Table 3
Integrated line intensities of HCO+, H13CO+ and N2H+ towards our source sample.
| Source |  dV (K km s-1) |
|||||||||
| HCO+ | H13CO+ | N2H+ | ||||||||
| (6–5) | (8–7) | (11–10) | (12–11) | (6–5) | (7–8) | (9–8) | (6–5) | (8–7) | (11–10) | |
|
|
||||||||||
| VLA1623 | 2.2(0.4) | 0.7(0.2) | ≤0.5 | ≤0.3 | 0.10(0.06) | ≤0.2 | ≤0.3 | 0.16(0.06) | ≤0.3 | ≤0.2 |
| L1527 | 1.26(0.09) | ≤0.8 | ≤1.0 | ≤0.6 | ≤0.3 | ≤0.4 | ≤0.3 | ≤0.3 | ≤0.5 | ≤0.4 |
| L1157-MM | 0.63(0.09) | ≤0.8 | ≤0.8 | ≤0.5 | ≤0.2 | ≤0.3 | ≤0.2 | ≤0.2 | ≤0.4 | ≤0.3 |
| NGC 1333-IRAS2 | 1.4(0.6) | 1.5(0.3) | 0.8(0.3) | – | 0.09(0.06) | ≤0.1 | ≤0.1 | 0.36(0.09) | ≤0.6 | ≤0.6 |
| Serpens-FIRS 1 | 3.8(0.6) | 3.2(0.3) | 1.9(0.3) | – | 0.41(0.09) | 0.29(0.09) | 0.08(0.06) | 1.21(0.09) | 0.7(0.1) | 0.10(0.08) |
| L1641 S3 MMS 1 | 0.9(0.4) | 1.5(0.3) | 1.6(0.3) | 1.0(0.3) | ≤0.2 | ≤0.1 | ≤0.1 | 0.18(0.09) | ≤0.3 | ≤0.2 |
| Cep E-mm | 1.9(0.2) | 1.3(0.4) | 0.3(0.2) | ≤0.9 | ≤0.2 | ≤0.2 | ≤0.2 | 0.11(0.06) | ≤0.3 | ≤0.2 |
| IC 1396N | 6.7(0.6) | 3.4(0.5) | 2.24(0.05) | 1.31(0.03) | 0.21(0.10) | 0.2(0.1) | ≤0.4 | 0.9(0.1) | 0.8(0.2) | ≤0.6 |
| NGC 7129-FIRS2 | 1.2(0.2) | 1.6(0.4) | 0.5(0.3) | – | ≤0.5 | ≤0.5 | ≤0.4 | 0.34(0.09) | ≤0.6 | ≤0.4 |
Notes. For further details, see Tables B.1 to B.9. The 3σ uncertainties that are given in brackets result from Gaussian fits performed with the CLASS software. Finally, note that the HCO+ (12–11) transition has not been observed towards NGC 1333–IRAS2, Serpens–FIRS 1 and NGC 7129–FIRS2 (see Sect. 2.2).
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