inclined with respect to the Galactic plane and to the large-scale magnetic-field direction in the local ISM. Both clouds have magnetic pressures of the same magnitude as the thermal ones. Nevertheless, we find that the γ-ray emissivity per gas nucleon in one cloud, Reticulum, is $1.57 \pm 0.09$ times larger than in the other cloud, Eridu, over the whole energy range of analysis, from 0.16 to 63 GeV. The difference cannot be attributed to uncertainties in gas mass because the correlation between the dust and γ-ray data allows an efficient detection of any additional gas that is not traced by H I line emission (as we find in Reticulum) and the γ-ray contribution of this additional gas is included in the model. Furthermore, we cannot reduce the CR flux ratio below $1.32 \pm 0.08$ when allowing for strong differences in H I spin temperature between the two clouds (at the expense of a poorer γ-ray fit).

Beyond characterising the global magnetic orientation and average field strength of a few microGauss in the clouds, we studied turbulence characteristics at a parsec scale that might hint at different environmental conditions for CR diffusion, namely the dispersion in gas velocity and in magnetic-field orientation, differences in the sonic Mach numbers (compressibility) of the turbulence, and differences in magnetisation level (magnetic stiffness against gas turbulent motions). We find that the two clouds compare well in all these aspects. The only notable difference is that the core of the Reticulum cloud has collapsed (or has been compressed) to larger densities typical of the CNM and DNM phases, whereas a large fraction of the more diffuse gas in Eridu may be transitioning through the unstable, lukewarm phase. MHD simulations will help in studying the level of magnetic-field tangling in the different atomic and DNM gas phases, or in shell compression behind a slow shock, in order to search for changes that may impact the collective drift of the CR population, such as changes in the turbulent energy fraction of fast compressive modes or in the density of magnetic mirrors (Lazarian et al. 2023).

Alternatively, the 1–500 GeV/n CRs we probed in γ rays may primarily scatter off MHD waves they have excited through streaming instability. If so, one expects a stronger damping in the denser Reticulum cloud, but we show that the difference in expected steady-state diffusion coefficient between the two clouds can be small (less than a factor of two) because the increase in diffusion length with the ambient gas density is moderated by the corresponding drop in gas temperature and ionisation fraction. We plan to further investigate the impact of charged dust grains, which should reduce the damping rates along the core of the two clouds (Hennebelle & Lebreuilly 2023). However, we only probed the cloud properties at a parsec scale, whereas the growth and damping of the relevant MHD waves occur at wavelengths of a few micro-parsecs where the interstellar gas properties cannot be explored. Moreover, in the self-confinement mode, the wave growth rate in each cloud relates to the degree of anisotropy in CR pitch angle or, equivalently, to the steepness of the local CR spatial density gradient (Zweibel 2013), which could differ in the vicinity of the clouds or in bottlenecks along their edge (different $l_{CR}$).

The damping rates we estimate suggest that the magnetic perturbations propagating along the field lines should dissipate over typical lengths of tens to hundreds of micro-parsecs. ($l \approx 10^{10}$pc, $T \approx 10^{10}$K, $\dot{\Gamma}/\Gamma_{\text{E}} \sim 10^{-3}$, Spangler et al. 2011). The median of their distribution is $A$ in

twice as large in Eridu as in Reticulum. The dissipation lengths correspond to proton gyro-radii for energies in the~10 GeV to ~1 TeV band, with a median energy three times larger in Eridu than in Reticulum. The waves must be constantly replenished or we would observe a spectral change in γ-ray emissivity in

the corresponding ~1 to ~100 GeV band as the higher-energy particles would leak out more rapidly. The fact that we find a change in CR flux but not in spectrum between the two clouds is therefore an important constraint. The same overall spectrum has been observed in several clouds in the local ISM (Grenier et al. 2015), but with improved photon statistics the Fermi-LAT data can now serve to precisely test the uniformity of this spectrum in different types of atomic clouds and independently of the CR flux pervading them.

**Acknowledgements.** We thank Jeong-Gyu Kim for sharing his interstellar model for the solar neighbourhood conditions, Lucia Armillotta for sharing information from her work, the members of the Interstellar Institute (I2) CNRS International Research Network for enlightening discussions, and the referee for helping us clarify several points in the discussion. We acknowledge the financial support by the LabEx UnivEarthS (ANR-10-LABX-0023 and ANR-18-IDEX-0001) for this work. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l'Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.

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**Appendix A: Distance estimates to the nearby clouds**

We used the 3D dust distribution reconstructed from stellar surveys by Leike et al. (2020) out to distances of about 400 pc from the Sun to place constraints on the distance to different cloud complexes seen in the analysis region. Figure A.1 displays the

dust extinction in the G band in contiguous 20-pc-wide intervals. The lack of dust information at latitudes below about 50° for the three most distant intervals is due to the limited size of the 3D data cube perpendicular to the Galactic plane (±270 pc). In addition to those maps, one can plot the extinction profile as a function of distance along sight lines of large $N_H$ column density in each cloud. Examples are shown in Fig. A.2 when

<figure><img src="image_22.png" /><figcaption>**Fig. A.1.** Maps of the G-band extinction optical depth integrated over 20 pc-wide intervals in distance from the Sun across the analysis region. The data come from the 3D distribution of Leike et al. (2020). The distance ranges are labelled in each map. The black contours delineate the Reticulum HI cloud as in Fig. 1.</figcaption></figure>

<figure><img src="image_23.png" /><figcaption>**Fig. A.2.** Dust extinction density profiles as a function of radial distance from the Sun for selected lines of sight along the Reticulum filament. The data come from the 3D distribution of Leike et al. (2020).</figcaption></figure>
**Appendix A: Distance estimates to the nearby clouds**

We used the 3D dust distribution reconstructed from stellar surveys by Leike et al. (2020) out to distances of about 400 pc from the Sun to place constraints on the distance to different cloud complexes seen in the analysis region. Figure A.1 displays the

dust extinction in the G band in contiguous 20-pc-wide intervals. The lack of dust information at latitudes below about 50° for the three most distant intervals is due to the limited size of the 3D data cube perpendicular to the Galactic plane (±270 pc). In addition to those maps, one can plot the extinction profile as a function of distance along sight lines of large $N_H$ column density in each cloud. Examples are shown in Fig. A.2 when

<figure><img src="image_21.png" /><figcaption>**Fig. A.1.** Maps of the G-band extinction optical depth integrated over 20 pc-wide intervals in distance from the Sun across the analysis region. The data come from the 3D distribution of Leike et al. (2020). The distance ranges are labelled in each map. The black contours delineate the Reticulum HI cloud as in Fig. 1.</figcaption></figure>

<figure><img src="image_22.png" /><figcaption>**Fig. A.2.** Dust extinction density profiles as a function of radial distance from the Sun for selected lines of sight along the Reticulum filament. The data come from the 3D distribution of Leike et al. (2020).</figcaption></figure>
<figure><img src="image_24.png" /><figcaption>**Fig. A.3.** Maps of the G-band extinction optical depth integrated over 20 pc-wide intervals in distance from the Sun, towards the Orion-Eridanus region. The data come from the 3D distribution of Leike et al. (2020). The dust cloud that spans the region nearly horizontally around $b = 50^\circ$ and at distances between 160 and 260 pc marks the rim of the Orion-Eridanus superbubble. At larger distances, the black contours delineate the Eridu HI cloud as in Fig. 1. The distance ranges are labelled in each map.</figcaption></figure>

probing directions along the Reticulum filament. We used the peaks found in the dust profiles and the correspondence in shape found between atomic clouds in Fig. 3 and dust clouds in Fig. A.1 to estimate the cloud distances that are given in Sect. A.

