Move 3D flux points into separate section
"cell_type": "markdown",
"metadata": {},
"source": [
- "Finally we compute flux points and check again our model (including now the diffuse emission):"
+ "## Computing Flux Points\n",
+ "\n",
+ "Finally we compute flux points for the galactic center source. For this we first define an energy binning:"
]
},
{
]
},
{
- "cell_type": "code",
- "execution_count": null,
+ "cell_type": "markdown",
"metadata": {},
- "outputs": [],
"source": [
- "ax = flux_points.plot(energy_power=2)\n",
- "model_ecpl.spectral_model.plot(ax=ax, energy_range=energy_range, energy_power=2);"
+ "Now let's plot the best fit model and flux points:"
]
},
{
- "cell_type": "markdown",
+ "cell_type": "code",
+ "execution_count": null,
"metadata": {},
+ "outputs": [],
"source": [
- "Results seems to be better (but not perfect yet). Next step to improve our model even more would be getting rid of the other bright source (G0.9+0.1)."
+ "flux_points.table[\"is_ul\"] = flux_points.table[\"ts\"] < 4\n",
+ "ax = flux_points.plot(energy_power=2)\n",
+ "model_ecpl.spectral_model.plot(ax=ax, energy_range=energy_range, energy_power=2);"
]
},
{
"cell_type": "markdown",
"metadata": {},
"source": [
+ "## Summary\n",
+ "\n",
"Note that this notebook aims to show you the procedure of a 3D analysis using just a few observations and a cutted Fermi model. Results get much better for a more complete analysis considering the GPS dataset from the CTA First Data Challenge (DC-1) and also the CTA model for the Galactic diffuse emission, as shown in the next image:"
]
},
