Table 2
Integrated fluxes in Jy km s−1 and radii in au of 12CO, 13CO, and C18O.
12CO |
13CO |
C18O |
|||||||
---|---|---|---|---|---|---|---|---|---|
Name | Flux | Rgas, 68% | Rgas, 90% | Flux | Rgas, 68% | Rgas, 90% | Flux | Rgas, 68% | Rgas, 90% |
(Jy km s−1) | (au) | (au) | (Jy km s−1) | (au) | (au) | (Jy km s−1) | (au) | (au) | |
AB Aur | 52.35 ± 0.30* | 232 ± 12 | 358 ± 12 | 37.01 ± 0.18 | 690 ± 35 | 1118 ± 35 | 7.50 ± 0.11 | 370 ± 35 | 678 ± 40 |
AK Sco | 2.18 ± 0.05 | 78 ± 4 | 114 ± 5 | 0.68 ± 0.04 | 66 ± 6 | 97 ± 18 | 0.27 ± 0.02 | 52 ± 5 | 69 ± 11 |
BH Cep | – | – | – | <0.07 | – | – | <0.07 | – | – |
BO Cep | – | – | – | 1.22 ± 0.08 | <387 | <525 | 0.35 ± 0.07 | <371 | <529 |
CQ Tau | 3.44± 0.04 | 103 ± 3 | 146 ± 3 | 1.12 ± 0.04 | 84 ± 5 | 113 ± 6 | 0.60 ± 0.02 | 65 ± 4 | 99 ± 7 |
HD 9672 | 3.61 ± 0.08 | <285 | <460 | 1.37 ± 0.08 | <285 | <439 | 0.12 ± 0.04 | <231 | <347 |
HD 31648 | 19.97 ± 0.08 | 389 ± 36 | 597 ± 36 | 7.03 ± 0.08 | 313 ± 38 | 467 ± 38 | 2.16 ± 0.05 | 237 ± 38 | 363 ± 38 |
HD 34282 | 9.47 ± 0.09 | 468 ± 17 | 673 ± 17 | 3.46 ± 0.05 | 340 ± 18 | 483 ± 18 | 1.89 ± 0.04 | 324 ± 18 | 568 ± 40 |
HD 36112 | 7.98 ± 0.14 | 211 ± 6 | 305 ± 12 | 1.87 ± 0.07 | 121 ± 9 | 192 ± 18 | 0.78 ± 0.04 | 103 ± 6 | 141 ± 15 |
HD 58647 | <0.03 | – | – | <0.02 | – | – | <0.02 | – | – |
HD 97048 | 27.40 ± 0.14 | 389 ± 45 | 596 ± 45 | 15.93 ± 0.11 | 433 ± 48 | 615 ± 48 | 8.41 ± 0.08 | 366 ± 48 | 512 ± 48 |
HD 100453 | 2.40 ± 0.03 | 51 ± 5 | 78 ± 5 | 0.91 ± 0.02 | 38 ± 5 | 56 ± 5 | 0.37 ± 0.01 | 39 ± 5 | 59 ± 10 |
HD 100546 | 63.56 ± 0.12 | 230 ± 6 | 322 ± 6 | 13.13 ± 0.08 | 187 ± 6 | 256 ± 6 | 3.35 ± 0.06 | 127 ± 9 | 236 ± 16 |
HD 104237 | 2.43 ± 0.06 | <43 | <64 | 0.64 ± 0.03 | <39 | <59 | 0.37 ± 0.03 | <46 | <69 |
HD 135344B | 20.07 ± 0.18* | 158 ± 10 | 219 ± 10 | 8.86 ± 0.08* | 119 ± 9 | 171 ± 9 | 3.55 ± 0.08* | 86 ± 9 | 125 ± 9 |
HD 139614 | – | – | – | 2.82 ± 0.05 | <130 | <179 | 1.12 ± 0.04 | <108 | <151 |
HD 141569 | 18.43 ± 0.12* | 162 ± 9 | 220 ± 9 | 1.27 ± 0.13 | 150 ± 17 | 193 ± 54 | <0.07 | – | – |
HD 142527 | 27.14 ± 0.10 | 542 ± 30 | 793 ± 30 | 11.88 ± 0.07 | 334 ± 31 | 491 ± 31 | 3.91 ± 0.04 | 271 ± 31 | 368 ± 31 |
HD 142666 | 4.05 ± 0.03 | 136 ± 6 | 186 ± 6 | 1.51 ± 0.06 | <182 | <260 | 0.64 ± 0.04 | <164 | <236 |
HD 163296 | 51.99 ± 0.09 | 348 ± 13 | 496 ± 13 | 16.98 ± 0.07 | 287 ± 14 | 400 ± 14 | 5.96 ± 0.04 | 228 ± 14 | 324 ± 14 |
HD 169142 | 18.93 ± 0.05 | 232 ± 8 | 347 ± 8 | 6.37 ± 0.04 | 156 ± 9 | 230 ± 9 | 2.93 ± 0.02 | 129 ± 9 | 169 ± 9 |
HD 176386 | <0.11 | – | – | <0.10 | – | – | <0.07 | – | – |
HD 200775 | – | – | – | <0.09 | – | – | <0.08 | – | – |
HD 245185 | 2.37 ± 0.10 | <221 | <396 | – | – | – | – | – | – |
HD 290764 | 6.55 ± 0.13* | 271 ± 11 | 386 ± 14 | 2.95 ± 0.05* | 218 ± 17 | 328 ± 17 | 1.51 ± 0.05* | 188 ± 18 | 277 ± 23 |
HR 5999 | <0.08 | – | – | <0.08 | – | – | <0.06 | – | – |
KK Oph | – | – | – | <0.18 | – | – | <0.07 | – | – |
MWC 297 | <0.03 | – | – | <0.05 | – | – | <0.02 | – | – |
SV Cep | – | – | – | <0.08 | – | – | <0.08 | – | – |
TY CrA | <0.10 | – | – | <0.10 | – | – | <0.07 | – | – |
V718 Sco | – | – | – | 1.63 ± 0.09 | <106 | <151 | 0.86 ± 0.07 | <113 | <170 |
V892 Tau | 16.18 ± 1.87 | 171 ± 30 | 242 ± 126 | 3.92 ± 0.20 | 128 ± 9 | 191 ± 18 | 0.86 ± 0.10 | 90 ± 15 | 123 ± 43 |
VV Ser | <0.24 | – | – | – | – | – | – | – | – |
XY Per | – | – | – | <0.08 | – | – | <0.08 | – | – |
Z CMa | <0.11 | – | – | <0.06 | – | – | <0.03 | – | – |
Notes. The fluxes with an asterisk are for the J = 3−2 transition, all others are for the J = 2−1 transition. The upper limits are estimated by using three times the noise in a single channel and multiplying this by the width of the channel and the square root of the number of independent measurements, assuming that the emission is coming from a range of 10 km s−1 in velocity and within a single beam. The error on the flux is estimated by multiplying the noise in an empty channel by the width of the channel and the square root of the number of independent measurements in the Keplerian mask and the area over which the integrated fluxes were computed. All integrated fluxes have an additional 10% calibration error.
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