all links added in doc (#219)

doc/1BasicFunctionality.html

@@ -7539,7 +7539,7 @@
 <li><strong>G19</strong>. Garcia-Garcia et al. 2019 (<a href="https://arxiv.org/abs/1906.11765">https://arxiv.org/abs/1906.11765</a>), which introduces the basic approximation used by NaMaster to estimate covariance matrix.</li>
 <li><strong>N20</strong>. Nicola et al. 2020 (<a href="https://arxiv.org/abs/2010.09717">https://arxiv.org/abs/2010.09717</a>), which refined these approximations and described in detail the procedure to estimate cosmic shear power spectra.</li>
 <li><strong>W24</strong>. Wolz et al. 2024 (<a href="https://arxiv.org/abs/2407.21013">https://arxiv.org/abs/2407.21013</a>), which introduced the formalism for catalog-based $C_\ell$s.</li>
-<li><strong>A24</strong>. Alonso 2024 (TBD), which generalised the estimator to anisotropic weights.</li>
+<li><strong>A24</strong>. Alonso 2024 (<a href="https://arxiv.org/abs/2410.07077">https://arxiv.org/abs/2410.07077</a>), which generalised the estimator to anisotropic weights.</li>
 </ul>
 </div>
 </div>

doc/1BasicFunctionality.ipynb

@@ -23,7 +23,7 @@
     "- **G19**. Garcia-Garcia et al. 2019 (https://arxiv.org/abs/1906.11765), which introduces the basic approximation used by NaMaster to estimate covariance matrix.\n",
     "- **N20**. Nicola et al. 2020 (https://arxiv.org/abs/2010.09717), which refined these approximations and described in detail the procedure to estimate cosmic shear power spectra.\n",
     "- **W24**. Wolz et al. 2024 (https://arxiv.org/abs/2407.21013), which introduced the formalism for catalog-based $C_\\ell$s.\n",
-    "- **A24**. Alonso 2024 (TBD), which generalised the estimator to anisotropic weights."
+    "- **A24**. Alonso 2024 (https://arxiv.org/abs/2410.07077), which generalised the estimator to anisotropic weights."
    ]
   },
   {

doc/2Spin.html

@@ -7539,7 +7539,7 @@
 <li><strong>G19</strong>. Garcia-Garcia et al. 2019 (<a href="https://arxiv.org/abs/1906.11765">https://arxiv.org/abs/1906.11765</a>), which introduces the basic approximation used by NaMaster to estimate covariance matrix.</li>
 <li><strong>N20</strong>. Nicola et al. 2020 (<a href="https://arxiv.org/abs/2010.09717">https://arxiv.org/abs/2010.09717</a>), which refined these approximations and described in detail the procedure to estimate cosmic shear power spectra.</li>
 <li><strong>W24</strong>. Wolz et al. 2024 (<a href="https://arxiv.org/abs/2407.21013">https://arxiv.org/abs/2407.21013</a>), which introduced the formalism for catalog-based $C_\ell$s.</li>
-<li><strong>A24</strong>. Alonso 2024 (TBD), which generalised the estimator to anisotropic weights.</li>
+<li><strong>A24</strong>. Alonso 2024 (<a href="https://arxiv.org/abs/2410.07077">https://arxiv.org/abs/2410.07077</a>), which generalised the estimator to anisotropic weights.</li>
 </ul>
 </div>
 </div>

doc/2Spin.ipynb

@@ -23,7 +23,7 @@
     "- **G19**. Garcia-Garcia et al. 2019 (https://arxiv.org/abs/1906.11765), which introduces the basic approximation used by NaMaster to estimate covariance matrix.\n",
     "- **N20**. Nicola et al. 2020 (https://arxiv.org/abs/2010.09717), which refined these approximations and described in detail the procedure to estimate cosmic shear power spectra.\n",
     "- **W24**. Wolz et al. 2024 (https://arxiv.org/abs/2407.21013), which introduced the formalism for catalog-based $C_\\ell$s.\n",
-    "- **A24**. Alonso 2024 (TBD), which generalised the estimator to anisotropic weights."
+    "- **A24**. Alonso 2024 (https://arxiv.org/abs/2410.07077), which generalised the estimator to anisotropic weights."
    ]
   },
   {

doc/3Covariances.html

@@ -7541,7 +7541,7 @@
 <li><strong>G19</strong>. Garcia-Garcia et al. 2019 (<a href="https://arxiv.org/abs/1906.11765">https://arxiv.org/abs/1906.11765</a>), which introduces the basic approximation used by NaMaster to estimate covariance matrix.</li>
 <li><strong>N20</strong>. Nicola et al. 2020 (<a href="https://arxiv.org/abs/2010.09717">https://arxiv.org/abs/2010.09717</a>), which refined these approximations and described in detail the procedure to estimate cosmic shear power spectra.</li>
 <li><strong>W24</strong>. Wolz et al. 2024 (<a href="https://arxiv.org/abs/2407.21013">https://arxiv.org/abs/2407.21013</a>), which introduced the formalism for catalog-based $C_\ell$s.</li>
-<li><strong>A24</strong>. Alonso 2024 (TBD), which generalised the estimator to anisotropic weights.</li>
+<li><strong>A24</strong>. Alonso 2024 (<a href="https://arxiv.org/abs/2410.07077">https://arxiv.org/abs/2410.07077</a>), which generalised the estimator to anisotropic weights.</li>
 </ul>
 </div>
 </div>

