Table 2
Detected AlF emission lines towards M-type AGB stars by ALMA observations.
| Source | v | Transition (GHz) | Eu | gu (K) | Aul | Flux (10−3 s−1) | FWHM (Jy kms−1) | Vc (kms−1) | Ang. res. (km s−1) | M.R.S. (arcsec) | Apr. (arcsec) | Obs. date (arcsec) | ϕ |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| o Ceti | 131.8988 | υ = 0, J = 4−3 | 16 | 9 | 0.025 | 0.12 ±0.04 | 5.9 | 47.8 | 0.077 | 2.897 | 0.25 | 21-09-17 | 0.9 |
| 228.7165 | υ = 1,J = 7−6 | 1184 | 15 | 0.147 | 0.46 ±0.14 | 9.7 | 48.5 | 0.049 | 1.267 | 0.5 | 22-09-17 | 0.9 | |
| 296.6988 | υ = 0,J = 9−8 | 71 | 19 | 0.299 | 1.84 ±0.23 | 6.6 | 47.7 | 0.286 | 9.238 | 0.5 | 19-11-18 | 0.1 | |
| 329.6416 (*) | υ = 0,J= 10−9 | 87 | 21 | 0.412 | 4.39 ±0.59 | 8.7 | 47.2 | 0.022 | 0.570 | 0.5 | 09-11-17 | 0.8 | |
| 494.2268 | υ = 0,J= 15−14 | 190 | 31 | 1.41 | 7.60 ±0.84 | 6.2 | 47.4 | 0.172 | 11.962 | 0.5 | 28-11-18 | 0.1 | |
| R Leo | 230.7938 | υ = 0,J = 7−6 | 44 | 15 | 0.138 | 0.24 ±0.06 | 7.2 | –1.0 | 0.133 | 1.941 | 1 | 01-10-16 | 0.5 |
| 0.26 ±0.04 | 6.4 | 0.3 | 1.275 | 13.166 | 5 | 22-03-17 | 0.6 | ||||||
| 0.22 ±0.03 | 5.8 | 0.2 | 0.365 | 5.521 | 2 | 03-05-17 | 0.0 | ||||||
| 0.15 ±0.04 | 6.2 | –2.3 | 0.028 | 0.695 | 0.3 | 21-09-17 | 0.7 | ||||||
| 0.24 ±0.05 | 4.3 | –0.6 | 0.022 | 0.431 | 0.3 | 03-10-17 | 0.7 | ||||||
| 0.19 ±0.05 | 5.7 | –0.6 | 0.025 | 0.597 | 0.3 | 27-10-17 | 0.9 | ||||||
| 494.2268 | υ, = 0,J = 15−14 | 190 | 31 | 1.41 | 3.16 ±0.49 | 5.7 | 0 | 2.570 | 15.118 | CP | 24-03-19 | 0.2 | |
| WHya | 230.7938 (**) | υ, = 0,J = 7−6 | 44 | 15 | 0.138 | 0.49 ±0.15 | 11 | 39.0 | 5.089 | 29.537 | CP | 21-05-17 | 0.5 |
| 494.2268 | υ, = 0,J = 15−14 | 190 | 31 | 1.41 | 4.29 ± 1.22 | 7.3 | 41.1 | 2.039 | 13.634 | CP | 08-06-19 | 0.8 | |
| R Dor | 494.2268 | υ = 0,J= 15−14 | 190 | 31 | 1.41 | 2.13 ±0.72 | 7.7 | 5.5 | 2.135 | 13.812 | CP | 08-06-19 | 0.3 |
| IK Tau | 230.7938 (**) | υ, = 0,J = 7−6 | 44 | 15 | 0.138 | 0.23 ±0.04 | 13.7 | 36.0 | 0.752 | 8.412 | 3 | 13-04-17 | – |
Notes. Spectroscopic data are taken from the CDMS. Integrated flux, the full width at half maximum (FWHM), and the line central velocity (Vc) are from Gaussian fitting. Flux uncertainties (σFlux) are a summation of Gaussian fitting uncertainty and 10% of the total flux due to calibration uncertainty of ALMA data. MRS stands for maximum recoverable scale. Apr. denotes circular aperture used to extract the spectra, and CP denotes where the spectra are extracted from the central pixel (6.6″ ×4.4″) for the ACA observations, ϕ denotes the stellar variability phase at visual wavelengths where ϕmin = 1 and ϕmax = 0.(*) and(**) lines are likely blended with an SO2 line at 329.6459 GHz and a 50TiO2 line at 230.7931 GHz, respectively.
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