WEIRD: Wide-orbit Exoplanet Search with InfraRed Direct Imaging

Baron, Frédérique; Artigau, Étienne; Rameau, Julien; Lafrenière, David; Gagné, Jonathan; Malo, Lison; Li, Albert; Naud, Marie-Ève; Doyon, René; Janson, Markus; Delorme, P.; Beichman, Charles

doi:10.3847/1538-3881/aad599

Cited by 16 publications

(27 citation statements)

References 124 publications

(195 reference statements)

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“…HD 25284B was flagged as 0.5" binary in WDS from Tycho, but this companion was not retrieved in our SPHERE observations (Langlois et al 2021) and then the target was kept in the SHINE statistical analysis as an isolated object. Nothing found at large separation by WEIRD (Baron et al 2018). The companion we found around the primary of this system is a new discovery.…”

Section: Idmentioning

confidence: 51%

New binaries from the SHINE survey

Bonavita,

Gratton,

Desidera

et al. 2021

Preprint

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We present the multiple stellar systems observed within the SpHere INfrared survey for Exoplanet (SHINE). SHINE searched for substellar companions to young stars using high contrast imaging. Although stars with known stellar companions within SPHERE field of view (< 5.5 arcsec) were removed from the original target list, we detected additional stellar companions to 78 of the 463 SHINE targets observed so far. 27% of the systems have three or more components. Given the heterogeneity of the sample in terms of observing conditions and strategy, tailored routines were used for data reduction and analysis, some of which were specifically designed for these data sets. We then combined SPHERE data with literature and archival ones, TESS light curves and Gaia parallaxes and proper motions, to characterise these systems as completely as possible. Combining all data, we were able to constrain the orbits of 25 systems. We carefully assessed the completeness of our sample for the separation range 50-500 mas (period range a few years -a few tens of years), taking into account the initial selection biases and recovering part of the systems excluded from the original list due to their multiplicity. This allowed us to compare the binary frequency for our sample with previous studies and highlight some interesting trends in the mass ratio and period distribution. We also found that, for the few objects for which such estimate was possible, the values of the masses derived from dynamical arguments were in good agreement with the model predictions. Stellar and orbital spins appear fairly well aligned for the 12 stars having enough data, which favour a disk fragmentation origin. Our results highlight the importance of combining different techniques when tackling complex problems such as the formation of binaries and show how large samples can be useful for more than one purpose.

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Section: Idmentioning

confidence: 51%

New binaries from the SHINE survey

Bonavita,

Gratton,

Desidera

et al. 2021

Preprint

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“…Stamatellos et al 2007aStamatellos et al , 2011Stamatellos & Whitworth 2009b). Observational surveys indicate that only a small fraction of M dwarfs (less than ∼10%) host wide orbit planets and this also holds for higher-mass stars (Brandt et al 2014;Bowler et al 2015;Lannier et al 2016;Reggiani et al 2016;Galicher et al 2016;Bowler 2016;Vigan et al 2017;Baron et al 2018;Stone et al 2018;Wagner et al 2019;Nielsen et al 2019) (see review by Bowler & Nielsen 2018). These surveys typically explore a region out to a few hundred AU from the central star (or even a few thousand AU, Durkan et al 2016;Naud et al 2017) and they are sensitive down to Jupiter-mass planets.…”

