Table 2
Properties and timescales of the dense cores located within filaments in Sgr B2(N).
 |
 |
T(c) | L | Md+g |  |
Mstellar,ratio | tcore,ff | tfil,ff | |
|---|---|---|---|---|---|---|---|---|---|
| ID | (′′) | (pc) | (K) | (×103 L⊙) | (M⊙) | (M⊙) | (%) | (kyr) | (kyr) |
| F01 A02(e) | 0.64 | 0.21 | 120 | 61 | 300 ± 45 | 90–220 | 20–45 | 8 ± 0.3 | 10–16 |
| A03(e) | 0.70 | 0.20 | 195 | 510 | 140 ± 20 | 230–650 | 60–85 | 13 ± 0.6 | 9–15 |
| A06(e) | 0.90 | 0.19 | 80 | 24 | 255 ± 35 | 60–140 | 20–40 | 14 ± 0.6 | 9–13 |
| A17 | 0.53 | 0.12 | 110 | 29 | 15 ± 1 | 70–160 | 80–90 | 27 ± 1.0 | 4–7 |
| F05 A20 | 0.44 | 0.16 | 50(f) | 0.87 | 20 ± 5 | 20–35 | 40–70 | 18 ± 0.9 | 7–11 |
| F06 A10 | 0.64 | 0.11 | 105 | 36 | 40 ± 5 | 70–170 | 60–80 | 22 ± 0.9 | 4–6 |
| F08 A04 | 0.77 | 0.10 | 170 | 360 | 140 ± 20 | 70–170 | 30–60 | 15 ± 0.6 | 3–5 |
| A05 | 0.84 | 0.12 | 100 | 51 | 200 ± 30 | 80–200 | 25–55 | 15 ± 0.6 | 4–7 |
| A07 | 0.44 | 0.12 | 85 | 7.3 | 70 ± 10 | 35–85 | 30–60 | 9 ± 0.4 | 4–7 |
| A08 | 0.56 | 0.40 | 110 | 33 | 55 ± 10 | 65–170 | 50–80 | 15 ± 0.7 | 27–42 |
| A11 | 0.84 | 0.18 | 50(f) | 3.2 | 100 ± 15 | 30–60 | 20–40 | 21 ± 0.9 | 8–13 |
| A15 | 0.80 | 0.27 | 50(f) | 2.9 | 60 ± 10 | 30–60 | 30–55 | 25 ± 1.1 | 15–23 |
| A19 | 0.83 | 0.45 | 50(f) | 3.1 | 50 ± 5 | 30–65 | 35–60 | 29 ± 1.1 | 32–50 |
| Hub A01 | 1.45 | – | 250(f) | 5900 | 1960 ± 280 | 800–3000 | 25–65 | 11 ± 0.4 | – |
Notes. (a) Angular radius (θcore) of the cores as listed in Paper II. (b)The distance between the core andthe hub (dhub) is determined from a straight line connecting both, and can, therefore, be a lower limit to the real distance when considering projeciton effects. (c)The temperatures (T) have been determined for different molecular species (Möller et al., in prep.) resulting in an error of 10%. After propagation of these errors, we have determined the uncertainties in the gas mass and timescales. (d) The lower value of the stellar mass is obtained from the luminosity listed in the table after decreasing it by a factor of eight. This aims to reproduce: (i) a core radius two times smaller than the measured size, and (ii) a contribution of 50% to the total luminosity coming from accretion and not from stellar radiation. (e) Cores A02, A03, and A06 can also be connected to the central hub via filament F02. (f) Temperatures are assumed, rather than obtained by fitting.
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