Table 2
List of planets for which spectro-polarimetric detection of H2O vapor is possible with g = 0.05.
| Planet | m∗(J) | d | Sp. type | Mp | Rp † | θp | ap | SL‡ |
|
|
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|
| (mag) | (pc) | (MJup) | (104 km) | (′′) | (AU) | (%) | (%) | |||||
|
|
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| 55 Cnc f | 4.6 | 12.3 | K0IV-V | 1.4E−01 | 5.6 (2) | 0.06 | 0.78 | in | 1.9 | 5 | 1.3 | 8 |
| 61 Vir d | 3.3 | 8.5 | G5V | 7.2E−02 | 3.8 (2) | 0.06 | 0.48 | in | 1.0 | 10 | 1.6 | 6 |
| Aldebaran b | –2.1 | 20.4 | K5III | 6.5E+00 | 7.3 (1) | 0.07 | 1.46 | in | 0.2 | 62 | 1.6 | 6 |
| GJ 682 c | 6.5 | 5.1 | M3.5V | 2.7E−02 | 2.3 (3) | 0.04 | 0.18 | in | 2.9 | 4 | 2.3 | 4 |
| §Gliese 876 b | 5.9 | 4.7 | M4V | 1.9E+00 | 4.1 (1) | 0.04 | 0.21 | in | 0.7 | 15 | 0.6 | 18 |
| §Gliese 876 e | 5.9 | 4.7 | M4V | 3.9E−02 | 3.0 (2) | 0.07 | 0.33 | out | 2.0 | 5 | 0.5 | 19 |
| §HD 113538 b | 6.4 | 15.8 | K9V | 3.6E−01 | 9.9 (2) | 0.08 | 1.24 | out | 2.9 | 3 | 0.5 | 20 |
| §HD 176051 b | 3.9 | 15.0 | 1.5E+00 | 8.5 (1) | 0.12 | 1.76 | ? | 1.7 | 6 | 0.8 | 13 | |
| HD 192310 c | 4.1 | 8.8 | K3V | 7.6E−02 | 4.2 (2) | 0.13 | 1.18 | in | 3.2 | 3 | 1.0 | 10 |
| HD 27442 b | 2.6 | 18.1 | K2IVa | 1.4E+00 | 6.0 (1) | 0.06 | 1.16 | in | 1.4 | 7 | 2.3 | 4 |
| HD 60532 c | 3.7 | 25.7 | F6IV-V | 7.5E+00 | 8.0 (1) | 0.06 | 1.58 | in | 2.6 | 4 | 3.0 | 3 |
| §HD 62509 b | –0.5 | 10.3 | K0IIIb | 2.9E+00 | 5.7 (1) | 0.16 | 1.69 | in | 0.4 | 28 | 0.8 | 12 |
| α Ari b | 0.1 | 20.2 | K2III | 1.8E+00 | 6.7 (1) | 0.06 | 1.20 | in | 0.4 | 24 | 2.7 | 4 |
| μ Ara d | 4.2 | 15.3 | G3IV-V | 5.2E−01 | 5.1 (1) | 0.06 | 0.92 | in | 2.8 | 4 | 2.7 | 4 |
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| Average | 3.5 | 13.2 | 1.8E+00 | 5.7 | 0.08 | 1.01 | 1.7 | 6 | 1.6 | 6 | ||
| Summary | Total: 14 | F:G:K:M = 1:2:7:3 | in:out = 11:2 | |||||||||
Notes..
The radii of all the listed planets are predicted from the mass. The figures in the parentheses represent the methods to estimate Rp: (1) adopts the mass-radius relation for Mp > 150 MEarth(0.47 MJup); (2) 10 MEarth(0.031 MJup) < Mp ≤ 150 MEarth; and (3) 4 MEarth(0.013 MJup) <Mp ≤ 10 MEarth. See text for details.
This column describes whether the planet is located inside or outside the snow line. The snow line distance is estimated by Eq. (17) in Ida & Lin (2005).
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