Table A.1.
Source parameters assumed for propynethial in each of the sets of observations, and for propynal in those observations that resulted in a non-detection.
| Source | Telescope | θs(a) | Tbg | ΔV |  |
Tex | Refs. |
|---|---|---|---|---|---|---|---|
| (″) | (K) | (km s−1) | (mK) | (K) | |||
| Propynethial | |||||||
| NGC 6334I | ALMA | – | 27.0 | 3.2 | 3.3 (b) | 135 | 1 |
| Sgr B2(N) | GBT | 5 | 5.3 | 10.75 | 9.9 | 49.7 | 2, 13, 14, 15 |
| Barnard 1 | IRAM | – | 2.7 | 0.8 | 2.4 | 10 | 3, 4 |
| IRAS 4A | IRAM | – | 2.7 | 5.0 | 2.5 | 21 | 3, 5 |
| L1157B1 | IRAM | – | 2.7 | 8.0 | 1.8 | 60 | 6 |
| L1157mm | IRAM | – | 2.7 | 3.0 | 3.0 | 60 | 6 |
| L1448R2 | IRAM | – | 2.7 | 8.0 | 3.7 | 60 | 7 |
| L1527 | IRAM | – | 2.7 | 1.2 | 3.3 | 10 | 7, 8 |
| L1544 | IRAM | – | 2.7 | 0.5 | 2.1 | 10 | 9, 10 |
| SVS13A | IRAM | 0.3 | 2.7 | 3.0 | 6.4 | 80 | 3, 5 |
| TMC1 | IRAM | – | 2.7 | 0.3 | 6.5 | 10 | 11, 12 |
| Propynal | |||||||
| NGC 6334I | ALMA | – | 27.0 | 3.2 | 3.3 (b) | 135 | 1 |
| Sgr B2(N) | GBT | – | 2.7 | – | – |  |
(c) |
| Barnard 1 | IRAM | – | 2.7 | 0.8 | 2.4 | 10 | 3, 4 |
| IRAS 4A | IRAM | – | 2.7 | 5.0 | 2.5 | 21 | 3, 5 |
| L1157B1 | IRAM | – | 2.7 | 8.0 | 1.8 | 60 | 6 |
| L1157mm | IRAM | – | 2.7 | 3.0 | 3.0 | 60 | 6 |
| L1448R2 | IRAM | – | 2.7 | 8.0 | 3.7 | 60 | 7 |
| L1527 | IRAM | – | 2.7 | – | – |  |
(d) |
| L1544 | IRAM | – | 2.7 | 0.5 | 2.1 | 10 | 9, 10, (f) |
| SVS13A | IRAM | 0.3 | 2.7 | 3.0 | 6.4 | 80 | 3, 5 |
| TMC1 | IRAM | – | 2.7 | – | – | 10 | (e) |
Notes.
This detection was reported by Turner (1991). Individual fits to ΔV and 
for this multiline detection are detailed in Turner (1991); only the derived Tex is reported here.
This detection is reported in this work. Individual fits to ΔV and 
for this multiline detection are detailed in Table B.2; only the derived Tex is reported here.
This detection was reported by Irvine et al. (1988). Individual fits to ΔV and 
for this multiline detection are detailed in Irvine et al. (1988); only the assumed Tex is reported here.
Jimenez-Serra et al. (2016) reported a single line (90, 9 − 80, 8) detection of propynal in L1544. See text and Table B.1 for further discussion.
†Taken either as the 1σ RMS noise level at the location of the target line, or for line confusion limited spectra, the reported RMS noise of the observations.
References.Araki et al. (2017), McGuire et al. (2018a); [2] Neill et al. (2012); [3] Melosso et al. (2018); [4] Cernicharo et al. (2018); [5] Higuchi et al. (2018); [6] McGuire et al. (2015); [7]Jørgensen et al. (2002); [8] Araki et al. (2017); [9] Hily-Blant et al. (2018); [10] Crapsi et al. (2005); [11] McGuire et al. (2018b); [12] Gratier et al. (2016); [13] Remijan et al. (2008); [14] McGuire et al. (2016); [15] Turner (1991).
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