We repeated the analysis to revisit the distance to the Eridu cloud. The latter, being rather diffuse, is more difficult to identify in the dust data, but Fig. A.3 suggests that it lies at about 300 pc from the Sun, beyond the edge of the Orion-Eridanus superbubble that is clearly detected at closer distances around 200 pc as the long arc crossing the maps horizontally at latitudes around -50°.

## Appendix B: ISM properties in the 1°-wide squares along the cloud filaments

Tables B.1 and B.2 list the mean value and rms dispersion of the interstellar properties found in the 1°×1° squares that are depicted in Fig. 10 and that span the length of the Reticulum and Eridu filaments, along their core. The properties include the LOS depth, the $N_{HI}$ column density and $n_{HI}$ volume density in the atomic gas, the HI velocity dispersion in the plane of the sky ($S_v$) and along the line of sight ($\sigma_v$ line width), the gas temperature $T$ and the abundance ($x_{ion}$) and atomic weight ($A_{ion}$) of ions inferred from the gas density and the Kim et al. (2023) model, the $B_{sky}$ magnetic-field strengths estimated according to Eqs. 12 and 13 with the $S_v$ velocity dispersion or $\sigma_v$ line width as a proxy for the turbulent velocity $\delta v$, the sonic Mach numbers $M_s$ of the turbulence for the same options in $\delta v$, the Alfvénic Mach numbers $M_A$ of the MHD turbulence inferred with the ST and DCF methods, the ion-neutral damping rate according to Eq. 5, and the steady-state $\kappa_\parallel$ diffusion coefficient for self-confinement with the CR flux reaching the heliosphere in the 1–20 GV rigidity range.
<figure><img src="image_23.png" /><figcaption>**Fig. A.3.** Maps of the G-band extinction optical depth integrated over 20 pc-wide intervals in distance from the Sun, towards the Orion-Eridanus region. The data come from the 3D distribution of Leike et al. (2020). The dust cloud that spans the region nearly horizontally around *b* = 50° and at distances between 160 and 260 pc marks the rim of the Orion-Eridanus superbubble. At larger distances, the black contours delineate the Eridu HI cloud as in Fig. 1. The distance ranges are labelled in each map.</figcaption></figure>

probing directions along the Reticulum filament. We used the peaks found in the dust profiles and the correspondence in shape found between atomic clouds in Fig. 3 and dust clouds in Fig. A.1 to estimate the cloud distances that are given in Sect. A.

We repeated the analysis to revisit the distance to the Eridu cloud. The latter, being rather diffuse, is more difficult to identify in the dust data, but Fig. A.3 suggests that it lies at about 300 pc from the Sun, beyond the edge of the Orion-Eridanus superbubble that is clearly detected at closer distances around 200 pc as the long arc crossing the maps horizontally at latitudes around -50°.

