updates based on JOSS review and fixing broken link

docs/index.rst

@@ -164,12 +164,10 @@ contributors who will abide by the `Python Software Foundation Code of Conduct
 `Astropy`_.  The following pages will help you get started with contributing
 fixes, code, or documentation (no git or GitHub experience necessary):
 
-* `How to make a code contribution <https://docs.astropy.org/en/stable/development/workflow/development_workflow.html>`_
+* `How to make a code contribution <https://docs.astropy.org/en/latest/index_dev.html>`_
 
 * `Coding Guidelines <https://docs.astropy.org/en/stable/development/codeguide.html>`_
 
-* `Developer Documentation <https://docs.astropy.org/en/latest/index_dev.html>`_
-
 For the complete list of contributors please see the `dust_extinction
 contributors page on Github
 <https://github.com/karllark/dust_extinction/graphs/contributors>`_.

paper/paper.bib

@@ -17,6 +17,18 @@ @ARTICLE{Astropy22
       adsnote = {Provided by the SAO/NASA Astrophysics Data System}
 }
 
+@software{Barbary16,
+       author = {{Barbary}, Kyle},
+        title = "{extinction v0.3.0}",
+         year = 2016,
+        month = dec,
+          eid = {10.5281/zenodo.804967},
+          doi = {10.5281/zenodo.804967},
+    publisher = {Zenodo},
+       adsurl = {https://ui.adsabs.harvard.edu/abs/2016zndo....804967B},
+      adsnote = {Provided by the SAO/NASA Astrophysics Data System}
+}
+
 @ARTICLE{Bastiaansen92,
        author = {{Bastiaansen}, P.~A.},
         title = "{Narrow band multicolor photometry of reddened and unreddened early-type stars.}",

paper/paper.md

@@ -36,19 +36,21 @@ in one place with a consistent interface.
 Many observation- and theory-based extinction curves have been presented
 in the literature. Having one python package providing these models ensures
 that they are straightforward to use and used within their valid wavelength
-and parameter (where appropriate) ranges.
+and parameter (where appropriate) ranges.  Other packages provide extinction
+curves, but they generally provide one or a small number of curves for 
+specialized purposes [e.g., @Barbary16].
 
 The types of extinction models supported are Averages, Parameter Averages, Grain
 Models, and Shapes. The Averages are averages of a set of measured extinction
-curves and examples are shown in Fig. \autoref{fig:averages}. The Parameter
+curves and examples are shown in \autoref{fig:averages}. The Parameter
 Averages are extinction curve averages that depend on a parameter, often $R(V) =
-A(V)/E(B-V)$ which is the ratio of total to selective extinction. Fig.
+A(V)/E(B-V)$ which is the ratio of total to selective extinction. 
 \autoref{fig:parameter_averages} shows examples of such models. The Grain
-Models are those extinction curves computed using dust grain models. See Fig.
+Models are those extinction curves computed using dust grain models. See
 \autoref{fig:grain} and note that these models provide dust extinction
 predictions from X-ray through submm wavelengths. The final type of models
 are Shapes that provide flexible functional forms that fit selected wavelength
-ranges (see Fig. \autoref{fig:shapes} for an example).
+ranges (see \autoref{fig:shapes} for an example).
 
 ![Examples of Average models based on observations in the Milky Way, Large Magellanic Cloud (LMC), and Small Magellanic Cloud (SMC) [@Bastiaansen92; @Gordon03; @Gordon09; @Gordon21; @Gordon24].\label{fig:averages}](average_models_uv_nir.png){
 width=70% }
@@ -68,7 +70,7 @@ a helper `extinguish` function that alternatively provides the fractional
 effects of extinction for a specific dust column (e.g., $A(V)$ value). This
 allows for the effects of dust to be modeled for or removed from an observation.
 
-This package does not implement dust attenuation models. Dust attenuation
+This package does not implement dust attenuation models[^1]. Dust attenuation
 results when observing more complex systems like a star with nearby,
 circumstellar dust or a galaxy with many stars extinguished by different amounts
 of dust. In both cases, the wavelength dependence of effects of dust are
@@ -77,6 +79,8 @@ dust radiative transfer [@Steinacker13]. Specifically, these effects are the ave
 extinguished by differing amount of dust and the inclusion of a significant
 number of photons scattered into the observing beam.
 
+[^1]: See [karllark/dust_attenuation](https://github.com/karllark/dust_attenuation).
+
 Any published dust extinction model is welcome for inclusion in this package.
 
 # References