Table 3
Results of HCN J = 2 → 1 line observations.
| Object | (ν1, ν2, ν3) | vLSR -range | ∫ TMBdv | R |
|---|---|---|---|---|
| (km s−1) | (K km s−1) | |||
| R For | (0,0,0) | [−18.5,+18.5] | 5.8(1) | – |
| (0, 11c, 0) | [−6.1,+2.1] | 0.59(5) | 9.8 | |
| (0, 11d, 0) | – | <0.16 | >36 | |
| R Lep | (0,0,0) | [−4, +34.5] | 10.1(2) | – |
| (0, 11c, 0) | [+6.8, +16.5] | 1.02(8) | 9.9 | |
| (0, 11d, 0) | – | <0.23 | >44 | |
| AI Vol | (0,0,0) | [−54.4,-23.6] | 15.7(1) | – |
| (0, 11c, 0) | [−47.2,−31.3] | 11.8(1) | 1.3 | |
| (0, 11d, 0) | [−42.2,−34.3] | 1.14(9) | 14 | |
| X Cnc | (0,0,0) | [−19.6,-3.7] | 1.20(5) | – |
| (0, 11c, 0) | – | <0.14 | >8.6 | |
| (0, 11d, 0) | – | <0.17 | >7.0 | |
| CQ Pyx | (0,0,0) | [−11.3,+15.2] | 16.4(1) | – |
| (RAFGL 4254) | (0, 11c, 0) | [−11.3,+11.3] | 10.2(1) | 1.6 |
| (0, 11d, 0) | [−4.6,+3.1] | 0.28(7) | 59 | |
| CW Leo | (0,0,0) | [−47.0,-6.0] | 615.4(2) | – |
| (IRC+10216) | (0, 11c, 0) | [−40.9,−9.1] | 99.2(2) | 6.2 |
| (0, 11d, 0) | [−39.7,−10.6] | 9.7(1) | 63 | |
| X Vel | (0,0,0) | [≈−28.3, ≈−2.1] | 2.25(9) | – |
| (0, 11c, 0) | [≈−26.2, ≈−16.9] | 0.52(5) | 4.3 | |
| (0, 11d, 0) | – | <0.25 | >9 | |
| RW LMi | (0,0,0) | [−23.0,+21.6] | 68.7(2) | – |
| (CIT 6) | (0, 11c, 0) | [−23.0,+21.6] | 36.4(1) | 1.9 |
| (0, 11d, 0) | [−16.4,+6.0] | 1.47(8) | 47 | |
| U Hya | (0,0,0) | [−39.2,−22.3] | 2.49(1) | – |
| (0, 11c, 0) | – | <0.30 | >8.3 | |
| (0, 1 1d, 0) | – | <0.29 | >8.6 | |
| V Hya | (0,0,0) | [≈ −33, ≈ +7.1] | 9.3(2) | – |
| (0, 1 1c, 0) | [≈ −33, ≈ −3] | 6.2(1) | 1.5 | |
| (0, 1 1d, 0) | – | <0.41 | >23 | |
| V358 Lup | (0,0,0) | [−24.5,+22.1] | 30.7(1) | – |
| (RAFGL 4211) | (0, 1 1c, 0) | [−15.8,+6.7] | 4.8(1) | 6.4 |
| (0, 1 1d, 0) | – | <0.29 | >106 | |
| X Tra | (0,0,0) | [−15.8,+12.4] | 2.56(1) | – |
| (0, 1 1c, 0) | [−7.6,+7.8] | 0.68(8) | 3.8 | |
| (0, 1 1d, 0) | – | <0.25 | >10 | |
| II Lup | (0,0,0) | [−42.2,−15.2] | 22.3(1) | – |
| (0, 1 1c, 0) | [−27.3,−3.2] | 9.0(1) | 2.5 | |
| (0, 1 1d, 0) | – | <0.38 | >59 |
Notes. Results of our APEX observations of the three J = 2 → 1 lines in three rows for each star (name in the first column): preceded by its vibrational quantum numbers, we list the LSR velocity range covered by emission and the velocity-integrated main-beam brightness temperature for each line, i.e., the line flux, for which the uncertainty in the last digit is given in parentheses. Upper limits (3σ) in this quantity for the (0, 11d, 0) line were calculated by assuming that it covered the same velocity range as the (0, 1 1c, 0) line if detected, otherwise the range of the (0,0,0) was assumed, as it was for upper limits in the (0, 1 1c, 0) line. The rightmost column gives for the (0, 11c, 0) and (0, 11d, 0) lines the ratio of these line fluxes to that of the (0,0,0) line.
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