Table A.1.
Observation log with EMIR on the IRAM 30-m telescope.
| Source | Line | Project ID | Observing date (dd/mm/yy) | Band | νtuning (GHz) | tobs (h) | rms noise (mJy) | 
(Jy K−1) |
|---|---|---|---|---|---|---|---|---|
| PLCK_G045.1+61.1 | CO(4–3) | 094-13 | 07, 10/06/13 | E090 | 101.90 | 1.4 | 10.0 | 6.0 |
| CO(5–4) | 094-13 | 10/06/13 | E150 | 130.20 | 1.6 | 7.3 | 6.2 | |
| CO(6–5) | 223-13, 108-14 | 04/02/14 & 17/09/14 | E150 | 156.40 | 3.4 | 7.9 | 6.3 | |
| CO(8–7) | 223-13 | 19/04/14 | E230 | 207.00 | 2.4 | 4.6 | 7.2 | |
| CO(9–8) | 094-13 | 09/06/13 | E230 | 232.00 | 0.4 | 43.4 | 7.9 | |
| PLCK_G080.2+49.8 | CO(3–2) | 082-12 | 28/10/2012 | E090 | 97.40 | 1.6 | 6.0 | 6.0 |
| CO(5–4) | D09-12 | 30/11/2012 | E150 | 160.12 | 4.6 | 6.4 | 6.6 | |
| CO(7–6) | 223-13 | 03/02/14 | E230 | 224.40 | 3.2 | 6.1 | 7.6 | |
| PLCK_G092.5+42.9 | CO(4–3) | 094-13, 108-14 | 10/04/13 & 20, 21, 22/06/14 | E090 | 104.70 | 13.8 | 4.7 | 6.0 |
| CO(5–4) | 094-13 | 05/06/13 | E150 | 143.68 | 2.0 | 12.6 | 6.1 | |
| CO(6–5) | 108-14 | 17/09/14 | E150 | 162.47 | 0.8 | 10.4 | 6.4 | |
| CO(8–7) | 094-13 | 06/06/13 | E230 | 216.00 | 0.8 | 18.4 | 7.4 | |
| CO(9–8) | 223-13 | 02/02/14 | E230 | 244.60 | 2.4 | 9.0 | 8.0 | |
| CO(10–9) | 223-13 | 19/04/14 | E230 | 270.67 | 2.2 | 12.0 | 8.6 | |
| PLCK_G102.1+53.6 | CO(3–2) | 094-13 | 07, 09/06/13 | E090 | 89.40 | 0.9 | 7.0 | 5.9 |
| CO(5–4) | 094-13 | 09/06/13 | E150 | 148.00 | 1.0 | 9.3 | 6.4 | |
| CO(7–6) | 223-13 | 03/02/14 | E230 | 206.00 | 1.6 | 8.5 | 7.2 | |
| PLCK_G113.7+61.0 | CO(3–2) | 094-13 | 09/04/13 | E090 | 101.90 | 2.4 | 7.0 | 6.0 |
| CO(4–3) | 094-13 | 07/06/13 | E150 | 134.50 | 2.2 | 7.5 | 6.3 | |
| CO(5–4) | 223-13 | 19/04/14 | E150 | 168.80 | 1.2 | 10.2 | 6.5 | |
| CO(7–6) | 217-14 | 18, 19/02/15 | E230 | 236.67 | 4.0 | 15.5 | 7.9 | |
| CO(8–7) | 223-13 | 18/04/14 | E230 | 270.01 | 2.2 | 22.2 | 8.6 | |
| PLCK_G138.6+62.0 | CO(3–2) | 094-13 | 09/04/13 | E090 | 101.90 | 1.6 | 10.1 | 6.0 |
| CO(4–3) | 094-13 | 07/06/13 | E150 | 134.50 | 1.6 | 8.6 | 6.3 | |
| CO(5–4) | 094-13 | 07/06/13 | E150 | 168.00 | 0.8 | 16.1 | 6.7 | |
| CO(7–6) | 217-14 | 19/02/15 | E230 | 231.30 | 1.6 | 14.5 | 7.8 | |
| PLCK_G145.2+50.9 | CO(4–3) | 094-13 | 09/04/13 | E090 | 101.90 | 1.2 | 12.4 | 6.0 |
