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Table 4

List of transitions to which Gaussian or hyperfine-structure fits were applied.

Transition N obs a N det b N 2vel c N gb d N vir e
Chamaeleon I
HNC 1–0f 57 46 – – –
HC3N 10–9g 57 18 0 4h 1
N2H+ 1–0g 57 19 0 4h 1
C4H 1011–910 57 10 0 3i 1
C4H 1010–99 57 8 0 3j 1
C34S 2–1 57 23 1 1 1
CH3OH 21–11 E 57 31 0 3k 1
CH3OH 20–10 A+ 57 41 0 2l 1
CS 2–1f 57 56 – – –
C18O 2–1 60 60 4 1 1
C17O 2–1g 33 32 1 3j 1
H2CO 31,2–21,1 33 8 0 2l 0
N2H+ 3–2 15 5 0 4h 1
Chamaeleon III
H13CO+ 1–0 20 5 0 0 0
HNC 1–0f 20 17 – – –
HC3N 10–9g 20 3 0 1 0
N2H+ 1–0g 20 2 0 1 0
C34S 2–1 20 2 0 0 0
CH3OH 21–11 E 20 10 0 1 0
CH3OH 20–10 A+ 20 15 0 1 0
CS 2–1f 20 20 – – –
C18O 2–1 29 29 2 1 0
C17O 2–1g 2 2 0 1 0

Notes.

(a)

Number of observed cores.

(b)

Number of cores with 3σ detections in terms of the peak temperature that were used for the fitting (hyperfine structure fitting or symmetric, Gaussian lines).

(c)

Number of cores showing (and fitted by) two velocity components in their spectra.

(d)

Number of gravitationally bound cores assuming a temperature of 10 K to derive the non-thermal velocity dispersion.

(e)

Number of virialized cores.

(f)

CS 2−1 is optically thick in both Cha I and III toward all the cores detected in C34S 2−1 (see Sect. C.2). The majority of cores detected in HNC 1−0 have asymmetric, non-Gaussian like spectra which might be a sign of optical thickness. We therefore do not fit these two transitions.

(g)

Hyperfine-structure fit.

(h)

Bound cores: Cha1-C1, C2, C3, C4.

(i)

Bound cores: Cha1-C1, C3, C4.

(j)

Bound cores: Cha1-C1, C2, C3.

(k)

Bound cores: Cha1-C1, C2, C5.

(l)

Bound cores: Cha1-C1, C2.

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