### C.2. Error of $i = \arccos z$

Let us now calculate an approximation to the expected value and standard deviation of the inclination

$$i = \arccos z, \qquad (C18)$$

given the expected value, $\mu_z$, and standard deviation, $\sigma_z$, of $z$.

#### C.2.1. Expected value of $i = \arccos z$

The expected value $E[i]$ is

$$\mu_i \equiv E[i] = \int_{-\infty}^{+\infty} \arccos z \frac{1}{\sqrt{2\pi} \sigma_z} \exp \left[ -\frac{1}{2} \left( \frac{z - \mu_z}{\sigma_z} \right)^2 \right] dz. \quad (C19)$$

The expansion of arccos around the expected value $\mu_z$, using as before the standard normally distributed variable $\epsilon = (z - \mu_z)/\sigma_z$, is

$$\arccos z \approx \arccos \mu_z - \frac{\sigma_z}{\sqrt{1 - \mu_z^2}} \epsilon - \frac{1}{2!} \frac{\mu_z \sigma_z^2}{(1 - \mu_z^2)^{3/2}} \epsilon^2 + \dots \quad (C20)$$

The integral is not null for the even terms of the expansion only, and thus the approximation is correct up to order three. The result of the integration is

$$E[i] \approx \arccos \mu_z - \frac{1}{2} \frac{\mu_z \sigma_z^2}{(1 - \mu_z^2)^{3/2}}. \quad (C21)$$

It is noticeable that there is a bias in the expected value of the inclination, because $E[\arccos z] \neq \arccos(E[z])$.

#### C.2.2. Standard Deviation of $i = \arccos z$

In a similar way, let us calculate $E[i^2]$,

$$E[i^2] = \int_{-\infty}^{+\infty} \arccos^2 z \frac{1}{\sqrt{2\pi} \sigma_z} \times \exp \left[ -\frac{1}{2} \left( \frac{z - \mu_z}{\sigma_z} \right)^2 \right] dz. \quad (C22)$$

The expansion of $\arccos^2$ is

$$\arccos^2 z \approx \arccos^2 \mu_z - 2 \frac{\sigma_z \arccos \mu_z}{\sqrt{1 - \mu_z^2}} \epsilon - \frac{\sigma_z^2}{1 - \mu_z^2} \left( \frac{\mu_z \arccos \mu_z}{\sqrt{1 - \mu_z^2}} - 1 \right) \epsilon^2 + \dots \quad (C23)$$

The integration gives nonzero values for the even terms, resulting in

$$E[i^2] \approx \arccos^2 \mu_z - \frac{\sigma_z^2}{1 - \mu_z^2} \left( \frac{\mu_z \arccos \mu_z}{\sqrt{1 - \mu_z^2}} - 1 \right). \quad (C24)$$

The square of $E[i]$, discarding terms of fourth order, is

$$E^2[i] \approx \arccos^2 \mu_z - \frac{\sigma_z^2}{1 - \mu_z^2} \frac{\mu_z \arccos \mu_z}{\sqrt{1 - \mu_z^2}}. \quad (C25)$$

The difference gives us the variance $\sigma_i^2 = E[i^2] - E^2[i]$, resulting in a standard deviation that is simply

$$\sigma_i \approx \frac{\sigma_z}{\sqrt{1 - \mu_z^2}}. \quad (C26)$$

### C.3. Error of $i = \arctan z$

Let us now calculate an approximation to the expected value and standard deviation of the inclination

$$i = \arctan z, \quad (C27)$$

given the expected value, $\mu_z$, and standard deviation, $\sigma_z$, of $z$. The procedure is the same as that used in the former section.

#### C.3.1. Expected value of $i = \arctan z$

The expansion of arctan around the expected value $\mu_z$, using the standard normally distributed variable $\epsilon = (z - \mu_z)/\sigma_z$, is

$$\arctan z \approx \arctan \mu_z + \frac{\sigma_z}{(1 + \mu_z^2)^2} \epsilon - \frac{\mu_z \sigma_z^2}{(1 + \mu_z^2)^2} \epsilon^2 + \dots \quad (C28)$$

The expected value of $i$, neglecting terms of order higher than three, is

$$E[i] \approx \arctan \mu_z - \frac{\mu_z \sigma_z^2}{(1 + \mu_z^2)^2}. \quad (C29)$$

Like in the former case, there is a bias in the expected value of the inclination, because $E[\arctan z] \neq \arctan(E[z])$.

