All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2276fig1.eps} \end{figure}$ Figure 1: The region of the Pelican nebula (IC 5070), including the compact HII region G84.0+0.8 discussed in this paper. The image covers a field of 107'8 $\times$ 84'1 and is a negative print of an image obtained with the Schmidt telescope on Calar Alto, courtesy of the Centro Astronómico Hispano-Alemán.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2276fig2.eps} \end{figure}$ Figure 2: Narrow-band infrared images of G84.0+0.8 showing the distribution of ionized hydrogen ( top) and excited molecular hydrogen ( bottom), outlining the overall structure of a cavity in the molecular cloud filled with ionized gas. The embedded cluster is clearly seen in both images. North is at the top and East to the left. The size of both images is 3'05 $\times$ 3'05.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{2276fig3.eps} \end{figure}$ Figure 3: Spectrum of the brightest star that appears projected on the embedded cluster, which we classify as a late-type giant and is thus unrelated to the cluster.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{2276fig4.eps} \end{figure}$ Figure 4: Spectrum of the HII region, with the vertical scale increased in the bottom plot to enhance visibility of the faintest features. The prominence of the [OIII] lines near $\lambda = 5000$ Å with respect to the adjacent H $\beta$ and the strength of the HeI lines show that the nebula is ionized by a mid O-type star. The electron density inferred from the relative strengths of the [SII] doublet near $\lambda = 6720$ Å is 460 cm^-3, and the extinction from the H $\beta$ / H $\alpha$ ratio is $A_{\rm V} \simeq 5.9$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{2276fig5.eps} \end{figure}$ Figure 5: The ionizing flux of G84.0+0.8 as inferred from its radio continuum flux (Eq. (2), solid line); and from its angular size and density using respectively n = 460 cm^-3 (Eq. (1); dashed line) and n = 1000 cm^-3 (dotted line). The ionizing fluxes produced by O7V and O9V stars, whose temperatures are respectively T_* = 41 000 K and T_* = 35 900 K (Schaerer & de Koter 1997) are given for reference. As noted in the text, both T_* = 35 900 K and n = 1000 cm^-3 are excluded by the spectroscopy of the nebula, and are plotted here for reference only.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2276fig6.eps} \end{figure}$ Figure 6: 2MASS color-magnitude diagram containing the members of the cluster within a radius of 20'' of $\alpha (2000) = 20^{\rm h} 45^{\rm m} 38^{\rm s}0$ , $\delta (2000) = +44^\circ 15' 20''$ . The locus of the unreddened main sequence at 600 pc and three selected extinction vectors (whose slope is given by the Rieke & Lebofsky 1985, extinction law) are given, including one for the case of a O7V star at 3.5 kpc.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2276fig1.eps} \end{figure}$	Figure 1: The region of the Pelican nebula (IC 5070), including the compact HII region G84.0+0.8 discussed in this paper. The image covers a field of 107'8 $\times$ 84'1 and is a negative print of an image obtained with the Schmidt telescope on Calar Alto, courtesy of the Centro Astronómico Hispano-Alemán.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2276fig2.eps} \end{figure}$	Figure 2: Narrow-band infrared images of G84.0+0.8 showing the distribution of ionized hydrogen ( top) and excited molecular hydrogen ( bottom), outlining the overall structure of a cavity in the molecular cloud filled with ionized gas. The embedded cluster is clearly seen in both images. North is at the top and East to the left. The size of both images is 3'05 $\times$ 3'05.
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$\begin{figure} \par\includegraphics[width=8.35cm,clip]{2276fig3.eps} \end{figure}$	Figure 3: Spectrum of the brightest star that appears projected on the embedded cluster, which we classify as a late-type giant and is thus unrelated to the cluster.
Open with DEXTER