**Appendix B: ISM properties in the 1°-wide squares along the cloud filaments**

Tables B.1 and B.2 list the mean value and rms dispersion of the interstellar properties found in the 1°×1° squares that are depicted in Fig. 10 and that span the length of the Reticulum and Eridu filaments, along their core. The properties include the LOS depth, the *N*<sub>HI</sub> column density and *n*<sub>HI</sub> volume density in the atomic gas, the HI velocity dispersion in the plane of the sky (*S*<sub>v</sub>) and along the line of sight (*σ*<sub>v</sub> line width), the gas temperature *T* and the abundance (*x*<sub>ion</sub>) and atomic weight (*A*<sub>ion</sub>) of ions inferred from the gas density and the Kim et al. (2023) model, the *B*<sub>sky</sub> magnetic-field strengths estimated according to Eqs. 12 and 13 with the *S*<sub>v</sub> velocity dispersion or *σ*<sub>v</sub> line width as a proxy for the turbulent velocity *δ*<sub>v</sub>, the sonic Mach numbers *M*<sub>S</sub> of the turbulence for the same options in *δ*<sub>v</sub>, the Alfvénic Mach numbers *M*<sub>A</sub> of the MHD turbulence inferred with the ST and DCF methods, the ion-neutral damping rate according to Eq. 5, and the steady-state *κ*<sub>||</sub> diffusion coefficient for self-confinement with the CR flux reaching the heliosphere in the 1–20 GV rigidity range.
<table><caption>**Table B.1.** ISM properties along the Reticulum filament, for the fiber (regular font) or shell (bold font) geometry. The values and errors respectively give the mean value in each ~5 pc-wide square and the rms dispersion at 0.5–0.7 pc scale within each square. The Galactic coordinates refer to the square centre.</caption><tbody><tr><td>long. [deg]</td><td>282.09</td><td>281.58</td><td>280.05</td><td>277.51</td><td>276.15</td><td>272.59</td><td>269.88</td><td>268.18</td></tr><tr><td>lat. [deg]</td><td>-41.25</td><td>-42.0</td><td>-43.88</td><td>-46.25</td><td>-47.38</td><td>-49.12</td><td>-50.88</td><td>-51.5</td></tr><tr><td>N<sub>HI</sub> [10<sup>20</sup> cm<sup>-2</sup>]</td><td>4.4</td><td>3.8</td><td>3.4</td><td>2.5</td><td>2.2</td><td>1.9</td><td>1.4</td><td>1.4</td></tr><tr><td>LOS depth [pc]</td><td>3.6 ± 0.5</td><td>5.4 ± 0.7</td><td>3.6 ± 0.4</td><td>3.7 ± 0.5</td><td>5.2 ± 0.6</td><td>5.0 ± 0.6</td><td>4.4 ± 0.6</td><td>7.9 ± 1.0</td></tr><tr><td></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td></tr><tr><td>n<sub>HI</sub> [cm<sup>-3</sup>]</td><td>39 ± 11</td><td>23 ± 6</td><td>31 ± 14</td><td>22 ± 13</td><td>14 ± 3</td><td>12 ± 3</td><td>10 ± 3</td><td>6 ± 1</td></tr><tr><td></td><td><b>7 ± 2</b></td><td><b>6 ± 2</b></td><td><b>6 ± 3</b></td><td><b>4 ± 2</b></td><td><b>4 ± 1</b></td><td><b>3 ± 0.8</b></td><td><b>2 ± 0.5</b></td><td><b>2 ± 0.4</b></td></tr><tr><td>S<sub>v</sub> [km s<sup>-1</sup>]</td><td>0.78</td><td>0.48</td><td>0.48</td><td>0.52</td><td>0.49</td><td>0.55</td><td>0.81</td><td>0.37</td></tr><tr><td>σ<sub>v</sub> [km s<sup>-1</sup>]</td><td>2.2</td><td>1.9</td><td>1.7</td><td>1.4</td><td>1.3</td><td>1.5</td><td>2.3</td><td>1.4</td></tr><tr><td>S<sub>ψ</sub> [deg]</td><td>19.95</td><td>24.44</td><td>10.73</td><td>14.9</td><td>11.8</td><td>28.74</td><td>35.62</td><td>42.91</td></tr><tr><td>T [K]</td><td>106</td><td>143</td><td>130</td><td>194</td><td>220</td><td>238</td><td>290</td><td>502</td></tr><tr><td></td><td><b>503</b></td><td><b>517</b></td><td><b>843</b></td><td><b>1581</b></td><td><b>1193</b></td><td><b>1457</b></td><td><b>2322</b></td><td><b>2044</b></td></tr><tr><td>x<sub>ion</sub> [10<sup>-4</sup>]</td><td>4.2</td><td>6.3</td><td>5.6</td><td>8.9</td><td>10.5</td><td>11.5</td><td>14.2</td><td>24.3</td></tr><tr><td></td><td><b>23.2</b></td><td><b>24.6</b></td><td><b>35.3</b></td><td><b>59.2</b></td><td><b>48.4</b></td><td><b>56.9</b></td><td><b>82.8</b></td><td><b>74.8</b></td></tr><tr><td>A<sub>ion</sub></td><td>5.6</td><td>4.0</td><td>4.8</td><td>3.8</td><td>2.9</td><td>2.7</td><td>2.4</td><td>1.7</td></tr><tr><td></td><td><b>1.9</b></td><td><b>1.8</b></td><td><b>1.7</b></td><td><b>1.5</b></td><td><b>1.4</b></td><td><b>1.3</b></td><td><b>1.2</b></td><td><b>1.2</b></td></tr><tr><td>B<sub>v</sub><sup>DCF</sup>(S<sub>v</sub>) [µG]</td><td>3.9 ± 1.5</td><td>1.7 ± 0.9</td><td>3.6 ± 2.3</td><td>3.2 ± 1.8</td><td>3.9 ± 2.8</td><td>1.2 ± 0.7</td><td>1.1 ± 0.4</td><td>0.4 ± 0.2</td></tr><tr><td></td><td><b>1.7 ± 