Issue |
A&A
Volume 693, January 2025
|
|
---|---|---|
Article Number | A54 | |
Number of page(s) | 23 | |
Section | Planets, planetary systems, and small bodies | |
DOI | https://doi.org/10.1051/0004-6361/202452310 | |
Published online | 03 January 2025 |
The COBREX archival survey: Improved constraints on the occurrence rate of wide-orbit substellar companions
I. A uniform re-analysis of 400 stars from the GPIES survey
1
LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université,
Université Paris Cité, 5 place Jules Janssen,
92195
Meudon,
France
2
Univ. Grenoble Alpes, CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) UMR 5274,
Grenoble
38041,
France
3
Centre de Recherche Astrophysique de Lyon (CRAL) UMR 5574, CNRS, Univ. de Lyon,
Univ. Claude Bernard Lyon 1, ENS de Lyon,
69230
Saint-Genis-Laval,
France
★ Corresponding author; vito.squicciarini@obspm.fr
Received:
19
September
2024
Accepted:
7
November
2024
Context. Direct imaging (DI) campaigns are uniquely suited to probing the outer regions around young stars in pursuit of giant exoplanet and brown dwarf companions, providing key complementary information to radial velocity (RV) and transit searches for demographic studies. However, the critical 5–20 au region, where most giant planets are thought to form, remains poorly explored, as it lies between current RV and DI capabilities.
Aims. Significant gains in detection performances can be attained at no instrumental cost by means of advanced post-processing techniques. In the context of the COBREX project, we have assembled the largest collection of archival DI observations to date with the aim of undertaking a large and uniform reanalysis. In particular, this paper details the reanalysis of 400 stars from the Gemini Planet Imager Exoplanet Survey (GPIES) operated at GPI@Gemini South.
Methods. Following the prereduction of raw frames, the GPI data cubes were processed by means of the PACO algorithm. Candidates were identified and vetted based on multi-epoch proper motion analysis (whenever possible) and by means of a suitable color-magnitude diagram. The conversion of detection limits into detectability maps allowed us to estimate the unbiased occurrence frequencies of giant planets and brown dwarfs.
Results. We derived deeper detection limits than those reported in the literature, with up to a two-fold gain in minimum detectable mass, compared to previous GPI-based publications. Although no new substellar companion was confirmed, we identified two interesting planet candidates awaiting follow-up observations. We derived an occurrence rate of 1.7−0.7+0.9% for 5 MJup < m < 13 MJup planets in 10 au < a < 100 au. This rises to 2.2−0.8+1.0% when including substellar objects up to 80 MJup. Our results are in line with the literature, but with lower uncertainties, thanks to the enhanced detection sensitivity. We confirm, as hinted at by previous studies, a more frequent occurrence of giant planets around BA hosts compared to FGK stars. Moreover, we tentatively observe a smaller occurrence of brown dwarf companions around BA stars, although larger samples are needed to shed light on this point.
Conclusions. While awaiting the wealth of data anticipated from future instrument and facilities, valuable information can still be extracted from existing data. In this regard, a complete reanalysis of SPHERE and GPI data is expected to provide the most precise demographic constraints ever provided by direct imaging.
Key words: techniques: high angular resolution / planets and satellites: detection / planets and satellites: gaseous planets / brown dwarfs
© The Authors 2025
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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