update documentations

astrosmili · Mar 29, 2019 · 94cef6c · 94cef6c
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diff --git a/docs/_examples/image/imfits.ipynb b/docs/_examples/image/imfits.ipynb
@@ -11,7 +11,7 @@
    "cell_type": "markdown",
    "metadata": {},
    "source": [
-    "The most basic class for the image in SMILI is **imdata.IMFITS** object.Here, we show its basic usage.\n",
+    "The most basic class for the image in SMILI is *imdata.IMFITS* object.Here, we show its basic usage.\n",
     "You can see list of functions at [in this page](../../_autodoc/smili.html)."
    ]
   },

diff --git a/docs/_examples/imaging/imaging.ipynb b/docs/_examples/imaging/imaging.ipynb
@@ -11,7 +11,7 @@
    "cell_type": "markdown",
    "metadata": {},
    "source": [
-    "Here, we show a quick example of imaging using *imaging.lbfgs* module. In this notebook, we do not go to details of its theoretical backgroud nor practical imaging procedures; here we focus on going through the basic functions. We also note that the imaging function has been dynamical updated, so its usage may change on short time scales.  Here, we use a [VLBA data set of 3C 273 at 43 GHz](3C273DEC16.UVP) of [the Boston University Blazar Group](https://www.bu.edu/blazars/VLBAproject.html)."
+    "We show a quick example of imaging using *imaging.lbfgs* module. In this notebook, we do not go to details of its theoretical backgroud nor imaging procedures (tuning parameters, iterative imaging, self-calbiration, etc.); here we focus on going through the basic functions. We also note that the imaging function has been dynamical updated, so its usage may change on short time scales.  We use a [VLBA data set of 3C 273 at 43 GHz](3C273DEC16.UVP) of [the Boston University Blazar Group](https://www.bu.edu/blazars/VLBAproject.html)."
    ]
   },
   {
@@ -510,7 +510,7 @@
     "    if i < 2: # for the first two times, we will use amplitudes\n",
     "        imprm[\"amptable\"] = atable\n",
     "        imprm[\"vistable\"] = None\n",
-    "        imprm[\"cen_lambda\"] = 1  # don't forget to switch off the centroid regularizer, since now we have absolute position information from full complex visibilities.\n",
+    "        imprm[\"cen_lambda\"] = 1  # we need the centroid regularization during closure imaging, since the absolute potition information will be lost.\n",
     "    else:\n",
     "        imprm[\"amptable\"] = None\n",
     "        imprm[\"vistable\"] = vtable\n",

diff --git a/docs/_examples/uvdata/uvdata.ipynb b/docs/_examples/uvdata/uvdata.ipynb
@@ -11,7 +11,7 @@
    "cell_type": "markdown",
    "metadata": {},
    "source": [
-    "In SMILI, interfreometric data sets are handle by **uvdata** module. Here, we show a basic usage of uvdata module using a [VLBA data set of 3C 273 at 43 GHz](3C273DEC16.UVP) of [the Boston University Blazar Group](https://www.bu.edu/blazars/VLBAproject.html)."
+    "In SMILI, interfreometric data sets are handle by *uvdata* module. Here, we show a basic usage of uvdata module using a [VLBA data set of 3C 273 at 43 GHz](3C273DEC16.UVP) of [the Boston University Blazar Group](https://www.bu.edu/blazars/VLBAproject.html)."
    ]
   },
   {
@@ -550,7 +550,7 @@
    "cell_type": "markdown",
    "metadata": {},
    "source": [
-    "**uvdata.VisTable** has simple plot methods uvplot and raplot for plotting uv-coverages and radial plots. Each function is mocking pyploy.plot or pyplot.errorbar functions, and you can use almost all of arguments for pyplot.plot or pyplot.errorbar."
+    "*uvdata.VisTable* has simple plot methods uvplot and raplot for plotting uv-coverages and radial plots. Each function is mocking pyploy.plot or pyplot.errorbar functions, and you can use almost all of arguments for pyplot.plot or pyplot.errorbar."
    ]
   },
   {
@@ -645,7 +645,7 @@
    "cell_type": "markdown",
    "metadata": {},
    "source": [
-    "## 3.3 Make tables for bispectra and log closure amplitudes\n",
+    "## Make tables for bispectra and log closure amplitudes\n",
     "\n",
     "From *uvdata.VisTable*, you can make tables for closure quantities such as bispectra (*uvdata.BSTable*) and log closure amplitudes (*uvdata.CATable*). The classes of both table also inherit pandas.DataFrame class, so you can use this class like pandas.DataFrame. "
    ]

diff --git a/docs/_static/install.rst b/docs/_static/install.rst
@@ -170,9 +170,9 @@ Then install Anaconda.
   .. code-block:: Bash
 
     # Download the source code
-    wget http://www.fftw.org/fftw-3.3.X.tar.gz
-    tar xzvf fftw-3.3.X.tar.gz
-    cd fftw-3.X.7
+    wget http://www.fftw.org/fftw-3.X.X.tar.gz
+    tar xzvf fftw-3.X.X.tar.gz
+    cd fftw-3.X.X
 
     # Install
     ./configure prefix="/usr/local" --enable-openmp --enable-threads --enable-shared