Keywords: mrtcal-check

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# Observations dedicated to the comparison between MRTCAL and MIRA

Table: Observing setups. The covered frequency range is indicated for FTS200, and the center frequency of the 120MHz wide windows for VESPA. The last column lists the observing modes for the according setup (with WSW wobbler switching, FSW frequency switching, and PSW position switching).
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 225GHz. 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 40kHz resolution and 120MHz 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 2s, frequency switching (FSW) a throw of 23.4MHz at a phase time of 0.2s, 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.

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