Table A.3
Additional planets published in planetary systems.
| Name | Periodp [d] | m sin(i)p [M⊕] | Detection limit [M⊕] | Reference paper | Data used |
|---|---|---|---|---|---|
| GJ 180 c | 24.3 | 6.4 | 7.2 | Tuomi et al. (2014) | HARPS + UVES |
| d | 106 | 7.6 | 10.5 | Tuomi et al. (2014) | HARPS + UVES |
| GJ 433 c | 5100 | 32 | 56.7 | Tuomi et al. (2014) | HARPS + UVES |
| d | 36 | 5 | 8.2 | Feng et al. (2020) | HARPS + VLT2 |
| GJ 676A c | 13000 | 4288 | − | Sahlmann et al. (2016) | Astrometry + RV |
| Feng et al. (2022) | |||||
| d* | 3.6 | 3.8 | 7.3 | Anglada-Escudé & Tuomi (2012) | HARPS |
| e* | 35 | 6.7 | 18.4 | Anglada-Escudé & Tuomi (2012) | HARPS |
| GJ 849 c | 5990 | 315 | >103 | Montet et al. (2014) Pinamonti et al. (2023) |
RV + direct imaging |
| GJ 876 e | 124 | 14.6 | 18.5 | Rivera et al. (2010) Montet et al. (2014) |
Keck/Hires |
| GJ 3053 c | 3.8 | 1.7 | 1.9 | Ment et al. (2019) | transit + RV |
| GJ 3293 e | 13 | 3 | 4.1 | Astudillo-Defru et al. (2017a) | HARPS |
Notes. Additional planets not detected in the planetary systems used and detailed in Tab. A.2. Periodp and M.sin(i)p are the planetary parameters published in the reference paper, Detection limits are the average value of the detection limit in the domain of period of the period published computed in this study, and the Data used correspond to the method/data used to detect the additionnai planet in the system. *GJ 676 d and e are found using the same HARPS data set as Anglada-Escudé & Tuomi (2012) obtained before 2011, but not with the new full data set.
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.