diff --git a/structure/spk/module.yaml b/structure/spk/module.yaml
index 9fed247b..3a85825f 100644
--- a/structure/spk/module.yaml
+++ b/structure/spk/module.yaml
@@ -4,7 +4,7 @@ version: "v1.8"
 purpose: "A hydrodynamical simulation-based model for the impact of baryon physics on the non-linear matter power spectrum"
 url: "https://github.com/jemme07/pyspk/"
 interface: "spk_interface.py"
-attribution: [Salcido, McCarthy, Kwan, Upadhye, Font]
+attribution: [Jaime Salcido, Ian McCarthy, Juliana Kwan, Amol Upadhye, Andreea Font]
 rules:
     Please cite the papers below if you use this code in your research"
 cite:
@@ -18,7 +18,7 @@ explanation:
     py-SP(k) (Salcido et al. 2023) is a python package aimed at predicting the suppression of the 
     total matter power spectrum due to baryonic physics as a function of the baryon fraction of haloes and redshift.
 
-    py-SP(k) is not restrictive to a particular shape of the baryon fraction - halo mass relation. 
+    py-SP(k) is not restricted to a particular shape of the baryon fraction - halo mass relation. 
     In order to provide flexibility to the user, there are 4 different methods to provide py-SP(k) 
     with the required fb-Mhalo relation. 
 
@@ -31,15 +31,14 @@ explanation:
     https://github.com/jemme07/pyspk/blob/main/examples/pySPk_Examples.ipynb
 
     WARNING - if the combination of parameters and your choice for the functional form of the 
-    baryon fraction - halo mass relation goes outwith the SP(k) fitting limits, pyspk returns Nan values.
+    baryon fraction - halo mass relation goes outside the SP(k) fitting limits, pyspk returns NaN values.
     This can happen easily at high-z and high-k will return an error to cosmosis.  This SP(k) parameter combination will
     then be given a likelihood of zero, thus creating a theoretical prior that you should be aware of.
 
 
-# List of parameters that can go in the params.ini file in the section for this module    
 params:
     SO:
-        meaning: The spherical overdensity where pyspk only accepts 200 or 500. The halo mass then corresponds to the 
+        meaning: The spherical overdensity, which must be 200 or 500. The halo mass then corresponds to the 
                  mass with a radius where the mean density is 200 or 500 times the critical density of the Universe.
         type: int
         default: 500
@@ -48,15 +47,14 @@ params:
         type: bool
         default: False
     fb_table:
-        meaning: Optional for method 4. Name of the file containing the baryon fraction as a function of halo mass and redshift
+        meaning: Optional for method 4. Name of a file containing the baryon fraction as a function of halo mass and redshift
                  Format - Redshift, Halo mass [M_odot], Baryon fraction (normalised by the Universal baryon fraction)
                  The file BAHAMAS_fb_M200.csv provides this data from the BAHAMAS simulations (McCarthy et al. 2017).
-                 If this is not provided one of other three of methods will be used to determine the fb-Mhalo relationship
+                 If this is not provided one of the other three of methods will be used to determine the fb-Mhalo relationship
         type: str
         default: 
 
 
-#Inputs for a given choice of a parameter, from the values.ini or from other modules
 inputs:
     fb_a:
         meaning: method 1 power law constant.  Do not set for method 2 or 3.
@@ -90,6 +88,16 @@ inputs:
         meaning: method 2 or 3 power law exponent to sets the redshift dependence. Do not set for method 1.
         type: float
         default:
+    matter_power_nl:
+        z:
+            meaning: Redshifts of samples. 
+            type: real 1d
+        k_h:
+            meaning: Wavenumbers k of samples in Mpc/h.
+            type: real 1d
+        P_k:
+            meaning: Non-linear power spectrum at samples in (Mpc/h)^-3, before SP(k) baryon correction.
+            type: real 2d
 
 
 outputs: