Table C.1
Transition disks with a quantified gas density drop inside the dust cavity.
| Star | Rcav dust | δdust | λ | Ref. | Rcav gas | δgas | Σgas inner | g/d outer | Gas tracers | Ref. | Ṁ | Ref. |
| [au] | [au] | [g cm-2] | [M⊙ yr-1] | |||||||||
|
|
||||||||||||
| HD 139614 | 6 | 10-4 | near-IR, mid-IR | 1 | 5−6 | 10-2−10-4 | 7 × 10-5−2.4 × 10-3 | 1–100 | 12CO, 13CO, C18O ro-vib. | this work | 1 × 10-8 | 8 |
| sub-mm | ||||||||||||
| RXJ1615-3255 | 20 | 10-6 | sub-mm | 2 | 20 | >10-4 | 5 × 100−1 × 10-1 | 100 | 12CO sub-mm | 2 | 3.2 × 10-9 | 9 |
| SR21 | 25 | 10-6 | sub-mm | 3 | 25 | 5 × 10-2 | 1 × 101−1 × 100 | 100 | 12CO, 13CO sub-mm | 3 | 1.3 × 10-8 | 9 |
| 7 | ≤ 10-5 | 1 × 10-1−1 × 10-2 | ||||||||||
| DoAr 44 | 32 | 10-2 | sub-mm | 3 | 32 | 10-2 | 5 × 10-1−1 × 10-1 | 100 | 12CO, 13CO sub-mm | 3 | 6.3 × 10-9 | 9 |
| 16 | ≤ 10-4 | 1 × 10-2−5 × 10-4 | ||||||||||
| HD 135344 B | 30, 45 | 10-2 | near-IR, sub-mm | 4, 5, 6 | 45 | 10-1 | 1 × 10-2−2 × 10-2 | 4 | 12CO ro-vib. & sub-mm | 6a | 2 × 10-8 | 10 |
| [OI] 63 μm | ||||||||||||
| HD 135344 B | 40 | 2 × 10-4 | sub-mm | 5, 3 | 30 | 2 × 10-4 | 7 × 10-1−2 × 10-2 | 80 | 12CO, 13CO sub-mm | 3a | 2 × 10-8 | 10 |
| LkCa 15 | 45 | 10-5 | sub-mm | 2 | 45 | 10-1 | 1 × 103−1 × 101 | 100 | 12CO sub-mm | 2 | 4 × 10-9 | 9 |
| IRS 48 | 60 | 10-3 | sub-mm | 3 | 25 | ≤ 10-3 | 1 × 10-2−5 × 10-4 | 12 | 12CO, 13CO sub-mm | 3 | 3.2 × 10-9 | 11 |
| J1604-2130 | 70 | 10-1 | sub-mm | 2 | 30 | 10-5 | 1 × 10-2−1 × 10-4 | 100 | 12CO sub-mm | 2 | <10-11 | 12 |
| HD 142527b | 130 | 10-5 | sub-mm | 7 | 90 | 2 × 10-2 | 1 × 102−4 × 100 | 100 | 12CO, 13CO, C18O sub-mm | 7 | 2 ± 1 × 10-7 | 13 |
Notes. Rcav dust is the dust cavity radius resolved by near-IR or sub-mm observations. When two values appear, the first corresponds to the small dust particles in the near-IR and the second to the large dust grains in the sub-mm. Rcav gas is the reference radius for the drop in the gas surface density. An additional Rcav gas is given if a second drop in the gas surface density is suggested in the literature. Σgas inner is generally described as a power-law, the interval of values given correspond to Σgas inner at the inner disk’s radius Rin, and at Rcav gas. If two drops for the surface density are suggested in the literature, two intervals for the surface density in the inner disk are given.
Two models are available in the literature for HD 135344B. Although they have dust mass estimations similar within a factor 2 (1–2 × 10-4 M⊙) the gas mass and gas surface density in the outer disk differ. Carmona et al. (2014) find a gas-to-dust mass ratio of 4 and a gas mass of 8 × 10-4 M⊙ for the outer disk, van der Marel et al. (2016) find a gas-to-dust mass ratio of 80 and a gas mass of 1.5 × 10-2 M⊙. Both models also used a different disk outer radius, 200 AU in Carmona et al. (2014) and 125 AU in van der Marel et al. (2016);
δdust was calculated from the surface density profile provided by Perez et al. (2015), using a gas-to-dust mass of 100 at R > 130 AU, such that the dust mass between 0.2 and 6 AU is 10-9 M⊙ as reported by the same authors.
Reference. (1) Matter et al. (2016); (2) van der Marel et al. (2015b); (3) van der Marel et al. (2016); (4) Andrews et al. (2011); (5) Muto et al. (2012); (6) Carmona et al. (2014); (7) Perez et al. (2015); (8) Garcia Lopez et al. (2006); (9) Manara et al. (2014); (10) Sitko et al. (2012); (11) Follette et al. (2015); (12) Mathews et al. (2012); (13) Mendigutía et al. (2014).
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