<figure><img src="image_24.png" /><figcaption>**Fig. C.6.** Best-fitting model (part six) plotted against the observations from the CHARA/VEGA spectro-interferometer. In each panel, the observed squared visibility $V^2$ is plotted with red triangles; the model corresponding to parameters listed in Table 11 is denoted with black points. Residuals of the fit are shown below each panel. The mean acquisition date, the corresponding mean reduced heliocentric Julian date, and the instrument are indicated above each panel.</figcaption></figure>
<figure><img src="image_25.png" /><figcaption>**Fig. C.7.** Best-fitting model (part seven) plotted against the observations from the CHARA/VEGA spectro-interferometer. In each panel, the observed squared visibility $V^2$ is plotted with red triangles; the model corresponding to parameters listed in Table 11 is denoted with black points. Residuals of the fit are shown below each panel. The mean acquisition date, the corresponding mean reduced heliocentric Julian date, and the instrument are indicated above each panel.</figcaption></figure>
<figure><img src="image_26.png" /><figcaption>**Fig. C.8.** Best-fitting model (part eight) plotted against the observations from the CHARA/VEGA spectro-interferometer. In each panel, the observed squared visibility $V^2$ is plotted with red triangles; the model corresponding to parameters listed in Table 11 is denoted with black points. Residuals of the fit are shown below each panel. The mean acquisition date, the corresponding mean reduced heliocentric Julian date, and the instrument are indicated above each panel.</figcaption></figure>
<figure><img src="image_27.png" /><figcaption>**Fig. C.9.** Best-fitting model (part nine) plotted against the observations from the VLTI/AMBER spectro-interferometer. In each panel, the observed squared visibility $V^2$ is plotted with red triangles; the model corresponding to parameters listed in Table 11 is denoted with black points. Residuals of the fit are shown below each panel. The mean acquisition date, the corresponding mean reduced heliocentric Julian date, and the instrument are indicated above each panel.</figcaption></figure>
<figure><img src="image_28.png" /><figcaption>**Fig. C.10.** Best-fitting model (part ten) plotted against the observations from the VLTI/AMBER spectro-interferometer. In each panel, the observed closure phase $T_3\phi$ is plotted with red triangles; the model corresponding to parameters listed in Table 11 is denoted with black points. Residuals of the fit are shown below each panel. The mean acquisition date, the corresponding mean reduced heliocentric Julian date, and the instrument are indicated above each panel.</figcaption></figure>
## Appendix D: Description of the observational material

This section contains templates of tables with observational material. The full tables are available at the CDS.

- Radial velocity measurements are published in Table D.1.

- Photometric observations are published separately for each photometric filter (MO, U, B, V) in Tables D.2–D.5.

- The spectro-interferometric observations are published in form of calibrated squared visibility moduli in Table D.6, and closure phases in Table D.7.

<table><caption>**Table D.1.** RV measurements obtained with the cross-correlation technique described in Sect. 3.2.</caption><thead><tr><th>t<br>(RJD)</th><th>RV<br>(km s<sup>-1</sup>)</th><th>σ<sub>RV</sub><br>(km s<sup>-1</sup>)</th><th>Component</th></tr></thead></table>

**Notes.** *t* denotes time, RV the heliocentric radial velocity, *σ*<sub>RV</sub> the uncertainty of the heliocentric radial velocity, and *component* denotes members of ξ Tau (Aa, Ab, or B). RJD = HJD – 2 400 000, components: Aa., primary of orbit 1, Ab., secondary of orbit 1, and B., primary of orbit 2.

<table><caption>**Table D.2.** Reduced photometric observations acquired with the MOST satellite.</caption><thead><tr><th>t<br>(RJD)</th><th>MO<br>(mag)</th><th>σ<sub>MO</sub><br>(mag)</th></tr></thead></table>

**Notes.** *t* denotes time, MO the magnitude in the MOST filter, and *σ*<sub>MO</sub> the uncertainty of the magnitude in the MOST filter. RJD = HJD – 2 400 000.

