --git a/examples/intermediate/ClosureImaging/main.jl b/examples/intermediate/ClosureImaging/main.jl index d53edcfa..7e4d90e7 100644 --- a/examples/intermediate/ClosureImaging/main.jl +++ b/examples/intermediate/ClosureImaging/main.jl @@ -117,7 +117,7 @@ skymeta = (;mimg = imgpr./flux(imgpr)); # of the GMRF is a hyperparameter that is fit during imaging. We pass the data to the prior # to estimate what the maximumal resolutoin of the array is and prevent the prior from allowing # correlation lengths that are much small than the telescope beam size. Note that this GMRF prior -# has unit variance. For more information on the GMRF prior see the [corr_image_prior](@ref) doc string. +# has unit variance. For more information on the GMRF prior see the [`corr_image_prior`](@ref) doc string. cprior = corr_image_prior(grid, dlcamp) # Putting everything together the total prior is then our image prior, a prior on the