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Table 4

Data from HC3N observations.

Galaxy Line I(HC3N)a SνΔv Δv Telescope η mb θmb T scalea References
[K km s-1] [Jy km s-1] [km s-1] [′′]
Arp 220 10-9 2.02 ± 0.15 45  ±  3 340 OSO 20 m 0.59 44 (1)
Arp 220 10-9b 0.4 ± 0.15 11  ±  4 350 SEST 15 m 0.75 55 (2)
Arp 220 12-11 0.96 ± 0.1 23  ±  2 170 OSO 20 m 0.52 36 (1)
Circinus 10-9b 1.01 ± 0.1 27.6  ±  2.7 290 SEST 15 m 0.75 55 (1)
IC 342 10-9 2.6 ± 0.7 14  ±  4 52 IRAM 30 m 0.8 25 (3)
IC 694 12-11  < 0.30  < 7.4 ... OSO 20 m 0.52 36 (1)
IC 860 28-27 0.54 ± 0.07 3.9  ±  0.5 175 IRAM 30 m 0.59 9 (1)
I17208 10-9 0.33 ± 0.03 2.2  ±  0.2 330 IRAM 30 m 0.80 28 (1)
M82 12-11 5.6 ± 0.6 30  ±  3 155 IRAM 30 m 0.80 25 (3)
Maffei 2 12-11 1.42 ± 0.05 10.9  ±  0.4 200 IRAM 30 m 0.73 24 (1)
NGC 34 10-9b  < 0.45  < 12 ... SEST 15 m 0.75 55 (1)
NGC 253 9-8 5.8 ± 0.6 27  ±  3 63c IRAM 30 m ... 29 Tmb (4)
NGC 253 10-9 5.8 ± 0.6 27  ±  3 63c IRAM 30 m ... 26 Tmb (4)
NGC 253 12-11 4.4 ± 0.7 19  ±  3 63c IRAM 30 m ... 21 Tmb (4)
NGC 253 15-14 4.4 ± 0.3 24  ±  2 77, 85 IRAM 30 m ... 19 Tmb (5)
NGC 253 15-14 3.6 ± 0.6 16  ±  3 63c IRAM 30 m ... 17 Tmb (4)
NGC 253 16-15 3.8 19 77c, 85c IRAM 30 m ... 17 Tmb (5)
NGC 253 17-16 3.0 ± 0.2 15  ±  1 72c IRAM 30 m ... 16 Tmb (5)
NGC 253 17-16 3.4 ± 0.4 15  ±  2 63c IRAM 30 m ... 15 Tmb (4)
NGC 253 18-17 2.2 ± 0.5 11  ±  2 73 IRAM 30 m ... 15 Tmb (5)
NGC 253 19-18 4.6 ± 0.6 22  ±  3 74 IRAM 30 m ... 14 Tmb (5)
NGC 253 26-25 3.2 ± 0.7 21  ±  5 63c IRAM 30 m ... 12 Tmb (4)
NGC 613 10-9b  < 0.26  < 7.0 ... SEST 15 m 0.75 55 (1)
NGC 1056 16-15  < 0.17  < 1.3 ... IRAM 30 m 0.67 17 (1)
NGC 1068 10-9b 0.39 ± 0.05 11  ±  1 100 SEST 15 m 0.75 55 (1)d
NGC 1365 10-9b  < 0.61  < 417 ... SEST 15 m 0.75 55 (1)d
NGC 1377 16-15  < 0.28  < 2.1 ... IRAM 30 m 0.67 17 (1)
NGC 1377 25-24  < 0.26  < 1.9 ... IRAM 30 m 0.63 10.5 (1)
NGC 1614 10-9b  < 0.39  < 11 ... SEST 15 m 0.75 55 (1)
NGC 1808 10-9b 0.2 ± 0.1 6  ±  3 250 SEST 15 m 0.75 57 (2)
NGC 2146 10-9  < 0.38  < 7.7 ... OSO 20 m 0.59 42 (1)
NGC 2146 12-11  < 0.38  < 9.2 ... OSO 20 m 0.52 36 (1)
NGC 2623 12-11  < 0.50  < 12 ... OSO 20 m 0.52 36 (1)
NGC 3079 10-9 0.60 ±  0.05 4.0  ±  0.3 500 IRAM 30 m 0.80 28 (1)
NGC 3079 16-15  < 0.54  < 4 ... IRAM 30 m 0.80 17 (1)
NGC 3079 25-24  < 0.40  < 3 ... IRAM 30 m 0.80 10.5 (1)
