All Figures

$\begin{figure} \par\mbox{\includegraphics[height=0.1875\textheight]{4038fg1a.ps}... ...ludegraphics[height=0.1875\textheight]{4038fg1n.ps}\hspace*{2.3cm}} \end{figure}$ Figure 1: VLA D-configuration images of the $\lambda =7$ mm continuum emission. Contour levels are drawn in steps of the corresponding 2 $\sigma$ rms noise level; the average 1 $\sigma$ rms noise level is $\sim$ 0.15 mJy/beam. The synthesized beam is shown in the bottom left corner of each panel; the average beam size is $\sim$ 1 $.\!\!^{\prime\prime}$ 5.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.5cm]{4038fg2a.ps}\hspace*{0.8m... ...g2k.ps}\hspace*{0.8mm} \includegraphics[width=5.5cm]{4038fg2l.ps} } \end{figure}$ Figure 2: VLA D-configuration images at $\lambda =1.3$ cm ( left column), $\lambda =2.0$ cm ( middle column), and $\lambda =3.6$ cm ( right column) for RY Tau, DG Tau and DG Tau B, HL Tau, and UZ Tau. Contour levels are given for each panel separately in multiples of 2 $\sigma$ rms noise level. The average 1 $\sigma$ rms noise levels are approximately 50, 80, and 30 $\mu$ Jy/beam at 1.3, 2.0, and 3.6 cm, respectively. About 30 $^{\prime \prime }$ to the east of HL Tau lies XZ Tau (indicated by crosshairs).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.5cm]{4038fg3a}\hspace*{3mm} \... ...{4038fg3c}\hspace*{3mm} \includegraphics[width=8.5cm]{4038fg3d} } \end{figure}$ Figure 3: Free-free emission contribution to 7-mm flux densities. The dashed line represents the fit to the centimetre fluxes, assuming that 50% of the 1.3-cm emission arises from free-free radiation. The square depicts the corrected 7-mm flux after subtraction of the estimated free-free contribution (shown as open circle). The thick line shows the power-law fit to the millimetre data; the shaded region indicates the uncertainty range for the 1-7 mm slope. Data points shortwards of $\lambda =7$ mm were compiled from the literature (Table 5).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{4038fg4.ps} \end{figure}$ Figure 4: Distribution of dust opacity indices. ISM-sized dust grains have $\beta \simeq 2$ , while particles much larger than the observing wavelength $\lambda =7$ mm have a frequency-independent opacity law ( $\beta =0$ ). The populated intermediate regime is indicative for the presence of millimetre-sized dust aggregates.
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=0.1875\textheight]{4038fg1a.ps}... ...ludegraphics[height=0.1875\textheight]{4038fg1n.ps}\hspace*{2.3cm}} \end{figure}$	Figure 1: VLA D-configuration images of the $\lambda =7$ mm continuum emission. Contour levels are drawn in steps of the corresponding 2 $\sigma$ rms noise level; the average 1 $\sigma$ rms noise level is $\sim$ 0.15 mJy/beam. The synthesized beam is shown in the bottom left corner of each panel; the average beam size is $\sim$ 1 $.\!\!^{\prime\prime}$ 5.
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$\begin{figure} \par\includegraphics[width=7.5cm]{4038fg4.ps} \end{figure}$	Figure 4: Distribution of dust opacity indices. ISM-sized dust grains have $\beta \simeq 2$ , while particles much larger than the observing wavelength $\lambda =7$ mm have a frequency-independent opacity law ( $\beta =0$ ). The populated intermediate regime is indicative for the presence of millimetre-sized dust aggregates.
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