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Figure 1:
Integrated C18O
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Figure 2:
Maps of the C18O
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Figure 3:
The integrated 13CO(J=1-0)
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Figure 4:
Sample 13CO and C18O J=1-0 spectra observed in
a 6
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Figure 5:
A comparison of the
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Figure 6:
Clumps in the central and northern part of Cha I.
Output of the cl_surf routine. Each clump identified with
the Clumpfind programme is shown as an isointensity surface
in the (x,y,v) space. Different colours are used to help
in distinguishing between separate clumps. The intensity
level chosen for this figure is TA* = 1 K. The x and y axes represent the offset in arcminutes from the map
centre (RA =
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Figure 7: Cha I association members and candidate members projected on the integrated C18O intensity map of the cloud. Sources of the coordinates are Schwartz (1991) (Optical candidate members, black triangles), Persi et al. (2000) (known members with NIR excess, red squares; member candidates with NIR excess, open red triangles), Cambrésy et al. (1998) (new Young Stellar Object candidates, asterisks) and Gómez & Kenyon (2001) (candidate pre-main-sequence stars, open circles). The locations of the reflection nebulae Ced 112, Ced 110 and Ced 111 (from north to south) are indicated by open squares. The locations of the class 0 protostar candidates Cha-MMS1 and Cha-MMS2 are indicated by filled circles. |
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Figure 8: Polarization vectors of field stars and Cha I members (Whittet et al. 1994; McGregor et al. 1994) superposed on the integrated C18O intensity map of Cha I. |
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Figure 9:
Top: distribution of the clump masses in
Cha I. Middle: the ratios of the gravitational
potential to the kinetic energies,
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Figure 10:
The distribution of external pressures,
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Figure 11:
a) The "equilibrium mass'' m(x), i.e. the clump
mass as a function of the density parameter
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