The flux density upper limits for circumstellar OH maser emission for our SMC sample. Listed values are Spitzer MIPS 24 μm flux (F24) from Boyer et al. (2011), predicted 35 μm flux values taken from the best-fitting dusty model of the source (explained in Section 4.5), predicted OH maser flux (FOH,predicted) assuming our median masing efficiency of 23 per cent F35 photons to FOH photons, and the noise level (σ) of the observation (both combined observations for IRAS 00483−7347. Also shown are the upper limits for maser efficiency (maximum efficiency) and the probability of a 3σ-level detection for each targeted observation calculated with our bootstrapping method using the maser efficiencies of the LMC and Galactic samples from Goldman et al. (2017).
| Object . | F24μm . | F35μm, predicted . | FOH,predicted . | σ . | Maximum . | Likelihood . |
|---|---|---|---|---|---|---|
| name . | (mJy) . | (mJy) . | (mJy) . | (mJy) . | efficiency . | of detection . |
| Parkes targets | ||||||
| IRAS 00483−7347 | 660.0 | 307 | 71 | 3.7 | 3.6 per cent | 97.7 per cent |
| IRAS F00486−7308 | 91.1 | 39 | 9 | 4.5 | 34.5 per cent | 40.7 per cent |
| IRAS 00591−7307 | 95.4 | 44 | 10 | 7.7 | 52.1 per cent | 23.3 per cent |
| IRAS 01074−7140 | 396.0 | 235 | 54 | 3.4 | 4.3 per cent | 97.7 per cent |
| ATCA sources | ||||||
| OGLE SMC-LPV-15504 | 31.6 | 13 | 3 | 7.1 | 158.9 per cent | 5.8 per cent |
| 2MASS J01033142−7214072 | 19.2 | 8 | 1 | 6.3 | ||
| HV 12149 | 12.7 | 7 | 2 | 6.5 | 278.0 per cent | 1.2 per cent |
| OGLE SMC-LPV-14322 | 19.0 | 11 | 3 | 7.6 | ||
| 2MASS J00592646−7223417 | 18.9 | 13 | 3 | 6.5 | ||
| BMB-B75 | 92.0 | 43 | 10 | 9.5 | 66.5 per cent | 19.7 per cent |
| OGLE J004942.72−730220.4 | 27.8 | 14 | 3 | 10.0 | ||
| MSX SMC 018 | 262.0 | 116 | 27 | 7.2 | 18.7 per cent | 67.5 per cent |
| Object . | F24μm . | F35μm, predicted . | FOH,predicted . | σ . | Maximum . | Likelihood . |
|---|---|---|---|---|---|---|
| name . | (mJy) . | (mJy) . | (mJy) . | (mJy) . | efficiency . | of detection . |
| Parkes targets | ||||||
| IRAS 00483−7347 | 660.0 | 307 | 71 | 3.7 | 3.6 per cent | 97.7 per cent |
| IRAS F00486−7308 | 91.1 | 39 | 9 | 4.5 | 34.5 per cent | 40.7 per cent |
| IRAS 00591−7307 | 95.4 | 44 | 10 | 7.7 | 52.1 per cent | 23.3 per cent |
| IRAS 01074−7140 | 396.0 | 235 | 54 | 3.4 | 4.3 per cent | 97.7 per cent |
| ATCA sources | ||||||
| OGLE SMC-LPV-15504 | 31.6 | 13 | 3 | 7.1 | 158.9 per cent | 5.8 per cent |
| 2MASS J01033142−7214072 | 19.2 | 8 | 1 | 6.3 | ||
| HV 12149 | 12.7 | 7 | 2 | 6.5 | 278.0 per cent | 1.2 per cent |
| OGLE SMC-LPV-14322 | 19.0 | 11 | 3 | 7.6 | ||
| 2MASS J00592646−7223417 | 18.9 | 13 | 3 | 6.5 | ||
| BMB-B75 | 92.0 | 43 | 10 | 9.5 | 66.5 per cent | 19.7 per cent |
| OGLE J004942.72−730220.4 | 27.8 | 14 | 3 | 10.0 | ||
| MSX SMC 018 | 262.0 | 116 | 27 | 7.2 | 18.7 per cent | 67.5 per cent |
The flux density upper limits for circumstellar OH maser emission for our SMC sample. Listed values are Spitzer MIPS 24 μm flux (F24) from Boyer et al. (2011), predicted 35 μm flux values taken from the best-fitting dusty model of the source (explained in Section 4.5), predicted OH maser flux (FOH,predicted) assuming our median masing efficiency of 23 per cent F35 photons to FOH photons, and the noise level (σ) of the observation (both combined observations for IRAS 00483−7347. Also shown are the upper limits for maser efficiency (maximum efficiency) and the probability of a 3σ-level detection for each targeted observation calculated with our bootstrapping method using the maser efficiencies of the LMC and Galactic samples from Goldman et al. (2017).
