deletions | additions       diff --git a/sample_states.json b/sample_states.json  index cdff0cb..10ce34b 100644  --- a/sample_states.json  +++ b/sample_states.json 
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"caption" : "This plot shows the near-infrared 2MASS colors of M dwarfs observed by Newton et al. (2013). One color is plotted on the x-axis and another color is plotted on the y-axis. The stars trace out a main sequence, with some scatter.",  "plots" : [ {   "gridPosition" : [0,0],  "xAxis" : "J-Ks", "J-K",  "yAxis" : "H-K", "H-K"  },  {   "gridPosition" : [0,1], 
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},  {   "gridPosition" : [0,3],  "xAxis" : "Spectral Types", "H2OK2 Index",  "yAxis" : "H2OK2 Index"  } ]  },  {  "grid" : { "nRows" : 1,  "nColumns" : 2}, 4},  "name" : "Early M dwarfs",  "caption" : "",  "plots" : [ {   "gridPosition" : [0,0],  "xAxis" : "J-K",  "yAxis" : "H-K"  },  {   "gridPosition" : [0,1],  "xAxis" : "H-K",  "yAxis" : "J-H"  },  {   "gridPosition" : [0,2],  "xAxis" : "J-K",  "yAxis" : "J-H"  },  {   "gridPosition" : [0,3],  "xAxis" : "H2OK2 Index",  "yAxis" : "H2OK2 Index" }  ]  },  {  "grid" : { "nRows" : 1,  "nColumns" : 4},  "name" : "All the stars and their iron abundances",  "colorAxis" : "[Fe/H]",  "colorMap" : "YlOrRd",  "caption" : "In this plot, the near-infrared colors of the M dwarfs remain the same. However, now the stars are colored by their iron abundance, [Fe/H]. The [Fe/H] of each star was inferred following the methods described in Newton et al. (2013), which use the equivalent width of the Na line near 2.2 microns as a proxy for metallicity. You can see that a metal-rich star is seen to have a different color than a more metal-poor star of the same spectral type. This allowed us to calibrate a relation for iron abundance using 2MASS photometry.",  "plots" : [ {   "gridPosition" : [0,0],  "xAxis" : "J-Ks", "J-K",  "yAxis" : "H-K", "H-K"  },  {   "gridPosition" : [0,1], 
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},  {   "gridPosition" : [0,3],  "xAxis" : "Spectral Types", "H2OK2 Index",  "yAxis" : "H2OK2 Index"  } ]  }  ]  }