#### C.3.2. Standard Deviation of $i = \arctan z$

To calculate $E[i^2]$, we need the expansion

$$\arctan^2 z \approx \arctan^2 \mu_z + 2 \frac{\sigma_z \arctan \mu_z}{1 + \mu_z^2} \epsilon + \frac{\sigma_z^2}{(1 + \mu_z^2)^2} (1 - 2\mu_z \arctan \mu_z) \epsilon^2 + \dots \quad (C30)$$

resulting in

$$E[i^2] \approx \arctan^2 \mu_z + \frac{\sigma_z^2}{(1 + \mu_z^2)^2} (1 - 2\mu_z \arctan \mu_z). \quad (C31)$$

The difference, $\sigma_i^2 = E[i^2] - E^2[i]$, neglecting terms of the fourth order, gives

$$\sigma_i \approx \frac{\sigma_z}{1 + \mu_z^2}. \quad (C32)$$
### C.4. Summary

Given two independent Gaussian random variables x and y, with expected values $\mu_x$ and $\mu_y$, and standard deviations $\sigma_x$ and $\sigma_y$, the expected value and the standard deviation of the ratio $z = x/y$ are

$$ 
\begin{aligned}
\mu_z &\approx \frac{\mu_x}{\mu_y} \left( 1 + \frac{\sigma_y^2}{\mu_y^2} \right), \\
\sigma_z &\approx \frac{\mu_x}{\mu_y} \sqrt{\frac{\sigma_x^2}{\mu_x^2} + \frac{\sigma_y^2}{\mu_y^2}}.
\end{aligned} 
\quad (C33) 
$$

Given the ratio of the minor and major axes, $a_{min}$ and $a_{maj}$, of the projection of the disk on the plane of the sky, $z = a_{min}/a_{maj}$, the expected value and the standard deviation of the disk inclination, $i = \arccos z$, are

$$ 
\begin{aligned}
\mu_i &\approx \arccos \mu_z - \frac{1}{2} \frac{\mu_z \sigma_z^2}{(1 - \mu_z^2)^{3/2}}, \\
\sigma_i &\approx \frac{\sigma_z}{\sqrt{1 - \mu_z^2}}.
\end{aligned} 
\quad (C34) 
$$

Given the ratio of the components of the orbital velocity along the line of sight and on the plane of the sky, $z = v_{los}/v_{sky}$, the expected value and the standard deviation of the orbit inclination, $i = \arctan z$, are

$$ 
\begin{aligned}
\mu_i &\approx \arctan \mu_z - \frac{\mu_z \sigma_z^2}{(1 + \mu_z^2)^2}, \\
\sigma_i &\approx \frac{\sigma_z}{1 + \mu_z^2}.
\end{aligned} 
\quad (C35) 
$$

## Appendix D
### Fitting of a Keplerian Thin Disk Model

We use the model of a thin disk with a Keplerian rotation developed by R. Estalella (see Appendix B in Zapata et al. 2019 and references therein for details) to constrain the properties of the VLA 4A source. The model consists of a geometrically thin disk with an inner radius $R_{inn}$ and an outer radius $R_{out}$, where the intensity and velocity are described by power laws of the radius with indices $-1$ and $-0.5$, respectively. The kinematics of the disk is computed by considering a cube composed of a grid of points in the plane of the disk, and for each point of the grid, a number of velocity channels. For each point of the grid, the projection of its rotation velocity onto the line of sight is calculated. A Gaussian line profile, of width $\Delta V$ (assumed constant for the whole disk), and proportional to the estimated intensity, is added to the channels associated with the grid point. After this first cube is computed, its projection onto the plane of the sky is estimated. So, the plane-of-the-sky cube has two coordinate axes in the plane of the sky, and a third, spectral axis. Finally, each channel of the plane-of-the-sky cube is convolved with a Gaussian with the size of the beam. The intensity depends on a

<table><thead><tr><th>Identifier</th><th>Transition</th><th>Frequency (GHz)</th></tr></thead><tbody><tr><td>EthyGly1</td><td>(34 04 31 1–33 04 30 0)</td><td>342.801</td></tr><tr><td>EthyGly2</td><td>(34 03 31 1–33 03 30 0)</td><td>342.851</td></tr><tr><td rowspan="2">EthyGly3</td><td>(33 11 23 1–32 11 22 0)</td><td>345.737<sup>a</sup></td></tr><tr><td>(33 11 22 1–33 11 21 0)</td><td>345.738<sup>a</sup></td></tr></tbody></table>

