Table 1.
Parameters of the high-resolution spectral line observations.
| Observing Date | Frequencies | Line | Array | Phase | Program | ΔV | Beam | PA | rms |
|---|---|---|---|---|---|---|---|---|---|
| (GHz) | Calibrator | km s−1 | (″) × (″) | (°) | (mJy/beam) | ||||
| 2022Mar08 | 1.6 | OH | EVN | J1748+3404 | EW022A | 11.9 | 0.006 × 0.005 | 57 | 0.9 |
| 2023Sep10 | 1.4 | H I | GMRT | J1753+2848 | 44-048 | 10.8 | 4.14 × 2.76 | −10 | 0.5 |
| 2023Sep10 | 1.4 | H I | GMRT | J1753+2848 | 44-048 | 10.8 | 12.07 × 7.27 | 1 | 0.8 |
| 2023Sep10 | 1.4 | H I | GMRT | J1753+2848 | 44-048 | 10.8 | 32.47 × 19.49 | 36 | 1.0 |
Notes. Column (3): The atomic or molecular lines. Column (4): The observational array. Column (5): The phase calibrator. Column (6): The program name. Column (7): The adopted spectral velocity resolution in km s−1 after binning. For the EVN and GMRT line projects, we binned every 2 channels, and for the EVLA OH line project, we binned 4 channels. Columns (8) and (9): The beam FWHM and position angle. Column (10): The 1σ noise level for the channel image with the ΔV listed in Column (7).
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