Radial velocity survey for planets around young stars (RVSPY)

Zakhozhay, O. V.; Launhardt, R.; Trifonov, T.; Kürster, M.; Reffert, S.; Henning, Th.; Brahm, R.; Vines, José I.; Marleau, Gabriel-Dominique; Patel, J.

doi:10.1051/0004-6361/202244747

Cited by 11 publications

(6 citation statements)

References 45 publications

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“…In parallel with our work another study describing the discovery of this transiting planetary candidate appeared on arXiv (Zakhozhay et al 2022b). This study combines the constraints on the orbital period and planet mass from the TESS transit event in 2021 and RV data obtained from the 4-yr monitoring campaign of HD 114082 with the Fibre-fed Extended Range Échelle Spectrograph (FEROS) and publicly available spectra from the High Accuracy Radial velocity Planet Searcher (HARPS; Mayor et al 2003) archive.…”

Section: Discovery Of a Transiting Planetsupporting

confidence: 52%

“…The authors confirm the presence of a close-in giant planet in the system, which was assigned the identification name HD 114082 b. According to the analysis by Zakhozhay et al (2022b), the planet has a mass of 8.0 ± 1.0 M Jup and moves around the star on an eccentric orbit (e = 0.40 ± 0.04) with a semimajor axis of a = 0.51 ± 0.01 au and orbital period of 109.8 ± 0.4 days. The last two parameters are within 1σ-interval of our parameter values from the fitting of TESS light curve.…”

Section: Discovery Of a Transiting Planetmentioning

confidence: 85%

“…Two mass sensitivity maps were therefore created assuming the AMES-COND evolutionary model (Baraffe et al 2003), and used as input for MESS3. We also retrieved the archival HARPS and FEROS RV data of the target as described in Zakhozhay et al (2022b). We complemented that with the excess noise and proper motion anomaly from Gaia Data Release 3 (Gaia Collaboration 2021), with the technique described in Kiefer et al (in prep.).…”

Section: Companion Mass Sensitivity Limits Combining Direct Imaging R...mentioning

confidence: 99%

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The high-albedo, low polarization disk around HD 114082 that harbors a Jupiter-sized transiting planet

Engler

Milli

Gratton

et al. 2023

A&A

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Aims. We present new optical and near-infrared images of the debris disk around the F-type star HD 114082 in the Scorpius-Centaurus OB association. We obtained direct imaging observations and analyzed the TESS photometric time series data of this target with the goal of searching for planetary companions to HD 114082 and characterizing the morphology of the debris disk and the scattering properties of dust particles. Methods. HD 114082 was observed with the VLT/SPHERE instrument in different modes – the IRDIS camera in the K band (2.0–2.3 μm) together with the IFS in the Y, J, and H bands (0.95–1.66 μm) using the angular differential imaging technique as well as IRDIS in the H band (1.5–1.8 μm) and ZIMPOL in the I_PRIME band (0.71–0.87 μm) using the polarimetric differential imaging technique. To constrain the basic geometrical parameters of the disk and the scattering properties of dust grains, scattered light images were fitted with a 3D model for single scattering in an optically thin dust disk using a Markov chain Monte Carlo approach. We performed aperture photometry to derive the scattering and polarized phase functions, the polarization fraction, and the spectral scattering albedo for the dust particles in the disk. This method was also used to obtain the reflectance spectrum of the disk and, in turn, to retrieve the disk color and study the dust reflectivity in comparison to the debris disk HD 117214. We also performed the modeling of the HD 114082 light curve measured by TESS using models for planet transit and stellar activity to put constraints on the radius of the detected planet and its orbit. Last, we searched for additional planets in the system by combining archival radial velocity data, astrometry, and direct imaging. Results. The debris disk HD 114082 appears as an axisymmetric debris belt with a radius of ~0.37″ (35 au), an inclination of ~83°, and a wide inner cavity. Dust particles in HD 114082 have a maximum polarization fraction of ~17% and a higher reflectivity when compared to the debris disk HD 117214. This high reflectivity results in a spectral scattering albedo of ~0.65 for the HD 114082 disk at near-infrared wavelengths. The disk reflectance spectrum exhibits a red color at the position of the planetesimal belt and shows no obvious features, whereas that of HD 117214 might indicate the presence of CO2 ice. The analysis of TESS photometric data reveals a transiting planetary companion to HD 114082 with a radius of ~1 RJup on an orbit with a semimajor axis of 0.7 ± 0.4 au. No additional planet was detected in the system when we combined the SPHERE images with constraints from astrometry and radial velocity. We reach deep sensitivity limits down to ~5 MJup at 50 au and ~10 MJup at 30 au from the central star.

