All Figures

Figure 1: Example images from the survey of representative type 1 (SFO 68) and type 2 (SFO 62) clouds. Each cloud is represented by a pair of images, from the Digitised Sky Survey (left) and of the MSX 8 m emission (right). Contours of the radio emission are overlaid on each image, along with an arrow representing the direction towards the suspected ionising star from Yamaguchi et al. (1999) and identifiers in the case of multiple radio sources. In order to save space, we present only the radio maps at the wavelength with the best resolution or sensitivity for each cloud.

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In the text

	Figure 1: continued.
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In the text

	Figure 2: Digitised Sky Survey red image of SFO 86. The greyscale coding is a negative logarithmic scale to adequately present both the faint emission from the cloud and the bright optical emission to the NW of the BRC. The IRAS point source identified by Sugitani & Ogura (1994) is marked by a cross.
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In the text

Figure 3: Digitised Sky Survey red image of SFO 72 overlaid with contours of MSX 8 m emission. The greyscale coding is a negative logarithmic scale to better illustrate the high extinction seen towards the cloud and also the lack of bright-rim emission from its edge. The cross indicates the position of SFO 72 from Sugitani & Ogura (1994). The MSX 8 m emission is localised around a potential PDR or cluster at the cloud tip.

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In the text

	Figure 4: 2MASS band image of SFO 62, overlaid with the 3 cm contours from our radio survey. The contour levels begin at 6 mJy and are spaced by 10 mJy.
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In the text

Full Version

Figure 1: Images from the survey of clouds with radio detections. Each cloud is represented by a pair of images, from the Digitised Sky Survey (left) and of the MSX 8 m emission (right). Contours of the radio emission are overlaid on each image, along with an arrow representing the direction towards the suspected ionising star from Yamaguchi et al. (1999) and identifiers in the case of multiple radio sources. In order to save space, we present only the radio maps at the wavelength with the best resolution or sensitivity for each cloud.

Open with DEXTER


In the text

	Figure 1: continued.
Open with DEXTER


In the text

	Figure 1: continued.
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In the text

	Figure 1: continued.
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In the text

	Figure 1: continued.
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In the text

	Figure 1: continued.
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In the text

	Figure 1: continued.
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In the text

	Figure 1: continued.
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In the text

	Figure 1: continued.
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In the text

	Figure 1: continued.
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In the text

	Figure 1: continued.
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In the text

	Figure 1: continued.
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In the text

Figure 2: Digitised Sky Survey images of the three clouds for which MSX information is not available. Contours of the radio emission are overlaid on each image, along with an arrow representing the direction towards the suspected ionising star from Yamaguchi et al. (1999) and identifiers in the case of multiple radio sources. In order to save space, we present only the radio maps at the wavelength with the best resolution or sensitivity for each cloud.

Open with DEXTER


In the text