Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA

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Volume 571 (November 2014)

A&A, 571 (2014) A52

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Table 5

Parameters of the cores.

T_ex ^a

M_gas ^b

N_H₂ ^c

n_H₂ ^c

Σ ^d

ΔV ^e

M _virial

Core

(K)

log (N_CH₃OH/cm^-2)

(M_⊙)

(× 10²⁴ cm^-2)

(× 10⁷cm^-3)

(g cm^-2)

(km s^-1)

(M_⊙)

M_virial/M_gas

240±30

19.5±1.1

0.75±0.13

1.3 ± 0.5

9.9 ± 5.3

4.9 ± 2.1

6.0±0.8

11 ± 6^f

14 ± 10

50±5

15.2±0.2

1.3±0.2

0.8 ± 0.4

3.4 ± 2.4

2.9 ± 1.6

>1.4

>1.5

35 ± 4

16.3±0.2

4.2±0.7

1.1 ± 0.6

3.3 ± 2.4

4.2 ± 2.3

3.0±0.6

15 ± 9

3.6 ± 2.8

110±5

17.7±0.5

2.6±0.2

1.1 ± 0.3

4.4 ± 1.8

4.4 ± 1.3

7.0±0.8

65 ± 22^g

25 ± 10^g

50 ± 5

16.0±0.3

4.7±0.7

1.9 ± 0.7

6.9 ± 3.2

7.2 ± 2.6

2.2±0.5

7 ± 4

1.4 ± 0.6

40±4

15.0±0.3

5.4±0.8

2.8 ± 0.9

12 ± 5

11 ± 4

>1.4

>0.37

Notes.

^(a)

Methanol excitation temperature, T_ex, estimated from the source averaged CH₃OH emission with the myXCLASS software (see Sect. 4.1).

^(b)

Mass estimated using a dust opacity of 1.75 cm² g^-1 at 870 μm (see Sect. 4.1).

^(c)

Estimated from the continuum. The dust temperature, T_dust, corresponds to the excitation temperature, T_ex.

^(d)

Core mass surface density derived as Σ = M_gas/πR², where the radius of the source R was obtained from its size θ (Table 3), and following the expression R = θ/ 2 d, where d is the distance to G35.03.

^(e)

Line width estimated from CH₃OH.

^(f)

The contribution of the internal rotation motions of core A has been subtracted from the CH₃OH line width in the calculation of M_virial (see Sect. 4.2).

^(g)

M_virial would be 5.3 M_⊙ if using a line width of 2 km s^-1, which is the velocity dispersion of the core-free filament emission (see Sect. 3.2.1 and Fig. 5), and M_virial/M_gas would be 2.

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