Table B.1
Observed line parameters of objects.
T max | rms | T b | ΔV | V line | δV |
![]() |
T ex | N i | |
[K] | [K] | [K] | [km s-1] | [km s-1] | [km s-1] | @ = ∫τdV | [K] | [cm-2] | |
|
|||||||||
CH+(1–0) | |||||||||
835.1375 GHz | |||||||||
NGC 1333 I2A | −0.088 | 0.015 | 0.14 | 4.9 | 5.6 | −1.9 | 3.8@ | 9 | 1.1(13) |
NGC 1333 I4A | −0.071 | 0.016 | 0.21 | 5.6 | 5.8 | −1.1 | 2.7@ | 9 | 8.0(12) |
NGC 1333 I4B | −0.032 | 0.014 | 0.11 | 6.0 | 6.0 | −1.0 | 1.3@ | 9 | 2.9(12) |
Ser SMM1 | −0.096 | 0.013 | 0.25 | 7.3 | 4.1 | −4.1 | 5.8@ | 9 | 1.7(13) |
L 1489 | >–0.030 | 0.010 | 0.014 | − | − | − | <6.3@ | 9 | <1.9(13) |
NGC 7129 FIRS2 | −0.043 | 0.017 | 0.14 | 14.5 | −5.4 | 4.5 | 2.4@ | 9 | 7.0(12) |
W3 IRS5 | −1.3 | 0.009 | 0.89 | 7.1 | −38.5 | −0.1 | 10.0@ | 8a | 4.4(13)a |
2.1 | 0.009 | 0.89 | 3.0 | −34.5 | 3.9 | 9.8 | 38a | 9.6(12)a | |
NGC 6334 I | −3.6 | 0.030 | 3.7 | 5.9 | −2.6 | 5.1 | >48@ | 7a | 2.6(14)a DC |
−2.2 | 0.030 | 3.7 | 4.5 | −11 | −3.3 | 1.6@ | 12a | 5.7(13)a | |
NGC 6334 I(N) | −2.5 | 0.014 | 2.3 | 3.5 | −1.9 | 2.6 | <34@ | 9 | ≤1.0(14) |
−1.5 | 0.014 | 2.3 | 7.1 | 6.5 | 11.0 | 4.9@ | 9 | 1.5(13) DC | |
AFGL 2591 | −0.28 | 0.010 | 0.47 | 10.3 | −16.0 | −10.5 | 8.7@ | 3a | 1.8(14)a |
0.33 | 0.010 | 0.47 | 13.5 | −7.5 | −2.0 | 0.86 | 43a | 8.5(12)a | |
S 140 | −0.30 | 0.030 | − | 2.7 | −9.5 | −2.4 | 2.1–20.1@ | 9 | 0.6–5.9(13) |
0.27 | 0.030 | − | 1.9 | −7.0 | 0.1 | <0.38–2.4 | 38 | 0.16–1.0(12) | |
NGC 7538 IRS1 | 0.63 | 0.014 | 0.91 | 13.5 | −57.5 | −0.1 | 9.3 | 44a | 4.1(12)a |
−0.90 | 0.014 | 0.91 | 8.8 | −51.8 | 5.6 | 8.7@ | 3a | 1.1(14)a | |
|
|||||||||
CH+(2–1) | |||||||||
1669.2813 GHz | |||||||||
NGC 1333 I2A | <0.17 | 0.058 | − | − | − | <0.48 | |||
NGC 1333 I4A | <0.17 | 0.058 | − | − | − | <0.49 | |||
NGC 1333 I4B | <0.18 | 0.061 | − | − | − | <0.51 | |||
Ser SMM1 | <0.22 | 0.074 | − | − | − | <0.63 | |||
W3 IRS5 | 1.1 | 0.045 | 4.1 | 7.7 | −35.9 | 2.5 | 8.7 | ||
NGC 6334 I | −2.8 | 0.12 | 11.4 | 3.9 | −10.3 | −2.6 | 1.15@ | ||
−0.92 | 0.16 | 11.4 | 4.5 | −2.5 | 5.2 | 0.36@ | |||
NGC 6334 I(N) | <0.31 | 0.11 | 1.7 | − | − | − | <0.87 | ||
AFGL 2591 | 0.85 | 0.077 | 2.3 | 8 | −4.6 | 0.9 | 3.7 | ||
NGC 7538 IRS1 | 0.41 | 0.12 | 2.9 | 10.7 | −57.7 | 0.3 | 2.7 | ||
|
|||||||||
OH+ (1–0) | |||||||||
1033.1186 GHz | |||||||||
NGC 1333 I2A | <0.055 | 0.018 | 0.26 | − | − | − | <-0.59@ | 9 | <5.2(12) |
