Earliest phases of star formation (EPoS) - Dust temperature distributions in isolated starless cores

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Volume 592 (August 2016)

A&A, 592 (2016) A61

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Table 2

Properties of the studied cores.

Object

n₀^a

n_out^a

N₀^a

r₀^a

r_out^a

r_sym

N_H(r_sym)

η^a

T₀^a

T_out^a

M_core^b

L_bol^c

[cm^-3]

[cm^-2]

[au]

[cm^-2]

[K]

[M_⊙]

[L_⊙]

CB 4-SMM¹³

2.5E4

1E1

1.0E22

1.7E4

9.0E4

4.1E4

(0.4 ± 0.2)E21

5.2

11.9

19.0

2.9

0.77

CB 17-SMM²⁴

1.1E5

6E2

3.0E22

1.2E4

5.5E4

2.8E4

(3.5 ± 1.0)E21

4.8

10.4

13.5

3.9

0.37

CB 26-SMM2¹⁵

8.0E4

5E2

1.7E22

7.5e3

3.9E4

2.5E4

(2.5 ± 1.0)E21

3.0

11.8

14.2

3.1

0.30

CB 27-SMM²³

1.1E5

1E3

2.6E22

1.1E4

4.2E4

2.9E4

(5.0 ± 1.5)E21

4.0

9.8

14.4

6.0

0.44

B 68-SMM¹³

1.6E5

3E2

2.8E22

1.0E4

4.7E4

2.7E4

(1.0 ± 0.5)E21

5.0

7.7

17.3

2.6

0.23

CB 244-SMM2¹⁴

3.2E5

5E2

9.2E22

6.3E3

7.2E4

3.5E4

(5.0 ± 2.0)E21

2.6

7.5

14.0

0.53

Notes. Source-related remarks (see also Launhardt et al. 2013):

^(a)

Values determined from circular profile fits to the results of the ray-tracing inversion technique using the OH5a dust model; see Sect. 3.3.

^(b)

Derived by integrating the column density maps out to R = 5 × 10⁴ au (see Fig. 7) and corrected for He and metals with μ = 1.4 (see Sect. 3.2).

^(c)

Taken from Launhardt et al. (2013, Table 6).

⁽¹⁾

relatively round or only slightly elliptical core;

⁽²⁾

very elliptical core or pronounced tail;

⁽³⁾

single core and no nearby protostar;

⁽⁴⁾

multiple cores and nearby protostar with partial blending;

⁽⁵⁾

not a coherent core but super-projection of 2−3 filamentary cores.

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