Table 1
Parameters of the detected cyanopolyynes lines.
| Transition | Frequencyc | Eup | VLSR | FWHM | Int. | beam |
| [MHz] | [K] | [km s-1] | [km s-1] | [K km s-1] | ["] | |
|
|
||||||
| HC3N | ||||||
|
|
||||||
| 9−8a | 81 881.4 | 19.6 | 3.9(0.6) | 2.2(0.6) | 2.5(0.4) | 29.5 |
| 10−9a | 90 979.0 | 24.0 | 3.9(0.5) | 2.1(0.5) | 2.3(0.4) | 26.5 |
| 11−10a | 100 076.3 | 28.8 | 3.9(0.4) | 2.2(0.4) | 2.2(0.3) | 24.1 |
| 12−11b | 109 173.6 | 34.1 | 3.9(0.4) | 2.3(0.4) | 0.9(0.1) | 22.1 |
| 15−14 | 136 464.4 | 52.4 | 3.9(0.3) | 2.9(0.3) | 2.1(0.3) | 17.7 |
| 16−15 | 145 560.9 | 59.4 | 3.6(0.2) | 2.8(0.3) | 1.7(0.3) | 16.6 |
| 17−16 | 154 657.2 | 66.8 | 3.9(0.2) | 3.1(0.3) | 1.6(0.2) | 15.6 |
| 18−17 | 163 753.3 | 74.7 | 3.9(0.2) | 3.5(0.3) | 2.1(0.3) | 14.7 |
| 19−18 | 172 849.3 | 82.9 | 3.8(0.2) | 4.4(0.2) | 2.1(0.3) | 14.0 |
| 22−21 | 200 135.3 | 110.5 | 3.2(0.5) | 6.1(0.7) | 1.6(0.2) | 12.1 |
| 23−22 | 209 230.2 | 120.5 | 3.4(0.5) | 6.5(0.6) | 2.1(0.3) | 11.5 |
| 24−23 | 218 324.7 | 131.0 | 3.4(0.5) | 6.1(0.5) | 2.2(0.3) | 11.1 |
| 25−24 | 227 418.9 | 141.9 | 3.4(0.4) | 6.3(0.5) | 2.3(0.3) | 10.6 |
| 26−25 | 236 512.7 | 153.2 | 3.4(0.4) | 6.2(0.5) | 2.3(0.3) | 10.2 |
| 27−26b | 245 606.3 | 165.0 | 2.7(0.5) | 6.1(0.7) | 0.8(0.1) | 9.8 |
| 28−27b | 254 699.5 | 177.2 | 3.4(0.4) | 7.0(0.4) | 1.5(0.2) | 9.5 |
| 29−28b | 263 792.3 | 189.9 | 2.5(0.3) | 7.8(0.5) | 4.7(0.7) | 9.1 |
| 30−29 | 272 884.7 | 203.0 | 3.4(0.6) | 6.6(1.0) | 1.4(0.2) | 8.8 |
|
|
||||||
| HC5Nc | ||||||
|
|
||||||
| 31−30 | 82 539.0 | 63.4 | 3.7(0.7) | 1.7(0.7) | 0.08(0.01) | 29.2 |
| 32−31 | 85 201.3 | 67.5 | 3.9(0.6) | 2.6(0.7) | 0.07(0.01) | 28.3 |
| 33−32 | 87 863.6 | 71.7 | 4.0(0.6) | 2.0(0.6) | 0.06(0.01) | 27.5 |
| 34−33 | 90 525.9 | 76.0 | 3.9(0.6) | 1.8(0.6) | 0.06(0.01) | 26.7 |
| 35−34 | 93 188.1 | 80.5 | 3.9(0.5) | 2.7(0.5) | 0.06(0.01) | 25.9 |
| 36−35b | 95 850.3 | 85.1 | 4.5(0.6) | 1.4(0.7) | 0.04(0.01) | 25.2 |
| 37−36 | 98 512.5 | 89.8 | 3.8(0.6) | 2.7(1.2) | 0.06(0.01) | 24.5 |
| 38−37 | 101 174.7 | 94.7 | 4.6(0.5) | 1.8(0.6) | 0.05(0.01) | 23.9 |
| 39−38 | 103 836.8 | 99.6 | 4.3(0.5) | 1.9(0.5) | 0.03(0.01) | 23.2 |
|
|
||||||
| DC3N | ||||||
|
|
||||||
| 10−9 | 84 429.8 | 22.3 | 3.9(0.6) | 2.1(0.6) | 0.17(0.06) | 28.6 |
| 11−10 | 92 872.4 | 26.7 | 4.4(0.5) | 2.1(0.7) | 0.14(0.05) | 26.0 |
| 12−11 | 101 314.8 | 31.6 | 4.3(0.4) | 2.6(0.5) | 0.15(0.05) | 23.8 |
| 13−12 | 109 757.1 | 36.9 | 4.1(0.4) | 2.7(0.5) | 0.26(0.10) | 22.1 |
| 16−15d | 135 083.1 | 55.1 | 2.1(0.3) | 1.7(0.4) | 0.13(0.05) | 17.7 |
| 17−16 | 143 524.8 | 62.0 | 4.3(0.2) | 3.8(0.4) | 0.27(0.10) | 16.6 |
Notes. The first three columns report the transition, frequency, and upper energy level (Eup). The next three columns report the result of the Gaussian fitting: VLSR velocity, FWHM, and velocity-integrated line intensity (Int.). The last column reports the telescope beam at the frequency of the line.
Discarded line because it is probably contaminated by the molecular cloud (see text, Sect. 4.2).
Discarded line because it does not satisfy criteria 3 to 5 of Sect. 3.2.
The HC3N and DC3N line frequencies are the same in the CDMS and JPL database. In contrast, the JPL HC5N line frequencies are systematically overestimated with respect to those of CDMS, giving VLSR shifted by ~1 km s-1 with respect to the VLSR derived for the HC3N and DC3N lines. We therefore used the HC5N line frequencies from the CDMS database.
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