| Tuning | Setup | FTS200 coverage | VESPA center | Observing |
| name | [GHz] | [GHz] | mode | |
| E150 150.000 UI | POINT2MM | 147.70–155.48 | WSW | |
| E150 176.500 UI | L170250 | 158.52–166.30 & 174.20–181.98 | 176.553 | WSW |
| E230 230.500 UI | L224250 | 212.52–220.30 & 228.20–235.98 | 217.9102 & 230.538 | WSW, PSW, FSW |
| E330 345.139 UI | L338890 | 342.84–350.62 | 345.94 | WSW |
Observations on the approximately point-like source IRC10216 were
obtained under the technical time T06-16 during 2016 November 15–17 under
mostly stable weather with opacities of 0.1–0.2 at 225 GHz. Four EMIR
frequency setups (and one setup for HERA not included in this report) were
tested, including the 1mm band around the CO(2–1) line of frequent
interest for observers, as well as a setup close to the edge of the
atmospheric window of the 2mm band, which is expected to be especially
sensitive to the calibration. All spectral line backends - WILMA, FTS in
its wide resolution mode, and VESPA configured to 40 kHz resolution and
120 MHz bandwidth - were connected. The 1mm band setup was observed in
all three switching modes available for spectral line observations: wobbler
switching (designated WSW in the following) observations used a throw of
90
in azimuth with a phase time of 2 s, frequency switching
(FSW) a throw of
23.4 MHz at a phase time of 0.2 s, and position
switching (PSW) was done relative to an off position 600
west (in
right ascension) of the source. Table 1 lists the observing
setups and table 2 lists the spectral lines that are used in
the following work.