One main priority was to test and implement the band-to-band (B2B) observation mode. This technique allows the calibration of high-frequency observations by using a phase calibrator observed at a lower frequency, e.g. pairing Band 7 target observations with a Band 3 phase calibrator. The campaign conducted tests comparing standard In-Band phase referencing with the B2B mode using quasars, along with exploring the effects of phase calibrator to target separation angles, and phase referencing cycle times. A summary of the campaign is detailed by Asaki Y. et al. 2020 ApJS 247 23A. The successful campaign helped lead to the opening of Band 7 long-baselines during Cycle 7 and has also paved the way for Band 9 and 10 B2B mode observations that will be tested in the coming cycle.

As part of the HF-LBC-2017 effort observations were also conducted of previously targeted spatially extended sources, HL Tau and VY CMa in Band 9 which are available for download.

The released data consists of:

1) Continuum only (TDM) observations in Band 9 of the protostellar disk source HL Tau. Two single pointing executions blocks were taken. The tests included Walsh Switching enabling an aggregate bandwidth of ~15GHz and used phase referencing with <60s cycle times and a calibrator observed at Band 4.  B2B phase transfer was used to test the accuracy in imaging the disk around HL Tau in comparison to the 2014 SV data. A resolution <20mas was achieved and the inner ring structure could be discerned. However in using only the long-baseline array configuration at Band 9 the images resolve out most of the disk structure larger than 0.5” in size.. These data are available here.

2) Continuum and spectral line observations of the oxygen-rich red supergiant VY CMa. Walsh switching was enabled resulting in an aggregate bandwidth of 15GHz, with 6 of the 8 spectral windows (SPWs) using high-spectral resolution FDM mode and cover the 658GHz water maser and SiO line. The single execution block observation used a phase calibrator observed at Band 4 and a cycle time of ~76s. These observations use B2B calibration and subsequent self-calibration using a single channel covering the bright water maser. A comparisons was made to the 2014 SV data indicating that most of the North plume and Clump C is resolved out, while the central source of VY CMa remains unresolved in the continuum. The continuum (line-free) image achieved a resolution of 12x11mas. These data are available here.