this is for holding javascript data
Elisabeth Newton (Air) json file for the actual M dwarf data
over 10 years ago
Commit id: 8774323f5eefbdc7b5c7483e391bf821b8fc526f
deletions | additions
diff --git a/sample_states.json b/sample_states.json
new file mode 100644
index 0000000..cdff0cb
--- /dev/null
+++ b/sample_states.json
...
{
"states" : [{
"grid" : { "nRows" : 1,
"nColumns" : 4},
"name" : "All the stars",
"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",
"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" : "Spectral Types",
}
]
},
{
"grid" : { "nRows" : 1,
"nColumns" : 2},
"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",
"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" : "Spectral Types",
}
]
}
]
}