Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=17cm,clip]{h4310F1.ps} \end{figure}$ Figure 1: The Carina Nebula in 8 $\mu$ m emission (logarithmic grey-scale) with contours of visual extinction (levels are 7.5, 9.5, 11.5, 13.5 and 15.5 mag). Marked on the figure are the locations of $\eta$ Car (+), Tr 14 (x), the southern and northern molecular clouds, and the additional giant pillar and molecular cloud identified by Zhang et al. (2001). The dotted region outlines the extent of the extinction map. The four condensations labelled (in white) G287.73-0.92, G287.84-0.82, G287.93-0.99 and G288.07-0.80 are discussed in Sect. 3.5. The point sources labelled in black mark the sources discussed in Sect. 4.
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In the text

$\begin{figure} { \psfig{file=h4310F2.ps,width=17cm} }\end{figure}$ Figure 2: The Carina Nebula in 21 $\mu$ m emission (logarithmic grey-scale) with contours of 843 MHz radio continuum emission (levels are 0.04, 0.14, 0.24, 0.34, 0.5, 0.7, 0.9, 1.1, 1.3, 1.5 Jy/beam). Marked in this figure is the location of $\eta$ Car as well as several ionization fronts (including Car I and Car II), and the four condensations; G287.73-0.92, G287.84-0.82, G287.93-0.99 and G288.07-0.80.
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In the text

$\begin{figure} { \psfig{file=h4310F3.ps,width=17cm} }\end{figure}$ Figure 3: 8 $\mu$ m emission in grey-scale with contours of integrated ¹²CO(2-1) emission for the condensations. a) G287.73-0.92: Integrated from -25 to -32 km s^-1, levels are 20, 35, 50, 65, 80, 95 K km s^-1; b) G287.84-0.82: Integrated from -12 to -16 km s^-1, levels are 20, 40, 60, 80, 100, 140, 180 K km s^-1; c) G287.93-0.99: Integrated from -18 to -22 km s^-1, levels are 30, 50, 70, 90, 110, 130 K km s^-1; d) G288.07-0.80: Integrated from -19 to -24 km s^-1, levels are 15, 30, 45, 60, 75, 90, 105 K km s^-1.
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In the text

$\begin{figure} { \psfig{file=h4310F4.ps,angle=-90,width=8.8cm} }\end{figure}$ Figure 4: Line profiles spatially integrated over each condensation. Left to right: G287.73-0.92, G287.84-0.82, G287.93-0.99 and G288.07-0.80. Top to bottom: ¹²CO(2-1) and ¹²CO(1-0); ¹³CO(2-1) and C¹⁸O(1-0); CS(3-2) and CS(2-1) emission. The C¹⁸O(1-0) profiles are multiplied by 5 to make them visible. Note the different temperature scales and velocity ranges.
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In the text

$\begin{figure} { \psfig{file=h4310F5.ps,width=8.8cm} }\end{figure}$ Figure 5: $K_{\rm s}$ -band image for the southern Carina Nebula with contours representing the stellar density distribution for stars with $K_{\rm corr} < 12$ mag (thick black: levels are 2.6, 3, 3.4, 3.8 stars/arcmin²) and the visual extinction map (thin black: levels are 7.5, 9.5, 11.5, 13.5 and 15.5 mag). The cluster Bo 11 is marked, along with the condensations G287.84-0.82 and G287.93-0.99.
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In the text

$\begin{figure} { \psfig{file=h4310F6.ps,angle=-90,width=8.8cm} }\end{figure}$ Figure 6: Colour-colour plot for sources in the Carina Nebula. Included on this are the location of a black-body (solid line) and the limits derived by Lumsden et al. (2002) for MYSOs and compact ${\rm H~{\scriptstyle {II}}}$ regions (dashed lines). Plotted here are: point sources with MSX data (filled triangles), point sources with MSX and IRAS detections (open triangles), MSX sources associated with diffuse emission (filled squares) and the source identified by Megeath et al. (1996) (open asterisk) and Rathborne et al. (2002) (filled asterisk). The numbers mark the sources discussed in Sect. 4.3.
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In the text

