Figure 1 ESPa DOn S Narval and FEROS

Figure 4. Comparisons between the observed photometry (red points) and the model SED (solid

Figure 2. Top: the nearly sinusoidal fits to the radial velocities of the two

Figure 3. Marginalized posterior probability distributions returned by the MCMC algorithm that was applied

Figure 5. Top: comparisons between the best-fitting synthetic (red) and observed (black) H lines,

Figure 6. A subsample of the wavelength region used to determine the luminosity ratio,

Figure 9. H, He+metal, He, C, Si, and Fe Stokes I and V LSD

Figure 7. Comparisons between best-fitting model (red) and observed (black points) Fe ii (left)

Figure 8. The positions of HD 35502's A and B star components are indicated

Figure 10. Hβ longitudinal magnetic field measurements phased by the rotational period (equation 2).

Figure 11. Longitudinal magnetic field measurements phased by the rotational period (equation 2). The

Figure 12. Photometric observations obtained using various filters and phased by the B star's

Figure 13. Left: dynamic spectra of various H i, He i, C ii, and

Figure 14. Top: observed Hα spectrum (I/Ic, solid black curve) compared with the average

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Figure 1. ESPa. DOn. S, Narval, and FEROS Stokes I LSD profiles (right) and dynamic Stokes I LSD profiles (left) generated. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 4. Comparisons between the observed photometry (red points) and the model SED (solid black curve). The dashed. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 2. Top: the nearly sinusoidal fits to the radial velocities of the two A stars phased by a period of 5. 668 66 d. . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 3. Marginalized posterior probability distributions returned by the MCMC algorithm that was applied to the SED. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 5. Top: comparisons between the best-fitting synthetic (red) and observed (black) H lines, Hγ (left) and Hβ. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 6. A subsample of the wavelength region used to determine the luminosity ratio, LB/LA. The. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 9. H, He+metal, He, C, Si, and Fe Stokes I and V LSD profiles generated from a Teff = 26 k. K, . . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 7. Comparisons between best-fitting model (red) and observed (black points) Fe ii (left) and Mg i (right) lines. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 8. The positions of HD 35502's A and B star components are indicated by the blue diamond and black square. The. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 10. Hβ longitudinal magnetic field measurements phased by the rotational period (equation 2). The measurements. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 11. Longitudinal magnetic field measurements phased by the rotational period (equation 2). The measurements. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 12. Photometric observations obtained using various filters and phased by the B star's rotational period of. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 13. Left: dynamic spectra of various H i, He i, C ii, and Si iii lines. A low-pass filter has been applied to the. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.

Figure 14. Top: observed Hα spectrum (I/Ic, solid black curve) compared with the average synthetic spectrum. . . Mon Not R Astron Soc, Volume 460, Issue 2, 01 August 2016, Pages 1811– 1828, https: //doi. org/10. 1093/mnras/stw 1077 The content of this slide may be subject to copyright: please see the slide notes for details.