0.7</b></td><td><b>0.9 ± 0.5</b></td><td><b>1.5 ± 1.0</b></td><td><b>1.4 ± 0.8</b></td><td><b>2.0 ± 1.4</b></td><td><b>0.6 ± 0.4</b></td><td><b>0.5 ± 0.2</b></td><td><b>0.2 ± 0.1</b></td></tr><tr><td>B<sub>sky</sub><sup>DCF</sup>(σ<sub>v</sub>) [µG]</td><td>10.1 ± 4.2</td><td>6.8 ± 3.7</td><td>12.7 ± 6.1</td><td>9.2 ± 6.5</td><td>10.9 ± 8.4</td><td>3.2 ± 1.6</td><td>3.3 ± 1.2</td><td>1.2 ± 0.4</td></tr><tr><td></td><td><b>4.3 ± 1.8</b></td><td><b>3.5 ± 1.9</b></td><td><b>5.4 ± 2.6</b></td><td><b>3.9 ± 2.8</b></td><td><b>5.6 ± 4.3</b></td><td><b>1.6 ± 0.8</b></td><td><b>1.6 ± 0.6</b></td><td><b>0.8 ± 0.2</b></td></tr><tr><td>B<sub>sky</sub><sup>ST</sup>(S<sub>v</sub>) [µG]</td><td>3.2 ± 1.2</td><td>1.4 ± 0.7</td><td>2.1 ± 1.4</td><td>1.9 ± 0.7</td><td>1.9 ± 0.9</td><td>1.1 ± 0.5</td><td>1.2 ± 0.4</td><td>0.4 ± 0.2</td></tr><tr><td></td><td><b>1.3 ± 0.5</b></td><td><b>0.7 ± 0.4</b></td><td><b>0.9 ± 0.6</b></td><td><b>0.8 ± 0.3</b></td><td><b>0.9 ± 0.5</b></td><td><b>0.5 ± 0.2</b></td><td><b>0.6 ± 0.2</b></td><td><b>0.3 ± 0.1</b></td></tr><tr><td>B<sub>sky</sub><sup>ST</sup>(σ<sub>v</sub>) [µG]</td><td>8.6 ± 2.8</td><td>5.8 ± 2.7</td><td>7.6 ± 3.3</td><td>5.4 ± 2.6</td><td>5.1 ± 2.4</td><td>3.0 ± 0.9</td><td>3.5 ± 0.9</td><td>1.5 ± 0.3</td></tr><tr><td></td><td><b>3.6 ± 1.2</b></td><td><b>3.0 ± 1.4</b></td><td><b>3.2 ± 1.4</b></td><td><b>2.3 ± 1.1</b></td><td><b>2.6 ± 1.2</b></td><td><b>1.5 ± 0.5</b></td><td><b>1.7 ± 0.4</b></td><td><b>0.9 ± 0.2</b></td></tr><tr><td>Γ<sub>in,S16</sub> [10<sup>-9</sup> s<sup>-1</sup>]</td><td>6.4</td><td>6.1</td><td>6.3</td><td>6.1</td><td>5.9</td><td>5.9</td><td>5.9</td><td>6.0</td></tr><tr><td></td><td><b>6.0</b></td><td><b>6.0</b></td><td><b>6.0</b></td><td><b>6.0</b></td><td><b>6.1</b></td><td><b>6.1</b></td><td><b>6.1</b></td><td><b>6.2</b></td></tr><tr><td>κ<sub>v</sub> [10<sup>28</sup> cm<sup>2</sup> s<sup>-1</sup>]</td><td>6.9 ± 1.2</td><td>5.3 ± 0.6</td><td>6.2 ± 1.5</td><td>5.2 ± 1.3</td><td>4.4 ± 0.4</td><td>4.2 ± 0.3</td><td>4.0 ± 0.3</td><td>3.5 ± 0.07</td></tr><tr><td></td><td><b>3.7 ± 0.2</b></td><td><b>3.6 ± 0.1</b></td><td><b>3.6 ± 0.2</b></td><td><b>3.4 ± 0.3</b></td><td><b>3.4 ± 0.08</b></td><td><b>3.4 ± 0.04</b></td><td><b>3.4 ± 0.1</b></td><td><b>3.4 ± 0.02</b></td></tr><tr><td>M<sub>A</sub><sup>DCF</sup></td><td>0.99 ± 0.31</td><td>1.21 ± 0.54</td><td>0.53 ± 0.22</td><td>0.74 ± 0.45</td><td>0.58 ± 0.46</td><td>1.42 ± 0.56</td><td>1.76 ± 0.53</td><td>2.12 ± 0.47</td></tr><tr><td>M<sub>A</sub><sup>S T</sup></td><td>1.17 ± 0.17</td><td>1.28 ± 0.27</td><td>0.85 ± 0.17</td><td>0.97 ± 0.31</td><td>0.85 ± 0.32</td><td>1.39 ± 0.28</td><td>1.56 ± 0.25</td><td>1.72 ± 0.2</td></tr><tr><td>M<sub>S</sub>(S<sub>v</sub>)</td><td>1.35 ± 0.49</td><td>0.72 ± 0.37</td><td>0.72 ± 0.63</td><td>0.68 ± 0.22</td><td>0.6 ± 0.18</td><td>0.62 ± 0.26</td><td>0.84 ± 0.36</td><td>0.29 ± 0.11</td></tr><tr><td></td><td><b>0.67 ± 0.28</b></td><td><b>0.39 ± 0.21</b></td><td><b>0.31 ± 0.24</b></td><td><b>0.27 ± 0.1</b></td><td><b>0.27 ± 0.09</b></td><td><b>0.25 ± 0.1</b></td><td><b>0.3 ± 0.14</b></td><td><b>0.15 ± 0.05</b></td></tr><tr><td>M<sub>S</sub>(σ<sub>v</sub>)</td><td>3.83 ± 1.01</td><td>2.93 ± 1.3</td><td>2.57 ± 1.49</td><td>1.96 ± 0.48</td><td>1.63 ± 0.3</td><td>1.77 ± 0.33</td><td>2.39 ± 0.58</td><td>1.09 ± 0.22</td></tr><tr><td></td><td><b>1.92 ± 0.63</b></td><td><b>1.6 ± 0.77</b></td><td><b>1.14 ± 0.58</b></td><td><b>0.82 ± 0.34</b></td><td><b>0.74 ± 0.18</b></td><td><b>0.74 ± 0.17</b></td><td><b>0.86 ± 0.22</b></td><td><b>0.54 ± 0.11</b></td></tr></tbody></table>
<table><caption>**Table B.1.** ISM properties along the Reticulum filament, for the fiber (regular font) or shell (bold font) geometry. The values and errors respectively give the mean value in each ~5 pc-wide square and the rms dispersion at 0.5–0.7 pc scale within each square. The Galactic coordinates refer to the square centre.