Table 1.
Extragalactic spectral scans at mm and submm wavelengths.
| Source (#) | Frequency | Telescope | Ref. |
|---|---|---|---|
| coverage | |||
| (GHz) | |||
| NGC 4945 | 82–354 (a) | SEST 15m | 1 |
| NGC 253 | 86–116 | IRAM 30m | 2 |
| 86–116 (b) | ALMA | 3 | |
| 85–116 | Nobeyama 45m | 4, 5 | |
| 129–175 | IRAM 30m | 6 | |
| N113 (LMC) | 85–357 (a) | SEST 15m | 7 |
| M 82 | 86–116 | IRAM 30m | 2 |
| 130–175 | IRAM 30m | 8 | |
| 241–260 | IRAM 30m | 8 | |
| 190–307 (c) | CSO 10.4m | 9 | |
| NGC 1068 | 86–116 | IRAM 30m | 10 |
| 85–116 | Nobeyama 45m | 4, 5 | |
| 161–169 (b) | IRAM 30m | 11 | |
| 176–184 (b) | IRAM 30m | 11 | |
| 190–307 (c) | CSO 10.4m | 12 | |
| PKS 1830-211 (d) | 57–94 | ATCA | 13 |
| 59–94 | Yebes 40m | 14 | |
| Arp 220 | 86–116 | IRAM 30m | 2 |
| 202–242 | SMA | 15 | |
| M 51 | 86–116 | IRAM 30m | 2 |
| 83–116 | IRAM 30m | 16 | |
| 130–148 | IRAM 30m | 16 | |
| M 83 | 86–116 | IRAM 30m | 2 |
| NGC 4418 | 84–113 | ALMA | 17 |
| 214–294 (b) | ALMA | 17 | |
| IC 342 | 84–116 | Nobeyama 45m | 4, 5 |
| IC 10 | 84–116 | Nobeyama 45m | 18 |
| NGC 3256 | 85–113 | ALMA | 19 |
| 214–273 | ALMA | 19 | |
| NGC 3627 | 85–116 | IRAM 30m | 20 |
| 140–148 | IRAM 30m | 20 | |
| 85–115.5 | Nobeyama 45m | 20 | |
| Survey (10) | 74–111 (c) | FCRAO 14m | 21 |
| Survey (23) | 84–92 | IRAM 30m | 22 |
| 108–116 | IRAM 30m | 22 | |
| Survey (4) | 85–268 (b) | IRAM 30m | 23 |
| Survey (7, LMC) | 85–116 | MOPRA 22m | 24 |
Notes. The source column indicates the name of the survey target or the number of surveyed sources in multisource works (labeled Survey). Sources are chronologically ordered according to the year of its first survey publication. Large Magellanic Cloud (LMC) sources are indicated.
Not fully sampled. Multiple tunings within the indicated frequency coverage with broadband receivers.
Molecular absorber system. The frequency refers to rest frequency, which at the redshift of the source corresponds to observed frequecy range of 30 − 50 and 31.5 − 50 GHz for the two references, respectively.
References. (1) Wang et al. (2004); (2) Aladro et al. (2015); (3) Meier et al. (2015); (4) Nakajima et al. (2018); (5) Takano et al. (2019); (6) Martín et al. (2006); (7) Wang et al. (2009); (8) Aladro et al. (2011a); (9) Naylor et al. (2010); (10) Aladro et al. (2013); (11) Qiu et al. (2020); (12) Kamenetzky et al. (2011); (13) Muller et al. (2011); (14) Tercero et al. (2020); (15) Martín et al. (2011); (16) Watanabe et al. (2014); (17) Costagliola et al. (2015) (18) Nishimura et al. (2016a); (19) Harada et al. (2018) (20) Watanabe et al. (2019); (21) Snell et al. (2011); (22) Costagliola et al. (2011); (23) Li et al. (2019); (24) Nishimura et al. (2016b)
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