Table 3
Comparison of observed H2O, CO, and OH line ratios with literature values.
| Object | 212−101/16−15 | 404−313/24−23 | 16−15/24−23 | 212−101/404−313 | 221−110/404−313 | OH 84/79 | Ref. | |
|
|
||||||||
| Perseus (this work) | ||||||||
| Perseus | 0.2–2.4 | 0.2–1.1 | 1.2–4.6 | 1.3–6.3 | 1.4–5.5 | 1.1–2.4 | This work | |
|
|
||||||||
| On–source (literature) | ||||||||
| SMM3 b | 1.0 ± 0.1 | 0.5 ± 0.2 | 3.3 ± 0.8 | 7.1 ± 1.0 | 3.7 ± 1.0 | 1.4 ± 0.7 | (1) | |
| c | 0.9 ± 0.2 | 0.9 ± 0.3 | 4.6 ± 1.0 | 4.9 ± 1.0 | 2.3 ± 0.8 | 2.4 ± 1.2 | (1) | |
| r | 1.0 ± 0.1 | 2.0 ± 0.7 | 9.4 ± 2.3 | 4.7 ± 1.0 | 3.1 ± 0.9 | n.d. | (1) | |
| SMM4 r | 0.8 ± 0.1 | 0.4 ± 0.1 | 3.6 ± 0.6 | 7.8 ± 1.6 | 3.0 ± 1.3 | 1.1 ± 0.5 | (1) | |
| L1448-MM | 2.3 ± 1.3 | 1.2 ± 0.7 | 2.1 ± 1.2 | 4.1 ± 2.3 | 2.6 ± 1.5 | 1.4 ± 0.9 | (2) | |
| NGC 1333 I4B | 1.0 ± 0.1 | 1.0 ± 0.1 | 1.9 ± 0.1 | 1.9 ± 0.1 | 2.0 ± 0.1 | 1.2 ± 0.2 | (3) | |
|
|
||||||||
| Off–source (literature) | ||||||||
| L1157 B1 | 4.0 ± 0.5 | – | – | 11.0 | 2.9 ± 1.2 | n.d. | (4, 5) | |
| B1′ | 2.1 ± 0.2 | – | – | 9.2 ± 2.2 | 2.8 ± 1.0 | 0.9 ± 0.5 | (4, 5) | |
| B2 | 17.0 ± 8.4 | n.d. | >0.3 | > 7.7 | n.d. | – | (6) | |
| R | 5.3 ± 2.4 | >0.26 | >0.5 | 10.6 ± 4.7 | 1.8 ± 0.8 | – | (6) | |
| L1448 B2 | 2.3 ± 0.4 | 0.4 ± 0.3 | 2.8 ± 0.9 | 15.0 ± 6.5 | 3.7 ± 1.6 | – | (6) | |
| R4 | 8.2 ± 3.0 | >0.3 | >0.9 | 23.2 ± 9.7 | 3.3 ± 1.2 | – | (6) | |
Notes. Sources in the upper part of the table refer to protostellar positions within the PACS maps, sources in the lower part refer to shock positions away from the protostar. Ranges of line ratios calculated for Perseus sources are listed at the top. Line ratios of sources that exceed the Perseus values are shown in boldface. The L1157 B1′ position refers to the high-excitation CO emission peak close to the nominal position of the B1 shock spot (Benedettini et al. 2012). Non-detections are abbreviated with n.d. OH 84/79 refers to the ratio of two OH doublets, at 84 and 79 μm, respectively. The total flux of the 84 μm doublet is calculated by multiplying the 84.6 μm flux by two, because of the blending of the 84.4 μm line with the CO 31−30 line.
Reference. (1) Dionatos et al. (2013); (2) Lee et al. (2013); (3) Herczeg et al. (2012); (4) Benedettini et al. (2012); (5) Busquet et al. (2014); (6) Santangelo et al. (2013).
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