<table><caption>**Table D.3.** Reduced photometric observations acquired in the Johnson *U* filter.</caption><thead><tr><th>t<br>(RJD)</th><th>U<br>(mag)</th><th>σ<sub>U</sub><br>(mag)</th><th>Source</th></tr></thead></table>

**Notes.** *t* denotes time, *U* the magnitude in the Johnson *U* filter, *σ*<sub>*U*</sub> the uncertainty of the magnitude in the Johnson *U* filter, and *source* the origin of an observation. RJD = HJD – 2 400 000, sources: 1. Hvar Observatory; 2. South African Astronomical Observatory; 3. Four College Automatic Photometric Telescope.

<table><caption>**Table D.4.** Reduced photometric observations acquired in the Johnson *B* filter.</caption><thead><tr><th>t<br>(RJD)</th><th>B<br>(mag)</th><th>σ<sub>B</sub><br>(mag)</th><th>Source</th></tr></thead></table>

**Notes.** *t* denotes time, *B* the magnitude in the Johnson *B* filter, *σ*<sub>*B*</sub> the uncertainty of the magnitude in the Johnson *B* filter, and *source* the origin of an observation. RJD = HJD – 2 400 000, sources: 1. Hvar Observatory; 2. South African Astronomical Observatory; 3. Four College Automatic Photometric Telescope.

<table><caption>**Table D.5.** Reduced photometric observations acquired in the Johnson *V* filter.</caption><thead><tr><th>t<br>(RJD)</th><th>V<br>(mag)</th><th>σ<sub>V</sub><br>(mag)</th><th>Source</th></tr></thead></table>

**Notes.** *t* denotes time, *V* the magnitude in the Johnson *V* filter, *σ*<sub>*V*</sub> the uncertainty of the magnitude in the Johnson *V* filter, and *source* the origin of an observation. RJD = HJD – 2 400 000, sources: 1. Hvar Observatory; 2. South African Astronomical Observatory; 3. Four College Automatic Photometric Telescope.

<table><caption>**Table D.6.** Calibrated squared visibility moduli estimated from studied spectro-interferometric observations.</caption><thead><tr><th>t<br>(RJD)</th><th>u<br>(m)</th><th>v<br>(m)</th><th>λ<sub>eff</sub><br>(m)</th><th>V<sup>2</sup></th><th>σ<sub>V2</sub></th><th>src</th></tr></thead></table>

**Notes.** *t* denotes time, *u* the baseline projected in the east-west direction, *v* the baseline projected in the north-south direction, *λ*<sub>eff</sub> the effective wavelength, *V*<sup>2</sup> the calibrated squared visibility modulus, *σ*<sub>*V2*</sub> the uncertainty of the calibrated visibility, and *src* the origin of an observation. RJD = HJD – 2 400 000, sources: 1. CHARA/VEGA; 2. MARK III; 3. NPOI; 4. VLTI/AMBER.

<table><caption>**Table D.7.** Closure phases estimated from studied spectro-interferometric observations.</caption><thead><tr><th>t<br>(RJD)</th><th>u<sub>1</sub><br>(m)</th><th>v<sub>1</sub><br>(m)</th><th>u<sub>2</sub><br>(m)</th><th>v<sub>2</sub><br>(m)</th><th>λ<sub>eff</sub><br>(m)</th><th>T<sub>3</sub>φ<br>(deg)</th><th>σ<sub>T<sub>3</sub>φ</sub><br>(deg)</th><th>src</th></tr></thead></table>

**Notes.** *t* denotes time, *u*<sub>1</sub> the first baseline in a closing triangle projected in the east-west direction, *v*<sub>1</sub> the first baseline in a closing triangle projected in the north-south direction, *u*<sub>2</sub> the second baseline in a closing triangle projected in the east-west direction, *v*<sub>2</sub> the second baseline in a closing triangle projected in the north-south direction, *λ*<sub>eff</sub> the effective wavelength, *T*<sub>3</sub>φ the closure phase, *σ*<sub>*T<sub>3</sub>φ*</sub> the uncertainty of the closure phase, and *src* the origin of an observation. RJD = HJD – 2 400 000, sources: 1. CHARA/VEGA, 2. MARK III, 3. NPOI, 4. VLTI/AMBER.