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.