Table 8
Confidence interval of the giant planet frequency of with a confidence level of 68% reported in this work around young, nearby and dusty A-F stars assuming different planet populations, the detections of β Pictoris b, and the system around HR 8799 for planets, and the detection of HR 7329 b as brown dwarf.
| Sep. range | Mass range | Frequency | Distribution |
| (AU) | (MJ) | (%) | |
|
|
|||
| A-F sample | |||
| [1,1000] | [1,13] | 10.8−24.8 | flat |
| [1,1000] | [1,13] | 14.8−36.8 | Cu08 |
| [1,1000] | [1,75] | 2.2−5.4 | flat+GI |
|
|
|||
| A-F dusty sample | |||
| [1,1000] | [1,13] | 14.3−35.2 | flat |
| [1,1000] | [1,13] | 18.7−47.9 | Cu08 |
| [1,1000] | [1,75] | 2.9−6.7 | flat+GI |
Notes. Results on the frequency of giant planets are reported according to a flat/uniform giant planet distribution or to a power law distribution of giant planets with the mass and semi-major axis (Cumming et al. 2008) or driven by formation boundaries according to the gravitational instability scenario. The first two scenarii consider the detections of two planetary systems, whereas the later set with one brown dwarf detection since planet formation through GI remains very low because they are not allowed to form closer-in and become too massive farther out.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.