**Note.**

### Table D2
Positions and Reference Velocities

<table><thead><tr><th>Object</th><th>α(J2000)<br>(h:m:s)</th><th>δ(J2000)<br>(d:m:s)</th><th>V<sub>sys</sub><br>(km s<sup>-1</sup>)</th></tr></thead><tbody><tr><td>VLA 4A</td><td>03:29:03.7460</td><td>+31:16:03.769</td><td>7.36 ± 0.21</td></tr><tr><td>VLA 4B</td><td>03:29:03.7691</td><td>+31:16:03.761</td><td>9.33 ± 0.18</td></tr><tr><td>Ambient Cloud</td><td>...</td><td>...</td><td>8.5<sup>a</sup></td></tr></tbody></table>

**Note.**

scale factor, which is estimated by minimizing the sum of the squared differences between the data cube and the model cube. The parameter space is searched for the minimum of the rms fit residual for all the channel maps, using a pseudo-random sequence as described in Estalella et al. (2012), and Estalella (2017). Once a minimum of the rms fit residual is found, the uncertainty in the parameters fitted is found as described in Wall & Jenkins (2003) and Estalella (2017).

### D.1. VLA 4A Circumstellar Disk Traced by Ethylene Glycol

The ethylene glycol lines detected only toward VLA 4A (Table D1) were used to fit the rotation of a geometrically thin disk. The model was fitted to the spectral data, assuming as position of its center that of VLA 4A, and a reference velocity $V_{sys} = 7.36$ km s⁻¹ (see Table D2). The beam used to convolve the model intensity was that of the observation, $0''154 \times 0''079$ (PA = −1°.9). The free parameters of the model were the linewidth (without rotational broadening), $\Delta V$, the inclination of the disk, $i$, the inner and outer radii, $R_{inn}$ and $R_{out}$, and the rotation velocity at a reference radius of $1''$, times the sinus of the inclination, $V_0 \sin i$.

The results from the fit are given in Table D3, and the derived parameters, for a distance to SVS 13 of 300 pc, are given in Table D4.

Figure D1 shows a comparison of the zeroth-order and first-order moment maps of the EthyGly1 and EthyGly2 transitions with the thin-disk model. Figure D2 and D3 show a comparison of the observed and thin-disk model PV plots and channel maps, respectively.

The results obtained for the three lines are remarkably consistent. The linewidth of EthyGly3 is consistent with those

<footnote>a The frequency difference between the two transitions is 1.432 MHz (1.242 km s⁻¹), and both appear blended.</footnote>

<footnote>a Adopted (Section 3.4.1).</footnote>
<figure><img src="image_28.png" /><figcaption>**Figure D1.** VLA 4A circumstellar disk: first-order moment (intensity-weighted velocity in km s⁻¹; color scale) overlaid on the zeroth-order moment (integrated intensity; contours) of EthyGly1 (left), EthyGly2 (center), and the thin-disk model of EthyGly2 (right). For the three panels, contours range from 15% to 90% in steps of 15% of the peak (0.120, 0.168, and 0.150 Jy beam⁻¹ km s⁻¹ for EthyGly1, EthyGly2, and the model of EthyGly2, respectively). Offsets are relative to the position of VLA 4A (Table D2), in R.A. (x-axis) and decl. (y-axis), positive toward east and north respectively.</figcaption></figure>

<table><caption>**Table D3**
VLA 4A: Best Fit of a Geometrically Thin Disk with Keplerian Rotation</caption><thead><tr><th>Line</th><th>ΔV<br>(km s<sup>-1</sup>)</th><th><i>i</i><br>(deg)</th><th><i>R</i><sub>inn</sub><br>(arcsec)</th><th><i>R</i><sub>out</sub><br>(arcsec)</th><th><i>V</i><sub>0</sub> sin <i>i</i><sup>a</sup><br>(km s<sup>-1</sup>)</th></tr></thead><tbody><tr><td>EthyGly1</td><td>1.53 ± 0.18</td><td>22.6 ± 5.6</td><td>0.011 ± 0.003</td><td>0.109 ± 0.004</td><td>0.312 ± 0.018</td></tr><tr><td>EthyGly2</td><td>1.87 ± 0.22</td><td>21.8 ± 6.7</td><td>0.006 ± 0.003</td><td>0.112 ± 0.010</td><td>0.327 ± 0.019</td></tr><tr><td>EthyGly3</td><td>2.74 ± 0.13</td><td>22.3 ± 3.2</td><td>0.010 ± 0.003</td><td>0.110 ± 0.004</td><td>0.255 ± 0.017</td></tr></tbody></table>

