diff --git a/paper.bib b/paper.bib
index 46da3b1..99850ab 100644
--- a/paper.bib
+++ b/paper.bib
@@ -310,14 +310,18 @@ @article{Lange:2017wki
     year = "2017"
 }
 
-@inproceedings{Herrmann:2006ks,
-    author = "Herrmann, F. and Hinder, Ian and Shoemaker, D. and Laguna, P.",
-    title = "{Unequal Mass Binary Black Hole Plunges and Gravitational Recoil}",
-    booktitle = "{New Frontiers in Numerical Relativity (NFNR 2006)}",
-    eprint = "gr-qc/0601026",
-    archivePrefix = "arXiv",
-    month = "1",
-    year = "2006"
+@article{Herrmann_2007,
+    doi = {10.1088/0264-9381/24/12/S04},
+    url = {https://dx.doi.org/10.1088/0264-9381/24/12/S04},
+    year = {2007},
+    month = {may},
+    publisher = {},
+    volume = {24},
+    number = {12},
+    pages = {S33},
+    author = {Frank Herrmann and Ian Hinder and Deirdre Shoemaker and Pablo Laguna},
+    title = {Unequal mass binary black hole plunges and gravitational recoil},
+    journal = {Classical and Quantum Gravity}
 }
 
 @article{Jani:2016wkt,
diff --git a/paper.md b/paper.md
index 56005ac..60dcfdc 100644
--- a/paper.md
+++ b/paper.md
@@ -54,7 +54,7 @@ Extracting these signals from noise and using them to infer the parameters of co
 While analytic solutions exist for the simplest cases within GR, e.g. single BHs, merging BBHs have no analytic solution.
 Approximate methods can be used when the BHs are far apart or have highly unequal masses, but the coalescence of BHs of comparable mass must be solved computationally.
 Numerical relativity (NR) simulations accomplish this by evolving a BBH space-time on supercomputers, enabling us to study the dymanics of BBH systems as well as predict the GWs they emit.
-The Einstein Toolkit (ETK) is a set of tools created to perform these NR simulations [@Loffler:2011ay], and `MAYA` is a branch of ETK used by the MAYA collaboration [@Herrmann:2006ks; @Jani:2016wkt; @Vaishnav:2007nm; @Healy:2009zm; @Pekowsky:2013ska].
+The Einstein Toolkit (ETK) is a set of tools created to perform these NR simulations [@Loffler:2011ay], and `MAYA` is a branch of ETK used by the MAYA collaboration [@Herrmann_2007; @Jani:2016wkt; @Vaishnav:2007nm; @Healy:2009zm; @Pekowsky:2013ska].
 
 These tools allow us to study the coalescence of compact objects, their evolution, and the gravitational radiation they emit.
 The `Mayawaves` library introduced in this paper is an analysis pipeline used to process and analyze such NR simulations.