doc/3Covariances.ipynb

@@ -25,7 +25,7 @@
     "- **G19**. Garcia-Garcia et al. 2019 (https://arxiv.org/abs/1906.11765), which introduces the basic approximation used by NaMaster to estimate covariance matrix.\n",
     "- **N20**. Nicola et al. 2020 (https://arxiv.org/abs/2010.09717), which refined these approximations and described in detail the procedure to estimate cosmic shear power spectra.\n",
     "- **W24**. Wolz et al. 2024 (https://arxiv.org/abs/2407.21013), which introduced the formalism for catalog-based $C_\\ell$s.\n",
-    "- **A24**. Alonso 2024 (TBD), which generalised the estimator to anisotropic weights."
+    "- **A24**. Alonso 2024 (https://arxiv.org/abs/2410.07077), which generalised the estimator to anisotropic weights."
    ]
   },
   {

doc/4Catalogs.html

@@ -7543,7 +7543,7 @@
 <li><strong>G19</strong>. Garcia-Garcia et al. 2019 (<a href="https://arxiv.org/abs/1906.11765">https://arxiv.org/abs/1906.11765</a>), which introduces the basic approximation used by NaMaster to estimate covariance matrix.</li>
 <li><strong>N20</strong>. Nicola et al. 2020 (<a href="https://arxiv.org/abs/2010.09717">https://arxiv.org/abs/2010.09717</a>), which refined these approximations and described in detail the procedure to estimate cosmic shear power spectra.</li>
 <li><strong>W24</strong>. Wolz et al. 2024 (<a href="https://arxiv.org/abs/2407.21013">https://arxiv.org/abs/2407.21013</a>), which introduced the formalism for catalog-based $C_\ell$s.</li>
-<li><strong>A24</strong>. Alonso 2024 (TBD), which generalised the estimator to anisotropic weights.</li>
+<li><strong>A24</strong>. Alonso 2024 (<a href="https://arxiv.org/abs/2410.07077">https://arxiv.org/abs/2410.07077</a>), which generalised the estimator to anisotropic weights.</li>
 </ul>
 </div>
 </div>

doc/4Catalogs.ipynb

@@ -27,7 +27,7 @@
     "- **G19**. Garcia-Garcia et al. 2019 (https://arxiv.org/abs/1906.11765), which introduces the basic approximation used by NaMaster to estimate covariance matrix.\n",
     "- **N20**. Nicola et al. 2020 (https://arxiv.org/abs/2010.09717), which refined these approximations and described in detail the procedure to estimate cosmic shear power spectra.\n",
     "- **W24**. Wolz et al. 2024 (https://arxiv.org/abs/2407.21013), which introduced the formalism for catalog-based $C_\\ell$s.\n",
-    "- **A24**. Alonso 2024 (TBD), which generalised the estimator to anisotropic weights."
+    "- **A24**. Alonso 2024 (https://arxiv.org/abs/2410.07077), which generalised the estimator to anisotropic weights."
    ]
   },
   {

doc/5AnisotropicWeighting.html

@@ -7540,7 +7540,7 @@
 <li><strong>G19</strong>. Garcia-Garcia et al. 2019 (<a href="https://arxiv.org/abs/1906.11765">https://arxiv.org/abs/1906.11765</a>), which introduces the basic approximation used by NaMaster to estimate covariance matrix.</li>
 <li><strong>N20</strong>. Nicola et al. 2020 (<a href="https://arxiv.org/abs/2010.09717">https://arxiv.org/abs/2010.09717</a>), which refined these approximations and described in detail the procedure to estimate cosmic shear power spectra.</li>
 <li><strong>W24</strong>. Wolz et al. 2024 (<a href="https://arxiv.org/abs/2407.21013">https://arxiv.org/abs/2407.21013</a>), which introduced the formalism for catalog-based $C_\ell$s.</li>
-<li><strong>A24</strong>. Alonso 2024 (TBD), which generalised the estimator to anisotropic weights.</li>
+<li><strong>A24</strong>. Alonso 2024 (<a href="https://arxiv.org/abs/2410.07077">https://arxiv.org/abs/2410.07077</a>), which generalised the estimator to anisotropic weights.</li>
 </ul>
 </div>
 </div>
@@ -7553,7 +7553,7 @@
 <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="5-Anisotropic-masks-">5 Anisotropic masks <a class="anchor" id="S5"></a><a class="anchor-link" href="#5-Anisotropic-masks-">¶</a></h1><p>This short tutorial shows how to use the functionality to account for anisotropic weighting of spin-$s$ fields. In short, anisotropic weighting applies different weights or masks to the different spin component of a field, and even mixes them up. This makes sense when the noise properties of your field are better characterised at every pixel by a covariance matrix that is not proportional to the identity (in which case, it may be appropriate to weight your field by the inverse of this matrix, instead of a simple scalar mask). The application of anisotropic weights causes additional mode coupling between different angular scales and $E/B$ modes, so the mode-coupling coefficients for the power spectra of these fields is also different.</p>
-<p>The code below describes one of the tests presented in <a href="TBD">Alonso et al. 2024</a> to validate the implementation of anisotropic weights in NaMaster.</p>
+<p>The code below describes one of the tests presented in <a href="https://arxiv.org/abs/2410.07077">Alonso 2024</a> to validate the implementation of anisotropic weights in NaMaster.</p>
 </div>
 </div>
 </div>

