Total velocity dispersion versus observed central column density. Similar plot to Fig. 6 for the filaments observed in IC 5146, Aquila and Polaris. The six C¹⁸O spectra showing two or three velocity components are flagged in yellow.

N₂H⁺(1−0) spectra observed toward filaments 6, 12, 13 in IC 5146. The filament numbers are indicated at the upper right of each panel. The corresponding one velocity hyperfine structure Gaussian fits are highlighted in blue.

C¹⁸O(2–1) spectra observed toward 6 filaments in IC 5146. The filament numbers are indicated at the upper right of each panel. The corresponding single-component Gaussian fits are highlighted in blue.

N₂H⁺(1−0) spectra observed toward 9 filaments in Aquila. The numbers indicated on the upper right hand side of the plots, correspond to the filaments marked on the column density map of Fig. A.5 and listed in Table 1. The corresponding single-component hyperfine structure Gaussian fits are highlighted in blue. Note that the y-axis scale is not the same for all spectra, but has been adjusted to match the peak temperatures which vary between  ~ 0.2 to  > 3 K.

Curvelet component of the column density map of the Aquila field around the Serpens South filaments taken from André et al. (2010). The curvelet component is obtained using a morphological component analysis algorithm (MCA, from Starck et al. 2003) which enhances the contrast of the filamentary structure against the more diffuse background of the cloud. The positions of the observed spectra are plotted in red squares and blue triangles for N₂H⁺ and C¹⁸O, respectively. The numbers correspond to the filaments listed in Table 1 and are given at the upper right of the spectra in Fig. A.4 and some of the spectra of Fig. A.7.

Continuation of Fig. A.4 presenting the N₂H⁺(1−0) spectra observed toward 9 filaments in Aquila.

C¹⁸O(1−0) spectra observed toward 6 filaments in Aquila. The corresponding Gaussian fits are highlighted in blue. Note that the scale of the y-axis has been adjusted to match the peak temperature of each spectrum. Note 1: filament 20 shows two components separated by 0.63 km s^-1. The component at V_LSR = 7.17 km s^-1 have been chosen to be tracing the filament, since this component has a velocity component which is closer to the average velocity ( km s^-1) of the filaments in Aquila which show one velocity component. Note 2: the spectrum observed at the position of filament 22 shows two velocity components, one centered at 6.5 km s^-1 and the other at 7.7 km s^-1. The strongest component has been selected for similar reasons to that explained for filament 20. Note 3: the spectrum observed at the position of filament 25 has two velocity components (at 5.0 km s^-1 and 6.52 km s^-1, respectively). The strongest component has been selected for similar reasons to that explained for filament 20. Note 4: the spectrum observed at the position of filament 26 shows three velocity components centered at 7.28 km s^-1, 8.45 km s^-1 and 9.17 km s^-1, respectively. The component centered at 7.28 km s^-1 has been selected because it is the component with the closest V_LSR value to the mean of neighboring filaments in Aquila.

C¹⁸O(1−0) spectra observed toward filaments 23 and 24 in Aquila, located in the south west part of the region. The positions of the two filaments are shown on a blow up of the column density map (cf., Könyves et al. 2010)on the right hand side. Filament 24 shows a single velocity C¹⁸O(1−0) spectrum at V_LSR = 6.87 km s^-1, while C¹⁸O(1−0) spectrum observed toward filament 23 shows three velocity components at V_LSR = 5.77 km s^-1, 9.13 km s^-1 and 10.3 km s^-1. The relevant velocity component associated to filament 23 is most probably the component at V_LSR = 5.77 km s^-1 (the closest to the LSR velocity of the neighboring filament 24), while the other components are likely associated to clouds/filaments observed on the same line-of-sight.

N₂H⁺(1−0) spectrum observed toward filament 1 in Polaris. The corresponding hyperfine structure Gaussian fit is highlighted in blue.

Curvelet component of the column density map of a subregion in the Polaris Cloud taken from André et al. (2010). The positions of the observed spectra are plotted in red squares and blue triangles for N₂H⁺ and C¹⁸O, respectively. The numbers correspond to the filaments listed in Table 1.

C¹⁸O(1−0) spectra observed toward 6 filaments in Polaris. The corresponding Gaussian fits are highlighted in blue. Note 1: the spectrum observed toward filament 4 shows two velocity components. Both velocity components have similar linewidths (0.19 km s^-1 and 0.14 km s^-1, respectively), they are separated by  ~0.8 km s^-1. They most probably belong to two filaments which are seen on the same line-of-sight (but a large map would be needed to study the kinematics of the field). The component observed at  −4.5 km s^-1 has been taken to be representative of filament 4.