deletions | additions       diff --git a/Scientific Justification.tex b/Scientific Justification.tex  index 1d2679b..384b572 100644  --- a/Scientific Justification.tex  +++ b/Scientific Justification.tex 
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The filament FN1 is identified based on the dendrogram analysis and its continuity in the position-position-velocity (PPV) space (Lee et al. 2014). It is selected as our target to test the two methods above because of its large velocity gradient (3.2 km/s), which makes it well distinguishable in the PPV space. Also, FN1 is not associated with any YSOs, and thus does not suffer from kinematics and chemistry complications around YSOs. It is bright in the N_2H^+ (1-0) emission, which suggests the detection of N_2H^+ (3-2) and makes it an ideal target for testing the 1st method described above. The large velocity dispersion of FN1 indicates that trans-/super-sonic turbulence dominates the region, which follows the assumption of the 2nd method above.  \subsection{Proposed observation}  {\bf Here we propose to observe the N_2H^+ (3-2; 279.511760 GHz) (3-2)  and the ^{13}CO (2-1; 220.398684 GHz)/C^{18}O (2-1; 219.560358 GHz) (2-1)/C^{18}O (2-1)  line emission of the filament FN1} in the Serpens Main molecular cloud. The first set of observations (N_2H^+ 3-2) 3-2; 279.511760 GHz)  allows us to test the 1st method described above, which estimates the line of sight ``thickness'' by the dependence of emission from N_2H^+ transitions on the volume density. The second set of observations (CO isotopologues) (^{13}CO and C^{18}O at 220.398684 GHz and 219.560358 GHz, respectively)  allows us to test the 2nd method, which estimates the line of sight thickness by the dependence of the Spectral Correlation Function on the spatial lag. The observations will in turn allow us to compare the results from the two methods. To obtain maps that cover a sufficient region along the filament and across the filament, we propose mosaicking observation composed of ten pointings in the hexagonal arrangement to Nyquist-sample the region. At 270 GHz, this will give us a coverage of \~ 100 arcsec (\~ 0.23 pc at the diatance of Serpens Main) along the filament, and of \~ 80 arcsec (\~ 0.18 pc) across the filament. At 230 GHz, the coverage is \~ 1.3 times larger in length unit. (spectral setup...)