Table 2
Overview of detected TiO2 lines.
| Transition | νlab | Eup/k | νmin | νmax | Δν | rms | Peak | I | Size | SW |
|
(MHz) | (K) | (km s-1) | (mJy) | (Jy) | (Jy km s-1) | (″) | tail | ||
|
|
||||||||||
| 22(1,21)−21(2,20) | 310 554.735 | 180.5 | −15.2 | 51.3 | 1.0 | 16 | 0.22 | 9.57 | 0.9 | Y |
| 23(1,23)−22(0,22) | 310 782.713 | 182.4 | −43.9 | 102.3 | 1.0 | 16 | 0.27 | 15.28 | 0.9 | Y |
| 40(8,32)−39(9,31) | 311 462.082 | 675.9 | 19.4 | 66.7 | 1.9 | 10 | 0.10 | 2.31 | 0.8 | – |
| 7(5,3)−6(4,2) | 312 248.341 | 47.9 | −43.7 | 80.96 | 1.9 | 16 | 0.29 | 20.32 | 0.8 | N |
| 10(4,6)−9(3,7) | 312 732.066 | 57.7 | −19.4 | 105.1 | 1.9 | 16 | 0.15 | 9.43 | 0.5 | ? |
| 30(3,27)−30(2,28) | 312 816.809 | 354.4 | −68.2 | 60.0 | 1.9 | 16 | 0.16 | 12.98 | 0.5 | ? |
| 11(4,8)−10(3,7) | 321 401.936 | 65.7 | −33.9 | 50.5 | 0.9 | 24 | 0.19 | 7.24 | 0.8 | ? |
| 28(2,26)−28(1,27) | 321 501.043 | 298.8 | −35.0 | 51.2 | 0.9 | 24 | 0.13 | 4.76 | 0.9 | N |
| 35(8,28)−35(7,29) | 322 333.594 | 532.4 | −36.4 | 108.1 | 1.0 | 19 | 0.15 | 7.03 | 0.8 | N |
| 33(8,26)−33(7,27) | 322 612.696 | 481.4 | −0.1 | 63.9 | 1.0 | 18 | 0.16 | 4.18 | 0.9 | N |
| 23(2,22)−22(1,21) | 324 492.930 | 196.1 | −47.9 | 79.4 | 1.9 | 29 | 0.21 | 9.64 | ≲0.5 | N |
| 37(8,30)−37(7,31) | 324 965.693 | 586.5 | 3.6 | 59.8 | 1.9 | 30 | 0.15 | 4.92 | 0.5 | N |
| 26(1,25)−26(0,26) | 325 322.035 | 246.5 | −25.2 | 81.8 | 7.6 | 21 | 0.11 | 1.85 | 0.5 | N |
| 26(4,22)−25(5,21) | 325 500.415 | 281.5 | −7.7 | 55.7 | 3.8 | 28 | 0.13 | 2.75 | 0.5 | N |
| 28(8,20)−28(7,21) | 325 600.792 | 367.0 | −0.4 | 90.2 | 3.8 | 28 | 0.18 | 3.89 | 0.5 | N |
Notes. Parameters listed for spectrum extracted in a 1″ diameter aperture centred on the star. See also Fig. 1. Columns are transition, rest frequency, upper-level energy, minimum and maximum νLSR reached, velocity resolution and rms noise at which the identification was made, peak and integrated flux, maximum diametric size of the integrated emission at 3σ level, and a marker for emission in the south-west tail (Y, N, ?, and – for yes, no, maybe, and unknown). Species other than TiO2 detected inside the plotted spectral windows are marked in Fig. 1.
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