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Section: Discovery Of a Transiting Planetsupporting

confidence: 52%

Section: Discovery Of a Transiting Planetmentioning

confidence: 85%

Section: Companion Mass Sensitivity Limits Combining Direct Imaging R...mentioning

confidence: 99%

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The high-albedo, low polarization disk around HD 114082 that harbors a Jupiter-sized transiting planet

Engler

Milli

Gratton

et al. 2023

A&A

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“…That being said, a planet could cause a similar warp inside of the disk, similar to the β Pic system, where Pearce et al (2022) predict that a sculpting planet of mass 0.5 ± 0.4 M Jup with semimajor axis 8 ± 8 au is sufficient to create a warp at 40 au. While a planet is known to exist in the HD 114082 system (Engler et al 2022;Zakhozhay et al 2022), this planet is within 2 au of the star, making it dynamically uncoupled from the disk. However, as seen in Engler et al (2022), there is a clear opening within the inner radius of the disk, likely meaning that there are additional planets closer to the disk edge, and given that the disk is radially narrow, this suggests that there may also be a shepherding planet outside of the outer disk edge.…”

Section: Disks With Large Aspect Ratiosmentioning

confidence: 99%

“…HD 114082 is the most recent system to have a resolved debris disk and a known planet (Engler et al 2022;Zakhozhay et al 2022). Similar to AU Mic, the planet has been observed via the transit and radial velocity method, where the planet found has a mass of 8 M Jup , orbits at a distance of 0.51 au, and has a possible large eccentricity of 0.4 (Zakhozhay et al 2022). The disk lies much farther out from the star compared to the planet, and is fairly compact, similar to the HD 110058 disk.…”

Section: C12 Hd 114082mentioning

confidence: 99%

A Uniform Analysis of Debris Disks with the Gemini Planet Imager. I. An Empirical Search for Perturbations from Planetary Companions in Polarized Light Images

Crotts,

Matthews,

Duchêne

et al. 2024

ApJ

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The Gemini Planet Imager (GPI) has excelled in imaging debris disks in the near-infrared. The GPI Exoplanet Survey imaged 24 debris disks in polarized H-band light, while other programs observed half of these disks in polarized J and/or K1 bands. Using these data, we present a uniform analysis of the morphology of each disk to find asymmetries suggestive of perturbations, particularly those due to planet–disk interactions. The multiwavelength surface brightness, disk color, and geometry permit the identification of any asymmetries such as warps or disk offsets from the central star. We find that 19 of the disks in this sample exhibit asymmetries in surface brightness, disk color, disk geometry, or a combination of the three, suggesting that for this sample, perturbations, as seen in scattered light, are common. The relationship between these perturbations and potential planets in the system is discussed. We also explore correlations among stellar temperatures, ages, disk properties, and observed perturbations. We find significant trends between the vertical aspect ratio and the stellar temperature, disk radial extent, and the dust grain size distribution power law, q. We also confirm a trend between the disk color and stellar effective temperature, where the disk becomes increasingly red/neutral with increasing temperature. Such results have important implications for the evolution of debris disk systems around stars of various spectral types.

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TOI-837 b: Characterisation, formation, and evolutionary history of an infant warm Saturn-mass planet

Damasso,

Polychroni,

Locci

et al. 2024

A&A

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The detection and characterisation of planets younger than sim 100 Myr offer the opportunity to get snapshots of systems immediately after their formation, where the main evolutionary processes that sculpt mature planetary systems are still ongoing. Known infant exoplanets are currently scarce, and dedicated surveys are required to increase their number. We aim to determine the fundamental properties of the sim 35 Myr old star TOI-837 and its close-in Saturn-sized planet, and to investigate the system's formation and evolutionary history. We analysed TESS photometry and HARPS spectroscopic data, measured stellar and planetary parameters, and characterised the stellar activity. We performed population synthesis simulations to track the formation history of TOI-837\,$b$, and to reconstruct its possible internal structure. We investigated the planetary atmospheric evolution through photo-evaporation, and quantified the prospects for atmospheric characterisation with JWST. TOI-837\,$b$ has similar radius and mass to those of Saturn and $ and is on a primordial circular orbit. Population synthesis and early migration simulations suggest that the planet could have originally formed between 2 and 4 au, and have either a large and massive core, or a smaller Saturn-like core, depending on the opacity of the protoplanetary gas and on the growth rate of the core. We find that photo-evaporation produced negligible effects even at early ages (3–10 Myr). Transmission spectroscopy with JWST is very promising, and is expected to provide constraints on atmospheric metallicity and the abundances of H$_2$O, CO$_2$, and CH$_4$ molecules, and to probe the presence of refractory elements. TOI-837 offers valuable prospects for follow-up observations, which are needed for a thorough characterisation. JWST will help to better constrain the formation and evolution history of the system, and to clarify whether or not TOI-837\,$b$ is a Saturn-analogue.

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Radial velocity survey for planets around young stars (RVSPY)

Cited by 11 publications

References 45 publications

The high-albedo, low polarization disk around HD 114082 that harbors a Jupiter-sized transiting planet

The high-albedo, low polarization disk around HD 114082 that harbors a Jupiter-sized transiting planet

A Uniform Analysis of Debris Disks with the Gemini Planet Imager. I. An Empirical Search for Perturbations from Planetary Companions in Polarized Light Images

TOI-837 b: Characterisation, formation, and evolutionary history of an infant warm Saturn-mass planet

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