Table 3
Measured line fluxes (10-18 W m-2) from the central region around each source.
Transition | Eu/k | λ | IRAS2A | HH 46 | DK Cha |
(K) | (μm) | ||||
|
|||||
CO | |||||
14–13 | 581 | 186.00 | 73 | 52 | 207 |
15–14 | 663 | 173.63 | 112 | 221 | |
16–15 | 752 | 162.81 | 67 | 44 | 219 |
17–16 | 846 | 153.27 | 64 | 238 | |
18–17 | 945 | 144.78 | 80 | 58 | 245 |
19–18 | 1050 | 137.20 | 95 | ||
20–19 | 1160 | 130.37 | <51 | ||
21–20 | 1276 | 124.19 | <94 | ||
22–21 | 1397 | 118.58 | <53 | 35 | 186 |
23–22 | 1524 | 113.46 | 177 | 74 | 327 |
24–23 | 1657 | 108.76 | 62 | 26 | 200 |
27–26 | 2086 | 96.77 | 187 | ||
28–27 | 2240 | 93.35 | 140 | ||
29–28 | 2400 | 90.16 | <35 | 20 | 254 |
30–29 | 2565 | 87.19 | <50 | 18 | 147 |
31–30 | 2735 | 84.41 | 297 | 74 | 263 |
32–31 | 2911 | 81.81 | <33 | <33 | 163 |
33–32 | 3092 | 79.36 | <36 | <23 | 92 |
34–33 | 3279 | 77.06 | <122 | 234 | |
35–34 | 3471 | 74.89 | <29 | 209 | |
36–35 | 3669 | 72.84 | <131 | <24 | 129 |
37–36 | 3872 | 70.91 | <33 | 69 | |
38–37 | 4080 | 69.07 | <25 | 118 | |
|
|||||
H2O | |||||
221–212 | 194 | 180.49 | 77 | 6 | <23 |
212–101 | 114 | 179.53 | 105 | 7 | 33 |
303–212 | 197 | 174.62 | 101 | 10 | 89 |
322–313 | 297 | 156.19 | 109 | ||
313–202 | 205 | 138.53 | 105 | 8 | 69 |
404–313 | 320 | 125.35 | 58 | 4 | 38 |
533–524 | 725 | 113.95 | <33 | <6 | <31 |
414–303 | 3234 | 113.54 | 177 | 74 | 327 |
743–734 | 1340 | 112.51 | 34 | ||
221–110 | 194 | 108.07 | 237 | 13 | <74 |
744–735 | 1335 | 90.05 | <33 | <5 | <63 |
322–211 | 297 | 89.99 | 97 | <5 | <63 |
716–707 | 1013 | 84.77 | <29 | <7 | <45 |
606–515 | 643 | 83.28 | 182 | <51 | |
835–744 | 1511 | 81.69 | <28 | <6 | <126 |
927–918 | 1729 | 81.40 | <29 | <5 | <125 |
423–312 | 432 | 78.74 | 38 | <7 | <86 |
321–212 | 305 | 75.38 | 126 | <87 | |
937–928 | 1750 | 73.61 | 158 | <126 | |
818–707 | 1071 | 63.32 | <39 | <11 | <177 |
Notes. Typical uncertainties are 30% for IRAS2A and DK Cha and 10 − 20% for HH 46. Upper limits are given at the 3σ level. Lines in italics are blended (CO 31 − 30 with an OH line) and their fluxes are treated as upper limits. Since the observations are compared with model images that are convolved with the Herschel point-spread function, the fluxes in this table are non-PSF-corrected.
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