From 0769c82230b8a1d5b5a739098f0f56bc309fa3be Mon Sep 17 00:00:00 2001
From: David Alonso <dam.phys@gmail.com>
Date: Tue, 23 Jul 2024 20:43:18 +0100
Subject: [PATCH] added citation (#202)

---
 doc/4Catalogs.html  | 2 +-
 doc/4Catalogs.ipynb | 2 +-
 pymaster/field.py   | 4 +++-
 3 files changed, 5 insertions(+), 3 deletions(-)

diff --git a/doc/4Catalogs.html b/doc/4Catalogs.html
index 389ac25..f38a67a 100644
--- a/doc/4Catalogs.html
+++ b/doc/4Catalogs.html
@@ -7554,7 +7554,7 @@
 </div>
 <div class="jp-InputArea jp-Cell-inputArea"><div class="jp-InputPrompt jp-InputArea-prompt">
 </div><div class="jp-RenderedHTMLCommon jp-RenderedMarkdown jp-MarkdownOutput" data-mime-type="text/markdown">
-<h1 id="4-Catalog-based-power-spectra-">4 Catalog-based power spectra <a class="anchor" id="S4"></a><a class="anchor-link" href="#4-Catalog-based-power-spectra-">¶</a></h1><p>This tutorial presents the infrastructure built in NaMaster for the calculation of power spectra of fields defined at (or from) the positions of a discrete set of sources. The methodology is described in detail in W24.</p>
+<h1 id="4-Catalog-based-power-spectra-">4 Catalog-based power spectra <a class="anchor" id="S4"></a><a class="anchor-link" href="#4-Catalog-based-power-spectra-">¶</a></h1><p>This tutorial presents the infrastructure built in NaMaster for the calculation of power spectra of fields defined at (or from) the positions of a discrete set of sources. The methodology is described in detail in W24. This builds on the work of <a href="https://arxiv.org/abs/2312.12285">Baleato &amp; White 2024</a>.</p>
 <p>The code below demonstrates the use of this methodology for a realistic galaxy catalog, in the context of spin-0 and spin-2 fields (similar to the case of cosmic shear catalogs), and in the context of galaxy clustering, where the overdensity of sources themselves is the field of interest.</p>
 </div>
 </div>
diff --git a/doc/4Catalogs.ipynb b/doc/4Catalogs.ipynb
index 0c7869d..69dc21f 100644
--- a/doc/4Catalogs.ipynb
+++ b/doc/4Catalogs.ipynb
@@ -35,7 +35,7 @@
    "metadata": {},
    "source": [
     "# 4 Catalog-based power spectra <a class=\"anchor\" id=\"S4\"></a>\n",
-    "This tutorial presents the infrastructure built in NaMaster for the calculation of power spectra of fields defined at (or from) the positions of a discrete set of sources. The methodology is described in detail in W24.\n",
+    "This tutorial presents the infrastructure built in NaMaster for the calculation of power spectra of fields defined at (or from) the positions of a discrete set of sources. The methodology is described in detail in W24. This builds on the work of [Baleato & White 2024](https://arxiv.org/abs/2312.12285).\n",
     "\n",
     "The code below demonstrates the use of this methodology for a realistic galaxy catalog, in the context of spin-0 and spin-2 fields (similar to the case of cosmic shear catalogs), and in the context of galaxy clustering, where the overdensity of sources themselves is the field of interest."
    ]
diff --git a/pymaster/field.py b/pymaster/field.py
index d003960..840efc5 100644
--- a/pymaster/field.py
+++ b/pymaster/field.py
@@ -704,7 +704,9 @@ class NmtFieldCatalog(NmtField):
     describing a field sampled at the discrete positions of
     a given catalog of sources. If you want to estimate clustering power
     spectra directly from catalogs, use :obj:`NmtFieldCatalogClustering`
-    instead.
+    instead. The mathematical background for these fields was laid out
+    in `Baleato & White 2024 <https://arxiv.org/abs/2312.12285>`_ , and
+    expanded in Wolz et al. 2024.
 
     Args:
         positions (`array`): Source positions, provided as a list or array