**Note.**

<table><caption>**Table D4**
VLA 4A: Parameters Derived from the Best Fit to the Ethylene Glycol Lines</caption><thead><tr><th>Line</th><th><i>R</i><sub>inn</sub><br>(au)</th><th><i>R</i><sub>out</sub><br>(au)</th><th><i>V</i><sub>0</sub><sup>a</sup><br>(km s<sup>-1</sup>)</th><th><i>M</i><sub>*</sub><sup>b</sup><br>(M<sub>☉</sub>)</th></tr></thead><tbody><tr><td>EthyGly1</td><td>3.3 ± 0.9</td><td>32.8 ± 1.3</td><td>0.81 ± 0.20</td><td>0.22 ± 0.11</td></tr><tr><td>EthyGly2</td><td>1.9 ± 0.8</td><td>33.5 ± 2.9</td><td>0.88 ± 0.26</td><td>0.26 ± 0.16</td></tr><tr><td>EthyGly3</td><td>2.9 ± 0.9</td><td>33.1 ± 1.1</td><td>0.67 ± 0.10</td><td>0.15 ± 0.05</td></tr></tbody></table>

**Notes.**

of EthyGly1 and EthyGly2 if we take into account the separation of the two blended lines in EthyGly3 (see Table D1). In summary, the ethylene glycol data indicate the presence of a rotating disk around VLA 4A, with an inner radius of ~2 au, an outer radius of 33 au, an inclination of 22° (0° for a face-on disk), and a Keplerian rotation velocity with a value of 0.9 km s⁻¹ at a reference radius of 300 au, corresponding to 2.7 km s⁻¹ at r = 30 au, or 9 km s⁻¹ at 3 au. The Keplerian rotation implies a central mass of ~0.25 $M_{☉}$.

<footnote>a At a radius of 1".</footnote>

<footnote>a At a radius of 1" (300 au).</footnote>

<footnote>b Central mass.</footnote>
<figure><img src="image_29.png" /><figcaption>**Figure D2.** VLA 4A circumstellar disk: position-velocity cuts for EthyGly1 (top panels), EthyGly2 (middle panels), and the thin-disk model (bottom panels). The left panels show the cuts along the major axis (east-west), while the right panels show the perpendicular direction. Offsets are positive westward and northward, respectively. The model is for a central mass $M_* = 0.25 M_\odot$, $R_{\text{inn}} = 1.8$ au, and $R_{\text{out}} = 33.5$ au, with an inclination $i = 22^\circ$. Contours start at 10% of the peak of the EthyGly2 emission (peak = $0.047 \text{ Jy beam}^{-1}$), increasing in steps of 10%. The curves in the major axis cuts are the Keplerian rotation curves for central masses $M_* = 0.10, 0.25$, and $0.40 M_\odot$, which are plotted as a reference.</figcaption></figure>
<figure><img src="image_30.png" /></figure>

**Figure D3.** VLA 4A circumstellar disk: channel maps around the reference velocity of the source, $V_{sys} = 7.36$ km s$^{-1}$, of EthyGly2 (three leftmost columns) and the thin-disk model (three rightmost columns). Velocities range from 4.76 km s$^{-1}$ (top left corner) to 9.45 km s$^{-1}$ (bottom right corner), in steps of 0.43 km s$^{-1}$. Contours start at 10% of the peak (0.047 Jy beam$^{-1}$), increasing in steps of 13%. Offsets are relative to the position of VLA 4A (Table D2), in R.A. (x-axis) and decl. (y-axis), positive toward east and north respectively.

## Appendix E
### Fitting of an Optically Thin Spherical Infalling Envelope Model

#### E.1. Spherical Infalling Envelope Centered on VLA 4A Traced by CS (7–6)

The integrated CS (7–6) emission is shown in Figure 11 (left column panels). The PV cuts through the position of VLA 4A show higher velocities near its center, suggesting gravitational acceleration (Figure 16). The morphology of the PV cuts is quite similar for all the position angles (see Figures 16 and E1), suggesting that assuming spherical symmetry is an acceptable approximation. The excess emission at offsets ~−0.5 in the cuts at PA = −90° and −110° is at the position of VLA 4B, and is associated with its own envelope. We assume that this emission does not belong to the envelope around VLA 4A.

