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`29`	`29`	`"#IFrame(\"doc/Physics/star_spectro_intro.pdf\", width=1200, height=800)"`
`30`	`30`	`]`
`31`	`31`	`},`
	`32`	`+ {`
	`33`	`+ "cell_type": "code",`
	`34`	`+ "execution_count": null,`
	`35`	`+ "metadata": {},`
	`36`	`+ "outputs": [],`
	`37`	`+ "source": []`
	`38`	`+ },`
	`39`	`+ {`
	`40`	`+ "cell_type": "markdown",`
	`41`	`+ "metadata": {},`
	`42`	`+ "source": [`
	`43`	`+ "## Why spectroscopy lines should be modeled as Lorentzian functions\n",`
	`44`	`+ "\n",`
	`45`	`+ "This introduction directly inspired by the [wikipedia article](https://en.wikipedia.org/wiki/Cauchy_distribution)"`
	`46`	`+ ]`
	`47`	`+ },`
`32`	`48`	`{`
`33`	`49`	`"cell_type": "code",`
`34`	`50`	`"execution_count": null,`

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