Table 3
Observable υ = 0 and 1, ΔJ = 0, ΔF = 0 transitions of OH in the ATOMIUM frequency line setting (excluding ΔF = ±1 and very high N, J transitions).
| Line | JPL Frequency(a) | Unc.(b) | υ, N, J(c) | Fup –Flow(c) | Eup(d) | A(e) | ndet.(f) |
|---|---|---|---|---|---|---|---|
| (MHz) | (MHz) | (cm−1, K) | (×10−6 s−1) | ||||
| 1 | 221335.49 | 0.29 | 0, 13, 27/2 | 13− −13+ | 3319.3,4776 | 2.39 | 6 |
| 2 | 221353.48 | 0.29 | 14− −14+ | 7 | |||
| 3 | 223683.92 | 1.53 | 1, 17, 33/2 | 17− −17+ | 8889.8,12791 | 0.90 | 0 |
| 4 | 223713.79 | 1.53 | 16− −16+ | 0 | |||
| 5 | 236328.12 | 0.56 | 0, 17, 33/2 | 17− −17+ | 5533.5, 7962 | 1.07 | 4(g) |
| 6 | 236359.64 | 0.56 | 16− −16+ | 2(h) | |||
| 7 | 252127.10 | 0.43 | 0, 14, 29/2 | 14+ −14− | 3819.1, 5495 | 3.03 | 6 |
| 8 | 252145.35 | 0.43 | 15+ −15− | 9 | |||
| 9 | 265734.66 | 0.80 | 0, 18, 35/2 | 18+ −18− | 6157.7, 8860 | 1.38 | 2(i) |
| 10 | 265765.32 | 0.80 | 17+ −17− | ?(i) | |||
| 11 | 269530.55 | 1.09 | 1, 15, 31/2 | 15− −15+ | 7752.6, 11155 | 3.23 | 0 |
| 12 | 269547.76 | 1.09 | 16− −16+ | 0 |
Notes. (a)Frequency taken from version 5 of the JPL catalog; frequency and uncertainty from observations of ATOMIUM stars are given in Table 4. (b)Calculated JPL catalog uncertainty derived from laboratory measurements. (c)Quantum numbers defined in Sect. 3.3. (d)Upper energy level in cm−1 and K (in italics). For a same value of J, the Fup and Flow level energies are identical within one tenth of a cm−1. (e)Einstein A spontaneous emission probability; see also last row in Appendix A tables. (f)Number of detected OH sources in ATOMIUM program. (g)Unambiguous assignment of hyperfine transition for R Hya, S Pav and R Aql; in U Her assignment to F′ – F′′= 17 – 17 from OH line stacking (see Sect. 8.2.3). (h)Unambiguous hyperfine identification for R Hya and identification from OH line stacking for T Mic. (i)Line 9 is observed at the ~5σ level in R Hya (Sect. 8.2.3) and in Mira (Fig. F.1). The J = 35/2 line 10 is detected at low (~2.5σ) significance in R Hya and blended with TiO2 in Mira (Fig. F.1).
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