Radial Velocity Survey for Planets around Young stars (RVSPY)

Zakhozhay, O. V.; Launhardt, R.; Müller, André; Brems, Stefan S.; Eigenthaler, Paul; Gennaro, Mario; Hempel, A.; Hempel, M.; Henning, Th.; Kennedy, Grant; Kim, S.; Kürster, M.; Lachaume, R.; Y., Manerikar,; Patel, J.; Pavlov, A.; Reffert, S.; Trifonov, T.

doi:10.1051/0004-6361/202244213

Cited by 4 publications

(1 citation statement)

References 74 publications

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“…Based on the analysis of the primary and secondary stars, we conclude that the age of the HD 117214 might be 7 ± 2 Myr. Our conclusion is supported by the results of the RV Survey for Planets around Young stars (RVSPY; Zakhozhay et al 2022a), which classifies this target as a pre-main-sequence star. Given the large intrinsic age spread for the LCC members, the HD 117214 might be one of the last formed stellar systems across the region.…”

Section: Appendix D: Companion Candidates' Astrometrysupporting

confidence: 76%

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: Appendix D: Companion Candidates' Astrometrysupporting

confidence: 76%

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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Radial velocity survey for planets around young stars (RVSPY)

Zakhozhay

Launhardt

Trifonov

et al. 2022

A&A

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Aims. We aim to detect planetary companions to young stars with debris disks via the radial velocity method. Methods. We observed HD 114082 during April 2018 -august 2022 as one of the targets of our RV SPY program (Radial Velocity Survey for Planets around Young stars). We use the FEROS spectrograph, mounted to the MPG/ESO 2.2 m telescope in Chile, to obtain high signal-to-noise spectra and time series of precise radial velocities (RVs). Additionally, we analyze archival HARPS spectra and TESS photometric data. We use the CERES, CERES++ and SERVAL pipelines to derive RVs and activity indicators and ExoStriker for the independent and combined analysis of the RVs and TESS photometry. Results. We report the discovery of a warm super-Jovian companion around HD 114082 based on a 109.8±0.4 day signal in the combined RV data from FEROS and HARPS, and on one transit event in the TESS photometry. The best-fit model indicates a 8.0±1.0 M Jup companion with a radius of 1.00±0.03R Jup in an orbit with a semi-major axis of 0.51±0.01 au and an eccentricity of 0.4±0.04. The companions orbit is in agreement with the known near edge-on debris disk located at ∼28 au. HD 114082 b is possibly the youngest (15±6 Myr), and one of only three young (<100 Myr) giant planetary companions for which both their mass and radius have been determined observationally. It is probably the first properly model-constraining giant planet that allows distinguishing between hot and cold-start models. It is significantly more compatible with the cold-start model.

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Evidence for Misalignment between Debris Disks and Their Host Stars

Hurt,

MacGregor

2023

ApJ

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We place lower limits on the obliquities between debris disks and their host stars for 31 systems by comparing their disk and stellar inclinations. While previous studies did not find evidence for misalignment, we identify six systems with minimum obliquities falling between ∼30°and 60°, indicating that debris disks can be significantly misaligned with their stars. These high-obliquity systems span a wide range of stellar parameters with spectral types K through A. Previous works have argued that stars with masses below 1.2 M ⊙ (spectral types of ∼F6) have magnetic fields strong enough to realign their rotation axes with the surrounding disk via magnetic warping; given that we observe high obliquities for relatively low-mass stars, magnetic warping alone is likely not responsible for the observed misalignments. Yet, chaotic accretion is expected to result in misalignments of ∼20° at most and cannot explain the larger obliquities found in this work. While it remains unclear how primordial misalignment might occur and what role it plays in determining the spin–orbit alignment of planets, future work expanding this sample is critical toward understanding the mechanisms that shape these high-obliquity systems.

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Radial Velocity Survey for Planets around Young stars (RVSPY)

Cited by 4 publications

References 74 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

Radial velocity survey for planets around young stars (RVSPY)

Evidence for Misalignment between Debris Disks and Their Host Stars

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