| CO(6–5) | 094-13 | 05/06/13 | E150 | 151.97 | 0.8 | 17.6 | 6.5 | |
| PLCK_G165.7+67.0 | CO(3–2) | 094-13 | 09/04/13 | E090 | 101.90 | 2.4 | 14.0 | 6.0 |
| CO(4–3) | 094-13 | 05/06/13 | E150 | 143.68 | 0.8 | 11.4 | 6.4 | |
| CO(6–5) | 223-13 | 02, 03/02/14 | E230 | 216.70 | 1.6 | 9.7 | 7.3 | |
| CO(7–6) | 217-14 | 19, 20/02/15 | E230 | 245.50 | 2.4 | 8.8 | 8.2 | |
| PLCK_G200.6+46.1 | CO(3–2) | 094-13 | 08, 10/06/13 | E090 | 88.00 | 1.6 | 6.7 | 5.9 |
| CO(4–3) | 065-13 | 31/08/13 | E090 | 115.90 | 1.4 | 31.9 | 6.0 | |
| CO(5–4) | 065-13 | 31/08/13 | E150 | 145.00 | 2.4 | 6.4 | 6.2 | |
| CO(7–6) | 217-14 | 20, 21/02/15 | E230 | 206.28 | 3.2 | 8.0 | 7.1 | |
| CO(8–7) | 094-13 | 09/06/13 | E230 | 232.00 | 0.8 | 18.3 | 7.8 | |
| PLCK_G231.3+72.2 | CO(3–2) | 094-13 | 08/06/13 | E090 | 89.40 | 1.6 | 5.9 | 5.9 |
| CO(5–4) | 094-13 | 09/06/13 | E150 | 148.00 | 0.8 | 10.6 | 6.4 | |
| CO(7–6) | 217-14 | 20/02/15 | E230 | 209.10 | 2.4 | 15.1 | 7.2 | |
| PLCK_G244.8+54.9 | CO(3–2) | 094-13, 108-14 | 05/04/13 & 17, 18, 19/06/14 | E090 | 89.00 | 9.0 | 3.1 | 5.9 |
| CO(4–3) | 094-13, 223-13 | 06/06/13 & 31/01/14 | E090 | 115.11 | 3.4 | 13.0 | 6.0 | |
| CO(5–4) | 094-13 | 05/06/13 | E150 | 143.68 | 1.6 | 8.8 | 6.4 | |
| CO(6–5) | 094-13, 223-13 | 06/06/13 & 31/01/14 | E150 | 172.30 | 1.6 | 16.8 | 6.6 | |
| CO(8–7) | 094-13 | 06/06/13 | E230 | 230.50 | 1.4 | 15.6 | 7.8 | |
| CO(9–8) | 223-13 | 01, 02/02/14 | E230 | 259.40 | 1.6 | 11.7 | 8.4 | |
| CO(10–9) | 223-13 | 02/02/14 | E330 | 289.70 | 1.4 | 11.5 | 9.1 | |
| CO(11–10) | 223-13 | 02/02/14 | E330 | 317.00 | 3.8 | 15.3 | 10.4 |
Notes. Here νtuning is the tuning frequency of the EMIR receivers that was used to observe a given CO transition. Total exposure times tobs do not include the bad scans discarded for the optimal spectrum reduction. The spectrum rms values were measured on baseline channels with CLASS. Telescope efficiencies 
were extrapolated from the calibration tables and used to convert the line fluxes to Jy km s−1. We note that the CO(3–2) and CO(4–3) transitions in PLCK_G244.8+54.9 and PLCK_G092.5+42.9, respectively, were included in a backup sideband while observing HCN and HCO+ transitions in these sources with long integrations (program 108-14).
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