Table A.1
Gaussian fits to the F = 0.5−1.5 and 0.5−0.5 lines of the NJ = 10−01 FS component of SH+ observed with three different telescopes toward the Orion Bar (for vLSR = 10.50 km s-1).
| Rest frequency |
|
Line width | ||||
| Telescope | Line | (MHz) | (mK km s-1) | (km s-1) | Signal-to-noise | |
|
|
||||||
| IRAM 30 m | ||||||
| 1.5−0.5 | 345 944.22 (20) | 383 (30) | 1.95 (19) | ~10 | ||
| 0.5−0.5 | 345 858.38 (20) | 185 (31) | 1.68 (32) | ~5 | ||
| ACA | ||||||
| 1.5−0.5 | 345 944.55 (20) | 260 (20) | 1.23 (10) | ~12 | ||
| 0.5−0.5 | 345 858.42 (20) | 114 (25) | 1.10 (26) | ~6 | ||
| ALMA | ||||||
| 1.5−0.5 | 345 944.29 (20) | 668 (51) | 1.20 (10) | ~12 | ||
| 0.5−0.5 | 345 858.00 (20) | 295 (58) | 0.92 (20) | ~7 | ||
Notes. Parentheses show the Gaussian fit uncertainties (in units of the least significant digits). For the fitted frequencies, we adopt an overall 1σ uncertainty of 0.2 MHz (~0.2 km s-1). This should be considered as a systematic uncertainty due to uncertainties in vLSR (see text). IRAM 30 m spectrum smoothed to ~0.4 km s-1, similar to ALMA and ACA; signal-to-noise determined on the peaks and refering to ~0.4 km s-1 resolution for IRAM 30 m and to the native spectral resolution for ALMA and ACA.
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