Thus, the CS emission seems to be tracing an infalling envelope. We compared the observed emission from that of a spherically symmetric envelope in infall, assuming that the line emission is optically thin (perhaps only for the wings of the line), with infall velocity and temperature proportional to $r^{-1/2}$ (characteristic of the main accretion phase of infall), with no rotation, inner radius $R_{inn}$, outer radius $R_{out}$, and constant linewidth $\Delta V$. The volume density of the envelope, as a consequence of the continuity equation, must be $\rho \propto r^{-3/2}$. For such a model, we computed the emission as a function of position and velocity, and calculated the 2D convolution of the emission with a Gaussian beam. In particular, the intensity as a

function of the projected radius was calculated at each line-of-sight velocity as proportional to the product of the temperature and density of the intersection of the isovelocity surface with the line of sight, and to the derivative of the line-of-sight distance with respect to the line-of-sight velocity (R. Estalella et al., in preparation).

A satisfactory agreement was obtained qualitatively for the range of parameters shown in Table E1. The model PV cut is shown in Figure E2. The inner radius of the envelope is $R_{inn} = 10–20$ au, and the outer radius is $R_{out} = 90–120$ au. The infall velocity is $V_0 = 1.0–1.5$ km s$^{-1}$ at a reference radius of 1" (300 au), corresponding to 1.7–2.6 km s$^{-1}$ at 100 au. This range of infall velocities corresponds to the freefall onto a central mass $M_* = 0.17–0.38 M_\odot$.

#### E.2. Spherical Infalling Envelope Centered on VLA 4B Traced by CS (7–6)

Because of the presence of the large envelope around VLA 4A (Figure 11), in the fitting of the VLA 4B data, we consider only positions east of VLA 4B, away from the position of VLA 4A. Also, there is a lack of emission to the south of VLA 4B, which could be due to the disruption of the southern half of the envelope by the blueshifted jet (Figure 2). Therefore, we restrict our fitting to position angles in the range 0° to 90°. In Figure E3, we show position–velocity cuts centered on the position of VLA 4B, for position angles in this range. As can be seen in the figure, the redshifted velocities, $V > 9.3$ km s$^{-1}$,
<figure><img src="image_31.png" /><figcaption>**Figure E1.** VLA 4A envelope: position-velocity cuts of the CS (7–6) emission, centered on the position of VLA 4A, for different position angles. The position offsets are distances from VLA 4A along the position angle, and are indicated for each panel. Positive offsets correspond to points north of VLA 4A in the cut at PA = 0° and to points west of VLA 4A in the cuts from PA = −20° to −150°. Contours start at 10% of the peak (0.120 Jy beam⁻¹), increasing in steps of 10%.</figcaption></figure>
<table><caption>**Table E1**
VLA 4A: Spherical Infalling Envelope Traced by the CS (7–6) Line</caption><thead><tr><th>Parameter</th><th>Value</th><th>Units</th></tr></thead><tbody><tr><td>Linewidth ΔV</td><td>0.5–1.5</td><td>km s<sup>-1</sup></td></tr><tr><td rowspan="2">Inner radius R<sub>inn</sub></td><td>0.04–0.07</td><td>arcsec</td></tr><tr><td>10–20</td><td>au</td></tr><tr><td rowspan="2">Outer radius R<sub>out</sub></td><td>0.3–0.4</td><td>arcsec</td></tr><tr><td>90–120</td><td>au</td></tr><tr><td>Infall velocity V<sub>0</sub><sup>a</sup></td><td>1.0–1.5</td><td>km s<sup>-1</sup></td></tr><tr><td>Central mass M<sub>*</sub></td><td>0.17–0.38</td><td>M<sub>☉</sub></td></tr></tbody></table>