| Object . | F24μm . | F35μm, predicted . | FOH,predicted . | σ . | Maximum . | Likelihood . |
|---|---|---|---|---|---|---|
| name . | (mJy) . | (mJy) . | (mJy) . | (mJy) . | efficiency . | of detection . |
| Parkes targets | ||||||
| IRAS 00483−7347 | 660.0 | 307 | 71 | 3.7 | 3.6 per cent | 97.7 per cent |
| IRAS F00486−7308 | 91.1 | 39 | 9 | 4.5 | 34.5 per cent | 40.7 per cent |
| IRAS 00591−7307 | 95.4 | 44 | 10 | 7.7 | 52.1 per cent | 23.3 per cent |
| IRAS 01074−7140 | 396.0 | 235 | 54 | 3.4 | 4.3 per cent | 97.7 per cent |
| ATCA sources | ||||||
| OGLE SMC-LPV-15504 | 31.6 | 13 | 3 | 7.1 | 158.9 per cent | 5.8 per cent |
| 2MASS J01033142−7214072 | 19.2 | 8 | 1 | 6.3 | ||
| HV 12149 | 12.7 | 7 | 2 | 6.5 | 278.0 per cent | 1.2 per cent |
| OGLE SMC-LPV-14322 | 19.0 | 11 | 3 | 7.6 | ||
| 2MASS J00592646−7223417 | 18.9 | 13 | 3 | 6.5 | ||
| BMB-B75 | 92.0 | 43 | 10 | 9.5 | 66.5 per cent | 19.7 per cent |
| OGLE J004942.72−730220.4 | 27.8 | 14 | 3 | 10.0 | ||
| MSX SMC 018 | 262.0 | 116 | 27 | 7.2 | 18.7 per cent | 67.5 per cent |
| Object . | F24μm . | F35μm, predicted . | FOH,predicted . | σ . | Maximum . | Likelihood . |
|---|---|---|---|---|---|---|
| name . | (mJy) . | (mJy) . | (mJy) . | (mJy) . | efficiency . | of detection . |
| Parkes targets | ||||||
| IRAS 00483−7347 | 660.0 | 307 | 71 | 3.7 | 3.6 per cent | 97.7 per cent |
| IRAS F00486−7308 | 91.1 | 39 | 9 | 4.5 | 34.5 per cent | 40.7 per cent |
| IRAS 00591−7307 | 95.4 | 44 | 10 | 7.7 | 52.1 per cent | 23.3 per cent |
| IRAS 01074−7140 | 396.0 | 235 | 54 | 3.4 | 4.3 per cent | 97.7 per cent |
| ATCA sources | ||||||
| OGLE SMC-LPV-15504 | 31.6 | 13 | 3 | 7.1 | 158.9 per cent | 5.8 per cent |
| 2MASS J01033142−7214072 | 19.2 | 8 | 1 | 6.3 | ||
| HV 12149 | 12.7 | 7 | 2 | 6.5 | 278.0 per cent | 1.2 per cent |
| OGLE SMC-LPV-14322 | 19.0 | 11 | 3 | 7.6 | ||
| 2MASS J00592646−7223417 | 18.9 | 13 | 3 | 6.5 | ||
| BMB-B75 | 92.0 | 43 | 10 | 9.5 | 66.5 per cent | 19.7 per cent |
| OGLE J004942.72−730220.4 | 27.8 | 14 | 3 | 10.0 | ||
| MSX SMC 018 | 262.0 | 116 | 27 | 7.2 | 18.7 per cent | 67.5 per cent |
This PDF is available to Subscribers Only
View Article Abstract & Purchase OptionsFor full access to this pdf, sign in to an existing account, or purchase an annual subscription.