</caption><tbody><tr><td>long. [deg]</td><td>282.09</td><td>281.58</td><td>280.05</td><td>277.51</td><td>276.15</td><td>272.59</td><td>269.88</td><td>268.18</td></tr><tr><td>lat. [deg]</td><td>-41.25</td><td>-42.0</td><td>-43.88</td><td>-46.25</td><td>-47.38</td><td>-49.12</td><td>-50.88</td><td>-51.5</td></tr><tr><td>N<sub>HI</sub> [10<sup>20</sup> cm<sup>-2</sup>]</td><td>4.4</td><td>3.8</td><td>3.4</td><td>2.5</td><td>2.2</td><td>1.9</td><td>1.4</td><td>1.4</td></tr><tr><td>LOS depth [pc]</td><td>3.6 ± 0.5</td><td>5.4 ± 0.7</td><td>3.6 ± 0.4</td><td>3.7 ± 0.5</td><td>5.2 ± 0.6</td><td>5.0 ± 0.6</td><td>4.4 ± 0.6</td><td>7.9 ± 1.0</td></tr><tr><td></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td><td><b>20.0 ± 2.5</b></td></tr><tr><td>n<sub>HI</sub> [cm<sup>-3</sup>]</td><td>39 ± 11</td><td>23 ± 6</td><td>31 ± 14</td><td>22 ± 13</td><td>14 ± 3</td><td>12 ± 3</td><td>10 ± 3</td><td>6 ± 1</td></tr><tr><td></td><td><b>7 ± 2</b></td><td><b>6 ± 2</b></td><td><b>6 ± 3</b></td><td><b>4 ± 2</b></td><td><b>4 ± 1</b></td><td><b>3 ± 0.8</b></td><td><b>2 ± 0.5</b></td><td><b>2 ± 0.4</b></td></tr><tr><td>S<sub>v</sub> [km s<sup>-1</sup>]</td><td>0.78</td><td>0.48</td><td>0.48</td><td>0.52</td><td>0.49</td><td>0.55</td><td>0.81</td><td>0.37</td></tr><tr><td>σ<sub>v</sub> [km s<sup>-1</sup>]</td><td>2.2</td><td>1.9</td><td>1.7</td><td>1.4</td><td>1.3</td><td>1.5</td><td>2.3</td><td>1.4</td></tr><tr><td>S<sub>ψ</sub> [deg]</td><td>19.95</td><td>24.44</td><td>10.73</td><td>14.9</td><td>11.8</td><td>28.74</td><td>35.62</td><td>42.91</td></tr><tr><td>T [K]</td><td>106</td><td>143</td><td>130</td><td>194</td><td>220</td><td>238</td><td>290</td><td>502</td></tr><tr><td></td><td><b>503</b></td><td><b>517</b></td><td><b>843</b></td><td><b>1581</b></td><td><b>1193</b></td><td><b>1457</b></td><td><b>2322</b></td><td><b>2044</b></td></tr><tr><td>x<sub>ion</sub> [10<sup>-4</sup>]</td><td>4.2</td><td>6.3</td><td>5.6</td><td>8.9</td><td>10.5</td><td>11.5</td><td>14.2</td><td>24.3</td></tr><tr><td></td><td><b>23.2</b></td><td><b>24.6</b></td><td><b>35.3</b></td><td><b>59.2</b></td><td><b>48.4</b></td><td><b>56.9</b></td><td><b>82.8</b></td><td><b>74.8</b></td></tr><tr><td>A<sub>ion</sub></td><td>5.6</td><td>4.0</td><td>4.8</td><td>3.8</td><td>2.9</td><td>2.7</td><td>2.4</td><td>1.7</td></tr><tr><td></td><td><b>1.9</b></td><td><b>1.8</b></td><td><b>1.7</b></td><td><b>1.5</b></td><td><b>1.4</b></td><td><b>1.3</b></td><td><b>1.2</b></td><td><b>1.2</b></td></tr><tr><td>B<sub>v</sub><sup>DCF</sup>(S<sub>v</sub>) [µG]</td><td>3.9 ± 1.5</td><td>1.7 ± 0.9</td><td>3.6 ± 2.3</td><td>3.2 ± 1.8</td><td>3.9 ± 2.8</td><td>1.2 ± 0.7</td><td>1.1 ± 0.4</td><td>0.4 ± 0.2</td></tr><tr><td></td><td><b>1.7 ± 0.7</b></td><td><b>0.9 ± 0.5</b></td><td><b>1.5 ± 1.0</b></td><td><b>1.4 ± 0.8</b></td><td><b>2.0 ± 1.4</b></td><td><b>0.6 ± 0.4</b></td><td><b>0.5 ± 0.2</b></td><td><b>0.2 ± 0.1</b></td></tr><tr><td>B<sub>sky</sub><sup>DCF</sup>(σ<sub>v</sub>) [µG]</td><td>10.1 ± 4.2</td><td>6.8 ± 3.7</td><td>12.7 ± 6.1</td><td>9.2 ± 6.5</td><td>10.9 ± 8.4</td><td>3.2 ± 1.6</td><td>3.3 ± 1.2</td><td>1.2 ± 0.4</td></tr><tr><td></td><td><b>4.3 ± 1.8</b></td><td><b>3.5 ± 1.9</b></td><td><b>5.4 ± 2.6</b></td><td><b>3.9 ± 2.8</b></td><td><b>5.6 ± 4.3</b></td><td><b>1.6 ± 0.8</b></td><td><b>1.6 ± 0.6</b></td><td><b>0.8 ± 0.2</b></td></tr><tr><td>B<sub>sky</sub><sup>ST</sup>(S<sub>v</sub>) [µG]</td><td>3.2 ± 1.2</td><td>1.4 ± 0.7</td><td>2.1 ± 1.4</td><td>1.9 ± 0.7</td><td>1.9 ± 0.9</td><td>1.1 ± 0.5</td><td>1.2 ± 0.4</td><td>0.4 ± 0.2</td></tr><tr><td></td><td><b>1.3 ± 0.5</b></td><td><b>0.7 ± 0.4</b></td><td><b>0.9 ± 0.6</b></td><td><b>0.8 ± 0.3</b></td><td><b>0.9 ± 0.5</b></td><td><b>0.5 ± 0.2</b></td><td><b>0.6 ± 0.2</b></td><td><b>0.3 ± 0.1</b></td></tr><tr><td>B<sub>sky</sub><sup>ST</sup>(σ<sub>v</sub>) [µG]</td><td>8.6 ± 2.8</td><td>5.8 ± 2.7</td><td>7.6 ± 3.3</td><td>5.4 ± 2.6</td><td>5.1 ± 2.4</td><td>3.0 ± 0.9</td><td>3.5 ± 0.9</td><td>1.5 ± 0.3</td></tr><tr><td></td><td><b>3.6 ± 1.2</b></td><td><b>3.0 ± 1.4</b></td><td><b>3.2 ± 1.4</b></td><td><b>2.3 ± 1.1</b></td><td><b>2.6 ± 1.2</b></td><td><b>1.5 ± 0.5</b></td><td><b>1.7 ± 0.4</b></td><td><b>0.9 ± 0.2</b></td></tr><tr><td>Γ<sub>in,S16</sub> [10<sup>-9</sup> s<sup>-1</sup>]</td><td>6.4</td><td>6.1</td><td>6.3</td><td>6.1</td><td>5.9</td><td>5.9</td><td>5.9</td><td>6.0</td></tr><tr><td></td><td><b>6.0</b></td><td><b>6.0</b></td><td><b>6.0</b></td><td><b>6.0</b></td><td><b>6.1</b></td><td><b>6.1</b></td><td><b>6.1</b></td><td><b>6.2</b></td></tr><tr><td>κ<sub>v</sub> [10<sup>28</sup> cm<sup>2</sup> s<sup>-1</sup>]</td><td>6.9 ± 1.2</td><td>5.3 ± 0.6</td><td>6.2 ± 1.5</td><td>5.2 ± 1.3</td><td>4.4 ± 0.4</td><td>4.2 ± 0.3</td><td>4.0 ± 0.3</td><td>3.5 ± 0.07</td></tr><tr><td></td><td><b>3.7 ± 0.2</b></td><td><b>3.6 ± 0.1</b></td><td><b>3.6 ± 0.2</b></td><td><b>3.4 ± 0.3</b></td><td><b>3.4 ± 0.08</b></td><td><b>3.4 ± 0.04</b></td><td><b>3.4 ± 0.1</b></td><td><b>3.4 ± 0.02</b></td></tr><tr><td>M<sub>A</sub><sup>DCF</sup></td><td>0.99 ± 0.31</td><td>1.21 ± 0.54</td><td>0.53 ± 0.22</td><td>0.74 ± 0.45</td><td>0.58 ± 0.46</td><td>1.42 ± 0.56</td><td>1.76 ± 0.53</td><td>2.12 ± 0.47</td></tr><tr><td>M<sub>A</sub><sup>S T</sup></td><td>1.17 ± 0.17</td><td>1.28 ± 0.27</td><td>0.85 ± 0.17</td><td>0.97 ± 0.31</td><td>0.85 ± 0.32</td><td>1.39 ± 0.28</td><td>1.56 ± 0.25</td><td>1.72 ± 0.2</td></tr><tr><td>M<sub>S</sub>(S<sub>v</sub>)</td><td>1.35 ± 0.49</td><td>0.72 ± 0.37</td><td>0.72 ± 0.63</td><td>0.68 ± 0.22</td><td>0.6 ± 0.18</td><td>0.62 ± 0.26</td><td>0.84 ± 0.36</td><td>0.29 ± 0.11</td></tr><tr><td></td><td><b>0.67 ± 0.28</b></td><td><b>0.39 ± 0.21</b></td><td><b>0.31 ± 0.24</b></td><td><b>0.27 ± 0.1</b></td><td><b>0.27 ± 0.09</b></td><td><b>0.25 ± 0.1</b></td><td><b>0.3 ± 0.14</b></td><td><b>0.15 ± 0.05</b></td></tr><tr><td>M<sub>S</sub>(σ<sub>v</sub>)</td><td>3.83 ± 1.01</td><td>2.93 ± 1.3</td><td>2.57 ± 1.49</td><td>1.96 ± 0.48</td><td>1.63 ± 0.3</td><td>1.77 ± 0.33</td><td>2.39 ± 0.58</td><td>1.09 ± 0.22</td></tr><tr><td></td><td><b>1.92 ± 0.63</b></td><td><b>1.6 ± 0.77</b></td><td><b>1.14 ± 0.58</b></td><td><b>0.82 ± 0.34</b></td><td><b>0.74 ± 0.18</b></td><td><b>0.74 ± 0.17</b></td><td><b>0.86 ± 0.22</b></td><td><b>0.54 ± 0.11</b></td></tr></tbody></table>
<table><caption>**Table B.2.** ISM properties along the Eridu filament, for the fiber (regular font) or shell (bold font) geometry. The values and errors respectively give the mean value in each ~5 pc-wide square and the rms dispersion at 0.5–0.7 pc scale within each square. The Galactic coordinates refer to the square centre.</caption><tbody><tr><td>long. [deg]</td><td>194.05</td><td>196.73</td><td>199.49</td><td>203.1</td><td>205.33</td><td>206.79</td><td>224.21</td></tr><tr><td>lat. [deg]</td><td>-56.77</td><td>-57.76</td><td>-59.73</td><td>-61.29</td><td>-62.52</td><td>-64.22</td><td>-62.46</td></tr><tr><td>N<sub>HI</sub> [10<sup>20</sup> cm<sup>-2</sup>]</td><td>2.0</td><td>1.8</td><td>1.7</td><td>2.6</td><td>1.9</td><td>2.0</td><td>0.9</td></tr><tr><td>LOS depth [pc]</td><td>8.1 ± 0.8</td><td>8.4 ± 0.8</td><td>11.4 ± 1.1</td><td>8.8 ± 0.9</td><td>16.1 ± 1.6</td><td>9.2 ± 0.9</td><td>6.7 ± 0.7</td></tr><tr><td></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td></tr><tr><td>n<sub>HI</sub> [cm<sup>-3</sup>]</td><td>9 ± 4</td><td>7 ± 2</td><td>5 ± 2</td><td>10 ± 1.7</td><td>5 ± 1</td><td>7 ± 1</td><td>5 ± 1</td></tr><tr><td></td><td><b>2 ± 0.8</b></td><td><b>2 ± 0.5</b></td><td><b>2 ± 0.7</b></td><td><b>3 ± 0.5</b></td><td><b>2 ± 0.6</b></td><td><b>2 ± 0.2</b></td><td><b>1 ± 0.2</b></td></tr><tr><td>S<sub>v</sub> [km s<sup>-1</sup>]</td><td>1.11</td><td>1.49</td><td>1.27</td><td>1.0</td><td>1.01</td><td>1.7</td><td>0.47</td></tr><tr><td>σ<sub>v</sub> [km s<sup>-1</sup>]</td><td>3.2</td><td>3.3</td><td>3.7</td><td>3.0</td><td>2.8</td><td>3.3</td><td>3.4</td></tr><tr><td>S<sub>ψ</sub> [deg]</td><td>11.62</td><td>14.32</td><td>18.15</td><td>9.41</td><td>15.05</td><td>19.01</td><td></td></tr><tr><td>T [K]</td><td>488</td><td>440</td><td>789</td><td>295</td><td>1102</td><td>408</td><td>845</td></tr><tr><td></td><td><b>2847</b></td><td><b>2867</b></td><td><b>3202</b></td><td><b>1592</b></td><td><b>2673</b></td><td><b>2317</b></td><td><b>5868</b></td></tr><tr><td>x<sub>ion</sub> [10<sup>-4</sup>]</td><td>22.2</td><td>21.4</td><td>34.6</td><td>14.6</td><td>45.3</td><td>20.1</td><td>36.9</td></tr><tr><td></td><td><b>101.2</b></td><td><b>98.2</b></td><td><b>108.9</b></td><td><b>61.4</b></td><td><b>94.4</b></td><td><b>82.7</b></td><td><b>200.4</b></td></tr><tr><td>A<sub>ion</sub></td><td>2.0</td><td>1.9</td><td>1.6</td><td>2.3</td><td>1.5</td><td>1.9</td><td>1.5</td></tr><tr><td></td><td><b>1.2</b></td><td><b>1.2</b></td><td><b>1.2</b></td><td><b>1.3</b></td><td><b>1.2</b></td><td><b>1.2</b></td><td><b>1.1</b></td></tr><tr><td>B<sub>Sky</sub><sup>DCF</sup>(S<sub>v</sub>) [µG]</td><td>4.6 ± 2.8</td><td>4.9 ± 2.3</td><td>4.6 ± 5.4</td><td>6.4 ± 4.0</td><td>2.2 ± 0.8</td><td>4.1 ± 1.6</td><td></td></tr><tr><td></td><td><b>2.4 ± 1.5</b></td><td><b>2.6 ± 1.2</b></td><td><b>2.9 ± 3.3</b></td><td><b>3.4 ± 2.2</b></td><td><b>1.6 ± 0.6</b></td><td><b>2.3 ± 0.9</b></td><td></td></tr><tr><td>B<sub>Sky</sub><sup>DCF</sup>(σ<sub>v</sub>) [µG]</td><td>10.7 ± 4.6</td><td>9.0 ± 4.6</td><td>9.1 ± 5.5</td><td>15.4 ± 8.6</td><td>5.9 ± 2.2</td><td>7.1 ± 3.3</td><td></td></tr><tr><td></td><td><b>5.3 ± 2.3</b></td><td><b>4.8 ± 2.5</b></td><td><b>5.6 ± 3.4</b></td><td><b>8.4 ± 4.7</b></td><td><b>3.9 ± 1.5</b></td><td><b>4.0 ± 1.8</b></td><td></td></tr><tr><td>B<sub>Sky</sub><sup>ST</sup>(S<sub>v</sub>) [µG]</td><td>2.8 ± 1.5</td><td>3.2 ± 1.1</td><td>2.5 ± 2.0</td><td>3.1 ± 1.2</td><td>1.5 ± 0.4</td><td>3.1 ± 0.7</td><td></td></tr><tr><td></td><td><b>1.4 ± 0.8</b></td><td><b>1.7 ± 0.6</b></td><td><b>1.6 ± 1.2</b></td><td><b>1.7 ± 0.6</b></td><td><b>1.1 ± 0.3</b></td><td><b>1.7 ± 0.4</b></td><td></td></tr><tr><td>B<sub>Sky</sub><sup>ST</sup>(σ<sub>v</sub>) [µG]</td><td>7.3 ± 2.6</td><td>6.3 ± 2.4</td><td>6.0 ± 2.2</td><td>8.5 ± 2.5</td><td>4.4 ± 1.1</td><td>5.7 ± 1.5</td><td></td></tr><tr><td></td><td><b>3.6 ± 1.3</b></td><td><b>3.4 ± 1.3</b></td><td><b>3.7 ± 1.3</b></td><td><b>4.6 ± 1.4</b></td><td><b>2.9 ± 0.8</b></td><td><b>3.2 ± 0.8</b></td><td></td></tr><tr><td>Γ<sub>In,S16</sub> [10<sup>-9</sup> s<sup>-1</sup>]</td><td>6.0</td><td>5.9</td><td>6.0</td><td>5.9</td><td>6.1</td><td>5.9</td><td>6.1</td></tr><tr><td></td><td><b>5.9</b></td><td><b>6.0</b></td><td><b>5.9</b></td><td><b>6.2</b></td><td><b>6.0</b></td><td><b>6.2</b></td><td><b>4.9</b></td></tr><tr><td>K<sub>ll</sub> [10<sup>28</sup> cm<sup>2</sup> s<sup>-1</sup>]</td><td>3.7 ± 0.3</td><td>3.6 ± 0.3</td><td>3.5 ± 0.1</td><td>3.9 ± 0.2</td><td>3.4 ± 0.08</td><td>3.6 ± 0.07</td><td>3.4 ± 0.05</td></tr><tr><td></td><td><b>3.3 ± 0.4</b></td><td><b>3.3 ± 0.3</b></td><td><b>3.3 ± 0.2</b></td><td><b>3.4 ± 0.03</b></td><td><b>3.3 ± 0.3</b></td><td><b>3.4 ± 0.06</b></td><td><b>2.7 ± 0.4</b></td></tr><tr><td>M<sub>A</sub><sup>DCF</sup></td><td>0.57 ± 0.19</td><td>0.71 ± 0.38</td><td>0.9 ± 0.7</td><td>0.46 ± 0.2</td><td>0.74 ± 0.25</td><td>0.94 ± 0.37</td><td></td></tr><tr><td>M<sub>A</sub><sup>ST</sup></td><td>0.89 ± 0.14</td><td>0.97 ± 0.25</td><td>1.05 ± 0.4</td><td>0.79 ± 0.18</td><td>1.01 ± 0.17</td><td>1.13 ± 0.22</td><td></td></tr><tr><td>M<sub>S</sub> (S<sub>v</sub>)</td><td>1.02 ± 0.53</td><td>1.3 ± 0.51</td><td>0.88 ± 0.5</td><td>1.03 ± 0.27</td><td>0.57 ± 0.14</td><td>1.48 ± 0.33</td><td>0.85 ± 0.16</td></tr><tr><td></td><td><b>0.41 ± 0.23</b></td><td><b>0.52 ± 0.23</b></td><td><b>0.44 ± 0.26</b></td><td><b>0.45 ± 0.12</b></td><td><b>0.36 ± 0.08</b></td><td><b>0.62 ± 0.14</b></td><td><b>0.31 ± 0.03</b></td></tr><tr><td>M<sub>S</sub> (σ<sub>v</sub>)</td><td>2.93 ± 1.02</td><td>2.85 ± 0.97</td><td>2.47 ± 0.69</td><td>3.05 ± 0.54</td><td>1.64 ± 0.42</td><td>2.89 ± 0.6</td><td>1.7 ± 0.31</td></tr><tr><td></td><td><b>1.18 ± 0.42</b></td><td><b>1.14 ± 0.42</b></td><td><b>1.22 ± 0.37</b></td><td><b>1.34 ± 0.27</b></td><td><b>1.02 ± 0.25</b></td><td><b>1.21 ± 0.25</b></td><td><b>0.61 ± 0.06</b></td></tr></tbody></table>
<table><caption>**Table B.2.** ISM properties along the Eridu filament, for the fiber (regular font) or shell (bold font) geometry. The values and errors respectively give the mean value in each ~5 pc-wide square and the rms dispersion at 0.5–0.7 pc scale within each square. The Galactic coordinates refer to the square centre.</caption><tbody><tr><td>long. [deg]</td><td>194.05</td><td>196.73</td><td>199.49</td><td>203.1</td><td>205.33</td><td>206.79</td><td>224.21</td></tr><tr><td>lat. [deg]</td><td>-56.77</td><td>-57.76</td><td>-59.73</td><td>-61.29</td><td>-62.52</td><td>-64.22</td><td>-62.46</td></tr><tr><td>N<sub>HI</sub> [10<sup>20</sup> cm<sup>-2</sup>]</td><td>2.0</td><td>1.8</td><td>1.7</td><td>2.6</td><td>1.9</td><td>2.0</td><td>0.9</td></tr><tr><td>LOS depth [pc]</td><td>8.1 ± 0.8</td><td>8.4 ± 0.8</td><td>11.4 ± 1.1</td><td>8.8 ± 0.9</td><td>16.1 ± 1.6</td><td>9.2 ± 0.9</td><td>6.7 ± 0.7</td></tr><tr><td></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td><td><b>30.0 ± 3.0</b></td></tr><tr><td>n<sub>HI</sub> [cm<sup>-3</sup>]</td><td>9 ± 4</td><td>7 ± 2</td><td>5 ± 2</td><td>10 ± 1.7</td><td>5 ± 1</td><td>7 ± 1</td><td>5 ± 1</td></tr><tr><td></td><td><b>2 ± 0.8</b></td><td><b>2 ± 0.5</b></td><td><b>2 ± 0.7</b></td><td><b>3 ± 0.5</b></td><td><b>2 ± 0.6</b></td><td><b>2 ± 0.2</b></td><td><b>1 ± 0.2</b></td></tr><tr><td>S<sub>v</sub> [km s<sup>-1</sup>]</td><td>1.11</td><td>1.49</td><td>1.27</td><td>1.0</td><td>1.01</td><td>1.7</td><td>0.47</td></tr><tr><td>σ<sub>v</sub> [km