$\begin{figure} { \psfig{file=h4310F7.ps,width=17cm,angle=-90} }\end{figure}$ Figure 7: Spectral energy distributions for the candidate YSOs; G287.52-0.41 (source 1, in Fig. 6), G287.84-0.82 (sources 2), G287.88-0.93 (source 3) and G287.87-1.36 (source 4). Open squares represent 2MASS fluxes, stars represent MSX fluxes, while circles mark the IRAS fluxes. The solid line in each plot is a fit to these points using a modified two component black-body function (see text for details). The 8 $\mu$ m flux is excluded from the fit for G287.84-0.82 as it is known to be dominated by emission from PAH molecules. The near-IR points were not included in the fits as these likely represent emission from an extincted hot component rather than dust emission.
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In the text

$\begin{figure} \par\begin{tabular}{rrr} \psfig{file=h4310F8a.eps,width=0.26\text... ...} & \psfig{file=h4310F8o.eps,width=0.27\textwidth}\\ \end{tabular} \end{figure}$ Figure 8: A collection of near-IR three-colour images for candidate YSOs within the Carina Nebula (J-band in blue, H-band in green and $K_{\rm s}$ -band in red). The images are presented in the order in which they are discussed in Sect. 4.5. Included also are yellow ellipses marking the location of IRAS point sources and contours of 8 $\mu$ m emission. Levels are, G287.52-0.41: 0.5, 1; G287.84-0.82: 1, 2, 4, 8, 10; G287.88-0.93: 0.5, 1; G287.57-0.91: 0.5, 1, 1.5; G287.87-1.36: 0.5, 1, 2; G287.86-0.82: 0.5, 0.7; G287.73-1.01: 0.5, 1, 2; G287.80-0.56: 1, 2; G287.51-0.49: 1, 2, 3; G287.22-0.53: 0.8, 1.3; G287.47-0.54: 2, 4, 6; G287.63-0.72: 1, 2, 3; G287.75-0.66: 2, 3, 4; G287.76-0.87: 1, 2; G287.68-1.09: 1, 1.5. All are in units of 10^-5 W m^-2 sr^-1.
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In the text

$\begin{figure} { \psfig{file=h4310F9.ps,width=8.8cm,angle=-90} }\end{figure}$ Figure 9: The IRAS LRS spectrum of G287.84-0.82 (open squares) with error bars, and comparisons with photometry from the IRAS PSC (filled triangles) and MSX PSC (filled squares) and from the MSX images (open circles).
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In the text

$\begin{figure} { \psfig{file=h4310F10.ps,width=8.8cm,angle=-90} }\end{figure}$ Figure 10: The IRAS LRS spectrum of G287.87-1.36 (open squares) with error bars, and comparisons with photometry from the IRAS (filled triangles) and MSX (filled squares) PSCs and from the MSX images (open circles).
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In the text

$\begin{figure} { \psfig{file=h4310F4.ps,angle=-90,width=8.8cm} }\end{figure}$	Figure 4: Line profiles spatially integrated over each condensation. Left to right: G287.73-0.92, G287.84-0.82, G287.93-0.99 and G288.07-0.80. Top to bottom: ¹²CO(2-1) and ¹²CO(1-0); ¹³CO(2-1) and C¹⁸O(1-0); CS(3-2) and CS(2-1) emission. The C¹⁸O(1-0) profiles are multiplied by 5 to make them visible. Note the different temperature scales and velocity ranges.
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$\begin{figure} { \psfig{file=h4310F9.ps,width=8.8cm,angle=-90} }\end{figure}$	Figure 9: The IRAS LRS spectrum of G287.84-0.82 (open squares) with error bars, and comparisons with photometry from the IRAS PSC (filled triangles) and MSX PSC (filled squares) and from the MSX images (open circles).
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$\begin{figure} { \psfig{file=h4310F10.ps,width=8.8cm,angle=-90} }\end{figure}$	Figure 10: The IRAS LRS spectrum of G287.87-1.36 (open squares) with error bars, and comparisons with photometry from the IRAS (filled triangles) and MSX (filled squares) PSCs and from the MSX images (open circles).
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