doc/5AnisotropicWeighting.ipynb

@@ -24,7 +24,7 @@
     "- **G19**. Garcia-Garcia et al. 2019 (https://arxiv.org/abs/1906.11765), which introduces the basic approximation used by NaMaster to estimate covariance matrix.\n",
     "- **N20**. Nicola et al. 2020 (https://arxiv.org/abs/2010.09717), which refined these approximations and described in detail the procedure to estimate cosmic shear power spectra.\n",
     "- **W24**. Wolz et al. 2024 (https://arxiv.org/abs/2407.21013), which introduced the formalism for catalog-based $C_\\ell$s.\n",
-    "- **A24**. Alonso 2024 (TBD), which generalised the estimator to anisotropic weights."
+    "- **A24**. Alonso 2024 (https://arxiv.org/abs/2410.07077), which generalised the estimator to anisotropic weights."
    ]
   },
   {
@@ -35,7 +35,7 @@
     "# 5 Anisotropic masks <a class=\"anchor\" id=\"S5\"></a>\n",
     "This short tutorial shows how to use the functionality to account for anisotropic weighting of spin-$s$ fields. In short, anisotropic weighting applies different weights or masks to the different spin component of a field, and even mixes them up. This makes sense when the noise properties of your field are better characterised at every pixel by a covariance matrix that is not proportional to the identity (in which case, it may be appropriate to weight your field by the inverse of this matrix, instead of a simple scalar mask). The application of anisotropic weights causes additional mode coupling between different angular scales and $E/B$ modes, so the mode-coupling coefficients for the power spectra of these fields is also different.\n",
     "\n",
-    "The code below describes one of the tests presented in [Alonso et al. 2024](TBD) to validate the implementation of anisotropic weights in NaMaster."
+    "The code below describes one of the tests presented in [Alonso 2024](https://arxiv.org/abs/2410.07077) to validate the implementation of anisotropic weights in NaMaster."
    ]
   },
   {

doc/index.rst

@@ -8,7 +8,7 @@ Welcome to NaMaster's documentation!
 
 NaMaster is a python package that provides support to compute the angular power spectrum of masked fields with arbitrary spin pymaster using the so-called pseudo-Cl formalism. ``pymaster`` is the python implementation of the NaMaster library. Below you can find links to NaMaster's full documentation, a series of detailed tutorials in the form of ipython notebooks, and various example scripts showcasing its usage. Understanding these notebooks and scripts will allow you to make the most efficient use of this package.
 
-We recommend that users read NaMaster's :download:`scientific documentation <doc_scientific.pdf>`, as well as the original paper `Alonso et al. 2019 <https://arxiv.org/abs/1809.09603>`_ to have a good understanding of the methods implemented in the library. Additional useful information, particularly regarding the calculation of covariance matrices, can be found in `Garcia-Garcia et al. 2019 <https://arxiv.org/abs/1906.11765>`_, and `Nicola et al. 2021 <https://arxiv.org/abs/2010.09717>`_. We kindly request that you cite these papers where relevant.
+We recommend that users read NaMaster's :download:`scientific documentation <doc_scientific.pdf>`, as well as the original paper `Alonso et al. 2019 <https://arxiv.org/abs/1809.09603>`_ to have a good understanding of the methods implemented in the library. Additional useful information, particularly regarding the calculation of covariance matrices, can be found in `Garcia-Garcia et al. 2019 <https://arxiv.org/abs/1906.11765>`_, and `Nicola et al. 2021 <https://arxiv.org/abs/2010.09717>`_. Support for catalog-based fields was documented in `Wolz et al. 2024 <https://arxiv.org/abs/2407.21013>`_, and the estimator's extension to anisotropic weighting of spin-s fields was presented in `Alonso 2024 <https://arxiv.org/abs/2410.07077>`_. We kindly request that you cite these papers where relevant.
 
 .. toctree::
    :maxdepth: 1