**Note.**

<table><caption>**Table E2**
VLA 4B. Spherical Infalling Envelope Traced by the CS (7–6) Line</caption><thead><tr><th>Parameter</th><th>Value</th><th>Units</th></tr></thead><tbody><tr><td>Linewidth ΔV</td><td>~0.3</td><td>km s<sup>-1</sup></td></tr><tr><td rowspan="2">Inner radius R<sub>inn</sub></td><td>~0.04</td><td>arcsec</td></tr><tr><td>~12</td><td>au</td></tr><tr><td rowspan="2">Outer radius R<sub>out</sub></td><td>~0.5</td><td>arcsec</td></tr><tr><td>~150</td><td>au</td></tr><tr><td>Infall velocity V<sub>0</sub><sup>a</sup></td><td>1.5–2.2</td><td>km s<sup>-1</sup></td></tr><tr><td>Central mass M<sub>*</sub></td><td>0.38–0.82</td><td>M<sub>☉</sub></td></tr></tbody></table>

**Note.**

<figure><img src="image_32.png" /><figcaption>**Figure E2.** VLA 4A envelope: position-velocity cut of a model of spherically symmetric envelope in freefall, with $\Delta V = 1$ km s$^{-1}$, $R_{\text{inn}} = 0''05$ (15 au), $R_{\text{out}} = 0''35$ (105 au), and $V_0 = 1.2$ km s$^{-1}$ (at a reference radius of 300 au), giving a central mass $M_* = 0.26 M_\odot$. Contours start at 10% of the peak (arbitrary intensity), increasing in steps of 10%.</figcaption></figure>

<figure><img src="image_33.png" /><figcaption>**Figure E3.** VLA 4B envelope. Leftmost panels: position-velocity cuts of the CS (7–6) emission, through the position of VLA 4B, for different position angles, from $\text{PA} = 0^{\circ}$ to $90^{\circ}$. Rightmost panel: position-velocity cut of a model of a spherically symmetric envelope in freefall, with $\Delta V = 0.3$ km s$^{-1}$, $R_{\text{inn}} = 0''04$ (12 au), $R_{\text{out}} = 0''5$ (150 au), and $V_0 = 1.8$ km s$^{-1}$ (at a reference radius of 300 au), giving a central mass $M_* = 0.6 M_\odot$. Contours start at 10% of the peak (0.100 Jy beam$^{-1}$), increasing in steps of 10%. The position offsets are distances from VLA 4B along the position angle, and are indicated for each panel.</figcaption></figure>

<footnote>a At a radius of 1" (300 au).</footnote>

<footnote>a At a radius of 1" (300 au).</footnote>
show a pattern similar to that expected for a spherical infalling envelope.

We fitted the model of an infalling envelope with optically thin emission, with infall velocity and temperature proportional to $r^{-1/2}$, with no rotation, inner radius $R_{\text{inn}}$, outer radius $R_{\text{out}}$, and constant linewidth $\Delta V$. The range of values of the parameters that better fit the pattern observed in the PV cuts are given in Table E2. The model PV cut is shown in the rightmost panel of Figure E3. The inner radius of the envelope is $R_{\text{inn}} \approx 12$ au, and the outer radius is $R_{\text{out}} \approx 150$ au. The infall velocity is $V_0 = 1.5-2.2 \text{ km s}^{-1}$ at a reference radius of $1''$ (300 au), corresponding to $2.6-3.8 \text{ km s}^{-1}$ at 100 au. This range of infall velocities corresponds to the freefall onto a central mass $M_* = 0.38-0.82 M_{\odot}$.

## ORCID iDs

Ana K. Diaz-Rodriguez https://orcid.org/0000-0001-9112-6474

Guillem Anglada https://orcid.org/0000-0002-7506-5429

Guillermo Blázquez-Calero https://orcid.org/0000-0002-7078-2373

Mayra Osorio https://orcid.org/0000-0002-6737-5267

José F. Gómez https://orcid.org/0000-0002-7065-542X

Gary A. Fuller https://orcid.org/0000-0001-8509-1818

Robert Estalella https://orcid.org/0000-0001-7341-8641

José M. Torrelles https://orcid.org/0000-0002-6896-6085

Sylvie Cabrit https://orcid.org/0000-0002-1593-3693

Luis F. Rodríguez https://orcid.org/0000-0003-2737-5681

Charlène Lefèvre https://orcid.org/0000-0001-7349-6113

Enrique Macías https://orcid.org/0000-0003-1283-6262

Carlos Carrasco-González https://orcid.org/0000-0003-2862-5363

Luis A. Zapata https://orcid.org/0000-0003-2343-7937

Itziar de Gregorio-Monsalvo https://orcid.org/0000-0003-4518-407X

Paul T. P. Ho https://orcid.org/0000-0002-3412-4306

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