NGC 1333 I4A | −0.040 | 0.020 | 0.25 | 1.4 | 4.1 | −2.8 | ≤0.2@ | 9 | ≤1.9(12) |
NGC 1333 I4B | −0.043 | 0.019 | 0.17 | 1.7 | 1.8 | −5.2 | ≤0.63@ | 9 | ≤5.7(12) |
Ser SMM1 | −0.20 | 0.065 | 0.43 | 9.7 | 4.8 | −3.7 | 8.3@ | 9 | 7.3(13) |
L 1489 | <0.50 | 0.017 | 0.037 | − | − | − | <3.9@ | 9 | <3.4(13) |
NGC 7129 FIRS2 | −0.024 | 0.021 | 0.22 | 7.4 | −1.9 | 8.0 | 1.0@ | 9 | 8.8(12) |
W3 IRS5 | −0.2 | 0.015 | 1.7 | 5.9 | −42 | −3.6 | 0.99@ | 9 | 8.8(12) |
0.1 | 0.015 | 1.7 | 9.4 | −33 | 5.4 | 0.50 | 38 | 5.9(11) | |
NGC 6334 I | −0.55 | 0.031 | 6.0 | 5.9 | −10.0 | −2.3 | 0.66@ | 9 | 5.2(12) |
−2.1 | 0.031 | 6.0 | 6.4 | −1.6 | 6.1 | 2.8@ | 9 | 2.3(13) DC | |
NGC 6334 I(N) | −0.99 | 0.021 | 3.0 | 4.9 | −1.6 | 2.9 | 3.8@ | 9 | 3.3(13) |
−1.35 | 0.021 | 3.0 | 3.5 | 3.2 | 7.7 | 3.7@ | 9 | 3.3(13) DC | |
AFGL 2591 | −0.14 | 0.016 | 0.90 | 11.8 | −16.1 | −10.6 | 1.0@ | 3a | 1.6(13)a |
−0.71 | 0.016 | 0.90 | 9.4 | 2.8 | 8.3 | 3.6@ | 3a | 6.1(13)a DC | |
S 140 | −0.30 | 0.024 | 0.96 | 4.5 | −4.1 | 3.0 | 1.5@ | 9 | 1.8(13) |
−0.18 | 0.024 | 0.96 | 6.7 | 3.5 | 10.6 | 1.3@ | 9 | 1.5(13) DC | |
NGC 7538 IRS1 | −0.18 | 0.026 | 1.6 | 12.0 | −48 | 9.4 | 1.6@ | 9 | 1.4(13) |
Notes. Tmax refers to the line peak intensity, negative values indicate absorption in [K] below background; ΔV to the FWHM line width; Vline to the line mean velocity; δV = Vline − VLSR to the line shift with respect to the systemic velocity of the object; rms to the root mean square noise level; Tb to the background (continuum) intensity; the integrated line flux (line luminosity) is given in [K km s-1]), @ indicates integrated optical depth [km s-1]; Tex is the assumed excitation temperature; and Ni is the total column density. Cases where the fitted line model had to be used for intensity or absorption instead of the observed data because of line blending are indicated with an asterisk (*), and values labeled (a) are from 1D slab model fitting (Bruderer et al. 2010a,Appendix B). A minus sign (−) indicates observations but no detection. Absorption components indicated with “DC” are suspected to originate from diffuse interstellar clouds in the foreground. The error range in emission measure is up to factors of 0.8–2 for emission lines, and factors of 0.8–1.5 for lines in absorption. Details and error margins of the column densities are given in Sect. 4 and Table 3.
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