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Christer Watson edited sectionAnalysis__sub.tex
over 8 years ago
Commit id: 79e56b3b892b610c392c971ad964b75a8672c867
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B_{mod} =B_0 \frac{2 h \nu^{3+\beta}}{c^3}\frac{1}{e^{\frac{h\nu}{kT}}-1}
\end{equation*}
where
$\beta$ $\beta${\bf, the emissivity index,} is assumed to be 2 \citep{Desert2008}. B$_0$ and T were taken as free parameters and a Levenberg{\textendash}Marquardt algorithm was used to find the best-fit. The fitting was done to the flux density in Jy, so B$_0$ carries these units. The total column density was calculated following \citet{Miettinen_2010}. Briefly, we used the following relations:
\begin{eqnarray*}
N_{tot} = \frac{I}{B_\nu \mu m_H \kappa R_d}\nonumber\\