All Figures

$\begin{figure} \par\includegraphics[width=9cm,clip]{4649fig1.eps} \end{figure}$ Figure 1: Calibrated measurements of $S_{\rm {A100}}$ and $S_{\rm {B100}}$ for 0716+714 vs. time during 2003 November 10 to 16. The sinusoidal pattern is due to source polarization (see the text).
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4649fig2.eps} \end{figure}$ Figure 2: Calibrated measurements of $S_{\rm {B230}}$ for 0716+714, 0836+710 and 1928+738 during 2003 November 10 to 15. The dashed line on the top inset represents the best linear fit to the 0716+714 light curve.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4649fig3.eps} \end{figure}$ Figure 3: Calibrated 86 GHz light curves of 0716+714, 0836+710 and 1928+738 during 2003 November 10 to 16. The dashed line on the top inset represents the best linear fit to the 0716+714 flux density evolution during 2003 November 10 to 15.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{4649fig4.eps} \end{figure}$ Figure 4: $D(\tau )$ function for 0716+714 at 86 GHz. Since the data are unevenly sampled, we derived $D(\tau )$ using an interpolation procedure. A minimal interpolation interval of ${\sim } 2.5$ h (3 to 5 times larger than the typical S₈₆ sampling time-range) was chosen. To assess the errors caused by the interpolation, $D(\tau )$ was derived twice, first by starting at the beginning of the time series and second by proceeding backwards.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{4649fig5.eps} \end{figure}$ Figure 5: Plots of the fits of functions (2) and (3) to the 86 GHz data of 0716+714. Each plot represents a time bin $\protect\la$ 12 h of observing time (labelled within each of them) with a minimum of ten data points. The time spans, ordered from top to bottom and from left to right, cover the whole observing time. The whole data set has been plotted together in the right-bottom plot. The sinusoidal lines represent the independent non-linear least squares fits of functions (2) and (3). The resulting averaged P and $\chi$ variables are given within each corresponding plot. Errors were originallycomputed as 1- $\sigma$ uncertainties from the fits. For the right-bottom plot, the errors from the absolute total flux density and polarization angle uncertainties (see Sect. 2) have been taken int account (added in quadrature).
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In the text

$\begin{figure*} \par\includegraphics[width=18cm,clip]{4649fig6.eps} \end{figure*}$ Figure 6: 86 GHz polarization patterns of the secondary calibrators. For the sake of clarity, a shift of $\pi$ rad was added to function (3) to match function (2), i.e. $S'_{\rm{B100}}(i)-S_{0}(i)=1/2 P(i) \cos{2(\alpha(i)+\pi/2)}$ (see Sect. 2.3). For each source, the data from the whole observing time-range is presented. The sinusoidal lines represent the non-linear least squares fits to the data. The resulting averaged P and $\chi$ variables are given within each corresponding plot. The errors presented on each plot were computed by adding in quadrature the 1- $\sigma$ uncertainties from the fits and the errors from the absolute total flux density and polarization angle uncertainties (see Sect. 2).
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{4649fig7.eps} \end{figure}$ Figure 7: 86 GHz P curves for 0716+714, 0836+710 and 1803+784. Time bins of <24 h were used for all the sources. For 0716+714 the results for time bins ${\protect \la} 12$ h are also presented. Horizontal bars symbolise the time range over which each estimate of P was computed.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4649fig8.eps} \end{figure}$ Figure 8: 86 GHz polarization angle vs. time for 0716+714. The results obtained for time bins of both <24 h and $\protect\la$ 12 h are presented. Horizontal bars symbolise the time range over which each $\chi$ estimate was computed. For the sake of clarity, the $\chi$ time series of the calibrators (which are all constant within their corresponding errors) have not been plotted due to their large uncertainties, typically of 15 $^{\circ }$ -20 $^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4649fig9.eps} \end{figure}$ Figure 9: Amplitude of fractional polarization variability, as a function of time. The vertical bars represent the V_P and $V_{\chi }$ propagated errors whereas the horizontal bars symbolise the maximum possible time range over which the variability took place. See the text for definitions.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4649fig10.eps} \end{figure}$ Figure 10: Evolution of the spectral index $\alpha _{86-229}$ in 0716+714. The absolute total flux density calibration errors of S₈₆ and S₂₂₉ (see Sect. 2) were taken into account to compute those of $\alpha _{86-229}$ . The dashed line represents the best linear fit to the data, which is consistent with a pattern with a rate $\dot{\alpha}_{86-229}=(\rm {-0.03}\pm \rm { 0.02})~\rm {d}^{-1}$ and average $\bar{\alpha}_{86-229}=-0.23 \pm 0.10$ .
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4649figa1.eps} \end{figure}$ Figure A.1: Angles in the reference polarization plane ( x, y) as seen from the A100 and B100, IRAM 30 m heterodyne receivers. $\alpha (t)$ , which is defined in ( x, y) and can be measured by fitting Eqs. (A.5) and (A.6), relates to the astronomical electric vector position angle $\chi (t)$ (defined from north to east in the equatorial coordinate system (RA, Dec), to the parallactic angle $\eta (t)$ and to the elevation angle $\epsilon (t)$ .

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4649fig1.eps} \end{figure}$	Figure 1: Calibrated measurements of $S_{\rm {A100}}$ and $S_{\rm {B100}}$ for 0716+714 vs. time during 2003 November 10 to 16. The sinusoidal pattern is due to source polarization (see the text).
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$\begin{figure} \par\includegraphics[width=9cm,clip]{4649fig2.eps} \end{figure}$	Figure 2: Calibrated measurements of $S_{\rm {B230}}$ for 0716+714, 0836+710 and 1928+738 during 2003 November 10 to 15. The dashed line on the top inset represents the best linear fit to the 0716+714 light curve.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{4649fig3.eps} \end{figure}$	Figure 3: Calibrated 86 GHz light curves of 0716+714, 0836+710 and 1928+738 during 2003 November 10 to 16. The dashed line on the top inset represents the best linear fit to the 0716+714 flux density evolution during 2003 November 10 to 15.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{4649fig7.eps} \end{figure}$	Figure 7: 86 GHz P curves for 0716+714, 0836+710 and 1803+784. Time bins of <24 h were used for all the sources. For 0716+714 the results for time bins ${\protect \la} 12$ h are also presented. Horizontal bars symbolise the time range over which each estimate of P was computed.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4649fig9.eps} \end{figure}$	Figure 9: Amplitude of fractional polarization variability, as a function of time. The vertical bars represent the V_P and $V_{\chi }$ propagated errors whereas the horizontal bars symbolise the maximum possible time range over which the variability took place. See the text for definitions.
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