Table 1
Observational parameters for our sample of debris disks.
| Name | LSR velocity | LIR/L⋆ | Ref. | 3σint | MH2 DiskFit | MH2 from SCO |
| (km s-1) | (Jy km s-1) | (3σ upp. limit) M⊕ | (3σ upp. limit) M⊕ | |||
|
|
||||||
| IRAM-30 m – CO J = 2 → 1 | ||||||
|
|
||||||
| HD 2772 | –5.4 | 8.2 × 10-6 | 1 | <0.569 | <0.110 | <0.454 |
| HD 14055 | 7.5 | 6.7 × 10-5 | 1 | <0.387 | <0.008 | <0.027 |
| HD 15115 | –0.2 | 4.8 × 10-4 | 2 | <1.89 | <0.063 | <0.229 |
| HD 21620 | –22.8 | 2.51 × 10-5 | 3 | <0.622 | <0.383 | <0.819 |
| HD 23642 | –4.0 | 2.2 × 10-5 | 1 | 0.71 ± 0.18 | 0.18 ± 0.04 | 0.57 ± 0.14 |
| HD 31295 | –3.5 | 4.7 × 10-5 | 1 | <0.768 | <0.016 | <0.058 |
| HD 42111 | 8.4 | 1.00 × 10-5 | 3 | <0.902 | <1.02 | <2.16 |
| HD 159082 | 7.1 | 5.7 × 10-5 | 1 | <0.497 | <0.132 | <0.537 |
| HD 218396 | –12.6 | 2.29 × 10-4 | 4 | <0.349 | <0.005 | <0.032 |
|
|
||||||
| APEX – CO J = 3 → 2 | ||||||
|
|
||||||
| HD 225200 | 13.4 | 7.4 × 10-5 | 1 | <3.15 | <0.260 | <0.470 |
| HD 17848 | 16.7 | 4.8 × 10-5 | 1 | <10.5 | <0.146 | <0.242 |
| HD 24966 | 11.7 | 3.1 × 10-4 | 1 | <2.85 | <0.166 | <0.278 |
| HD 30422 | –4.8 | 3.7 × 10-5 | 1 | <2.22 | <0.036 | <0.063 |
| HD 35850 | 1.4 | 2.3 × 10-5 | 1 | <2.26 | <0.007 | <0.015 |
| HD 38206 | 5.8 | 1.4 × 10-4 | 1 | <2.78 | <0.062 | <0.119 |
| HD 54341 | 20.0∗ | 1.9 × 10-4 | 1 | <2.49 | <0.106 | <0.232 |
| HD 71043 | 5.9 | 6.5 × 10-5 | 1 | <2.74 | <0.073 | <0.131 |
| HD 71155 | –4.7 | 4.2 × 10-5 | 1 | <2.66 | <0.017 | <0.035 |
| HD 78072 | 2.5 | 2.5 × 10-4 | 1 | <2.11 | <0.071 | <0.133 |
| HD 136246 | 4.2 | 4.9 × 10-5 | 1 | <2.47 | <0.281 | <0.459 |
| HD 164249 | 2.5 | 7.2 × 10-4 | 1 | <2.38 | <0.020 | <0.049 |
| HD 166191 | 3.8 | 1.0 × 10-1 | 5 | <2.77 | <0.187 | <0.351 |
| HD 181296 | 14.3 | 2.4 × 10-4 | 1 | <2.19 | <0.014 | <0.046 |
| HD 182681 | 10.5 | 1.95 × 10-4 | 4 | <2.91 | <0.083 | <0.124 |
| HD 220825 | –1.5 | 2.9 × 10-5 | 1 | <2.29 | <0.011 | <0.046 |
Notes. Stars in italics are systems with earlier detection limits in one CO transition, see Sect. 2.1. The last three colums show the 3σ upper limits derived from our study: on the integrated intensity of CO, the H2 mass derived from DiskFit model and the H2 mass directly derived from the integrated flux. The integrated flux and the H2 masses for the tentative detection around HD 23642 are also displayed.
Reference. For LIR/L⋆: 1 – Chen et al. (2014); 2 – Moór et al. (2011); 3 – Roberge & Weinberger (2008); 4 – Rhee et al. (2007); 5 – Schneider et al. (2013).
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