Section: Introductionmentioning

confidence: 99%

Planet formation around M dwarfs via disc instability

Mercer

Stamatellos

2020

A&A

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Context. Around 30 per cent of the observed exoplanets that orbit M dwarf stars are gas giants that are more massive than Jupiter. These planets are prime candidates for formation by disc instability. Aims. We want to determine the conditions for disc fragmentation around M dwarfs and the properties of the planets that are formed by disc instability. Methods. We performed hydrodynamic simulations of M dwarf protostellar discs in order to determine the minimum disc mass required for gravitational fragmentation to occur. Different stellar masses, disc radii, and metallicities were considered. The mass of each protostellar disc was steadily increased until the disc fragmented and a protoplanet was formed. Results. We find that a disc-to-star mass ratio between ~0.3 and ~0.6 is required for fragmentation to happen. The minimum mass at which a disc fragment increases with the stellar mass and the disc size. Metallicity does not significantly affect the minimum disc fragmentation mass but high metallicity may suppress fragmentation. Protoplanets form quickly (within a few thousand years) at distances around ~50 AU from the host star, and they are initially very hot; their centres have temperatures similar to the ones expected at the accretion shocks around planets formed by core accretion (up to 12 000 K). The final properties of these planets (e.g. mass and orbital radius) are determined through long-term disc-planet or planet–planet interactions. Conclusions. Disc instability is a plausible way to form gas giant planets around M dwarfs provided that discs have at least 30% the mass of their host stars during the initial stages of their formation. Future observations of massive M dwarf discs or planets around very young M dwarfs are required to establish the importance of disc instability for planet formation around low-mass stars.

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“…Durkan et al (2016) find companions with 0.5-13 M Jup at separations of 100-1000 au occur with an upper frequency limit of 9% based on a sample of 121 stars. Baron et al (2018) probe further separations of 1000-5000 au in their 177 star sample, finding an occurrence rate of < 3% for 1-13 M Jup companions. As mentioned previously, both surveys searched for wide companion systems in young moving groups that are closer (< 100 pc) and older (> 10 Myr) than the regions from which our target sample was created.…”

Section: Optimizing the Search For Wide Pmcs With Spitzermentioning

confidence: 87%

“…Note that the remaining residuals appear similar to the noise near the primary star, indicating a good fit. recently, Baron et al (2018) reported first results from the Wide-orbit Exoplanet search with InfraRed Direct Imaging (WEIRD) survey constraining the occurrence of Jupiter-like companions on orbits between 1000 and 5000 au. These studies focused their investigations on regions closer (d < 100 pc) and older (τ > 10 Myr) than the regions we analyze in this work (d > 100 pc; τ < 10 Myr).…”

Section: Discussionmentioning

confidence: 99%

Searching for Wide Companions and Identifying Circum(sub)stellar Disks through PSF Fitting of Spitzer/IRAC Archival Images

Martinez

Kraus

2019

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Direct imaging surveys have discovered wide-orbit planetary-mass companions that challenge existing models of both star and planet formation, but their demographics remain poorly sampled. We have developed an automated binary companion point spread function (PSF) fitting pipeline to take advantage of Spitzer 's infrared sensitivity to planetary-mass objects and circum(sub)stellar disks, measuring photometry across the four IRAC channels of 3.6 µm, 4.5 µm, 5.8 µm, and 8.0 µm. We present PSFfitting photometry of archival Spitzer /IRAC images for 11 young, low-mass (M ∼ 0.044-0.88 M ; M7.5-K3.5) members of three nearby star-forming regions (Chameleon, Taurus, and Upper Scorpius; d ∼150 pc; τ ∼1-10 Myr) that host confirmed or candidate faint companions at ρ = 1. 68 − 7. 31. We recover all system primaries, six confirmed, and two candidate low-mass companions in our sample. We also measure non-photospheric [3.6] − [8.0] colors for three of the system primaries, four of the confirmed companions, and one candidate companion, signifying the presence of circumstellar or circum(sub)stellar disks. We furthermore report the confirmation of a ρ = 4. 66 (540 au) companion to [SCH06] J0359+2009 which was previously identified as a candidate via imaging over five years ago, but was not studied further. Based on its brightness (M [3.6] = 8.53 mag), we infer the companion mass to be M = 20 ± 5 M Jup given the primary's model-derived age of 10 Myr. Our framework is sensitive to companions with masses less than 10 M Jup at separations of ρ = 300 AU in nearby star-forming regions, opening up a new regime of parameter space that has yet to be studied in detail, discovering planetary-mass companions in their birth environments and revealing their circum(sub)stellar disks.

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WEIRD: Wide-orbit Exoplanet Search with InfraRed Direct Imaging

Cited by 16 publications

References 124 publications

New binaries from the SHINE survey

New binaries from the SHINE survey

Planet formation around M dwarfs via disc instability

Searching for Wide Companions and Identifying Circum(sub)stellar Disks through PSF Fitting of Spitzer/IRAC Archival Images

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