NGC 3256 10-9b  < 0.12  < 3.3 ... SEST 15 m 0.75 55 (2)
NGC 3690 12-11  < 0.31  < 7.5 ... OSO 20 m 0.52 36 (1)
NGC 4418 e 10-9 0.8 ± 0.08 5  ±  0.5 122 IRAM 30 m 0.77 27 (6)
NGC 4418e 16-15f 1.7 ± 0.08 12  ±  0.6 130 IRAM 30 m 0.70 17 (6)
NGC 4418 e 25-24 1.6 ± 0.2 15  ±  2 140 IRAM 30 m 0.53 11 (6)
NGC 4945 9-8 2.16 ± 0.50 47  ±  11 230 SEST 15 m 0.78 63 Tmb (7)
NGC 4945 10-9 1.99 ± 0.21 41  ±  4 290 SEST 15 m 0.75 55 Tmb (7)
NGC 4945 11-10 2.92 ± 0.35 65  ±  8 340 SEST 15 m 0.73 52 Tmb (7)
NGC 4945 12-11 4.18 ± 0.38 98  ±  9 340 SEST 15 m 0.71 49 Tmb (7)
NGC 4945 15-14 2.13 ± 0.29 52  ±  7 250 SEST 15 m 0.65 40 Tmb (7)
NGC 4945 16-15g 5.02 ± 0.19 120  ±  5 330 SEST 15 m 0.63 37 Tmb (7)
NGC 4945 17-16 2.26 ± 0.55 48  ±  12 280 SEST 15 m 0.61 33 Tmb (7)
NGC 4945 24-23  < 0.60  < 12 ... SEST 15 m 0.48 23 Tmb (7)
NGC 4945 25-24  < 0.60  < 12 ... SEST 15 m 0.46 22 Tmb (7)
NGC 5135 10-9b  < 0.13  < 3.7 ... SEST 15 m 0.75 55 (1)
NGC 6946 12-11  < 0.32  < 2.5 ... IRAM 30 m 0.73 24 (1)
NGC 7130 10-9b  < 0.10  < 2.7 ... SEST 15 m 0.75 55 (2)
UGC 5101 10-9  < 0.12  < 0.76 ... IRAM 30 m 0.80 28 (1)

References. (1) This work; (2) Aalto et al. (2002); (3) Henkel et al. (1988); (4) Mauersberger et al. (1990); (5) Martín et al. (2006); (6) Aalto et al. (2007); (7) Wang et al. (2004).

Notes. 

(a)

The temperature scale of the integrated intensities are given in the T scale column. Upper limits are 2σ calculated from the rms of the noise surrounding the line for our data. For our data, errors are given in 1σ and calculated from the rms. Since many articles lack information about sizes of errors and methods used when calculating the errors, most errors are given as printed in the respective article. However, if the size of the error is clearly written, it has been recalculated to 1σ.

(b)

Measured in HNC 1-0 spectrum.

(c)

Fixed when fitting Gaussian.

(d)

These values are calculated from HNC 1-0 spectra already published in Pérez-Beaupuits et al. (2007).

(e)

See Costagliola & Aalto (2010) for an extensive survey of HC3N in this galaxy, with data not included in this table.

(f)

Contaminated by para-H2CO, estimated to 20%. The given value is only for the HC3N component.

(g)

Contaminated by para-H2CO.

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