s<sup>-1</sup>]</td><td>3.2</td><td>3.3</td><td>3.7</td><td>3.0</td><td>2.8</td><td>3.3</td><td>3.4</td></tr><tr><td>S<sub>ψ</sub> [deg]</td><td>11.62</td><td>14.32</td><td>18.15</td><td>9.41</td><td>15.05</td><td>19.01</td><td></td></tr><tr><td>T [K]</td><td>488</td><td>440</td><td>789</td><td>295</td><td>1102</td><td>408</td><td>845</td></tr><tr><td></td><td><b>2847</b></td><td><b>2867</b></td><td><b>3202</b></td><td><b>1592</b></td><td><b>2673</b></td><td><b>2317</b></td><td><b>5868</b></td></tr><tr><td>x<sub>ion</sub> [10<sup>-4</sup>]</td><td>22.2</td><td>21.4</td><td>34.6</td><td>14.6</td><td>45.3</td><td>20.1</td><td>36.9</td></tr><tr><td></td><td><b>101.2</b></td><td><b>98.2</b></td><td><b>108.9</b></td><td><b>61.4</b></td><td><b>94.4</b></td><td><b>82.7</b></td><td><b>200.4</b></td></tr><tr><td>A<sub>ion</sub></td><td>2.0</td><td>1.9</td><td>1.6</td><td>2.3</td><td>1.5</td><td>1.9</td><td>1.5</td></tr><tr><td></td><td><b>1.2</b></td><td><b>1.2</b></td><td><b>1.2</b></td><td><b>1.3</b></td><td><b>1.2</b></td><td><b>1.2</b></td><td><b>1.1</b></td></tr><tr><td>B<sub>Sky</sub><sup>DCF</sup>(S<sub>v</sub>) [µG]</td><td>4.6 ± 2.8</td><td>4.9 ± 2.3</td><td>4.6 ± 5.4</td><td>6.4 ± 4.0</td><td>2.2 ± 0.8</td><td>4.1 ± 1.6</td><td></td></tr><tr><td></td><td><b>2.4 ± 1.5</b></td><td><b>2.6 ± 1.2</b></td><td><b>2.9 ± 3.3</b></td><td><b>3.4 ± 2.2</b></td><td><b>1.6 ± 0.6</b></td><td><b>2.3 ± 0.9</b></td><td></td></tr><tr><td>B<sub>Sky</sub><sup>DCF</sup>(σ<sub>v</sub>) [µG]</td><td>10.7 ± 4.6</td><td>9.0 ± 4.6</td><td>9.1 ± 5.5</td><td>15.4 ± 8.6</td><td>5.9 ± 2.2</td><td>7.1 ± 3.3</td><td></td></tr><tr><td></td><td><b>5.3 ± 2.3</b></td><td><b>4.8 ± 2.5</b></td><td><b>5.6 ± 3.4</b></td><td><b>8.4 ± 4.7</b></td><td><b>3.9 ± 1.5</b></td><td><b>4.0 ± 1.8</b></td><td></td></tr><tr><td>B<sub>Sky</sub><sup>ST</sup>(S<sub>v</sub>) [µG]</td><td>2.8 ± 1.5</td><td>3.2 ± 1.1</td><td>2.5 ± 2.0</td><td>3.1 ± 1.2</td><td>1.5 ± 0.4</td><td>3.1 ± 0.7</td><td></td></tr><tr><td></td><td><b>1.4 ± 0.8</b></td><td><b>1.7 ± 0.6</b></td><td><b>1.6 ± 1.2</b></td><td><b>1.7 ± 0.6</b></td><td><b>1.1 ± 0.3</b></td><td><b>1.7 ± 0.4</b></td><td></td></tr><tr><td>B<sub>Sky</sub><sup>ST</sup>(σ<sub>v</sub>) [µG]</td><td>7.3 ± 2.6</td><td>6.3 ± 2.4</td><td>6.0 ± 2.2</td><td>8.5 ± 2.5</td><td>4.4 ± 1.1</td><td>5.7 ± 1.5</td><td></td></tr><tr><td></td><td><b>3.6 ± 1.3</b></td><td><b>3.4 ± 1.3</b></td><td><b>3.7 ± 1.3</b></td><td><b>4.6 ± 1.4</b></td><td><b>2.9 ± 0.8</b></td><td><b>3.2 ± 0.8</b></td><td></td></tr><tr><td>Γ<sub>in,S16</sub> [10<sup>-9</sup> s<sup>-1</sup>]</td><td>6.0</td><td>5.9</td><td>6.0</td><td>5.9</td><td>6.1</td><td>5.9</td><td>6.1</td></tr><tr><td></td><td><b>5.9</b></td><td><b>6.0</b></td><td><b>5.9</b></td><td><b>6.2</b></td><td><b>6.0</b></td><td><b>6.2</b></td><td><b>4.9</b></td></tr><tr><td>κ<sub>ll</sub> [10<sup>28</sup> cm<sup>2</sup> s<sup>-1</sup>]</td><td>3.7 ± 0.3</td><td>3.6 ± 0.3</td><td>3.5 ± 0.1</td><td>3.9 ± 0.2</td><td>3.4 ± 0.08</td><td>3.6 ± 0.07</td><td>3.4 ± 0.05</td></tr><tr><td></td><td><b>3.3 ± 0.4</b></td><td><b>3.3 ± 0.3</b></td><td><b>3.3 ± 0.2</b></td><td><b>3.4 ± 0.03</b></td><td><b>3.3 ± 0.3</b></td><td><b>3.4 ± 0.06</b></td><td><b>2.7 ± 0.4</b></td></tr><tr><td>M<sub>A</sub><sup>DCF</sup></td><td>0.57 ± 0.19</td><td>0.71 ± 0.38</td><td>0.9 ± 0.7</td><td>0.46 ± 0.2</td><td>0.74 ± 0.25</td><td>0.94 ± 0.37</td><td></td></tr><tr><td>M<sub>A</sub><sup>ST</sup></td><td>0.89 ± 0.14</td><td>0.97 ± 0.25</td><td>1.05 ± 0.4</td><td>0.79 ± 0.18</td><td>1.01 ± 0.17</td><td>1.13 ± 0.22</td><td></td></tr><tr><td>M<sub>S</sub> (S<sub>v</sub>)</td><td>1.02 ± 0.53</td><td>1.3 ± 0.51</td><td>0.88 ± 0.5</td><td>1.03 ± 0.27</td><td>0.57 ± 0.14</td><td>1.48 ± 0.33</td><td>0.85 ± 0.16</td></tr><tr><td></td><td><b>0.41 ± 0.23</b></td><td><b>0.52 ± 0.23</b></td><td><b>0.44 ± 0.26</b></td><td><b>0.45 ± 0.12</b></td><td><b>0.36 ± 0.08</b></td><td><b>0.62 ± 0.14</b></td><td><b>0.31 ± 0.03</b></td></tr><tr><td>M<sub>S</sub> (σ<sub>v</sub>)</td><td>2.93 ± 1.02</td><td>2.85 ± 0.97</td><td>2.47 ± 0.69</td><td>3.05 ± 0.54</td><td>1.64 ± 0.42</td><td>2.89 ± 0.6</td><td>1.7 ± 0.31</td></tr><tr><td></td><td><b>1.18 ± 0.42</b></td><td><b>1.14 ± 0.42</b></td><td><b>1.22 ± 0.37</b></td><td><b>1.34 ± 0.27</b></td><td><b>1.02 ± 0.25</b></td><td><b>1.21 ± 0.25</b></td><td><b>0.61 ± 0.06</b></td></tr></tbody></table>