TY - JOUR
T1 - Radial velocity survey for planets around young stars (RVSPY)
T2 - A transiting warm super-Jovian planet around HD 114082, a young star with a debris disk
AU - Zakhozhay, Olga V.
AU - Launhardt, Ralf
AU - Trifonov, Trifon
AU - Kürster, Martin
AU - Reffert, Sabine
AU - Henning, Thomas
AU - Brahm, Rafael
AU - Vinés, José I.
AU - Marleau, Gabriel Dominique
AU - Patel, Jayshil A.
N1 - Funding Information:
The authors thank Coryn Bailer-Jones, Christoph Mordasini and Remo Burn for helpful discussions and feedback. O.Z. acknowledges support within the framework of the Ukraine aid package for individual grants of the Max-Planck Society 2022. T.T. acknowledges support by the BNSF program “VIHREN-2021” project No. КП-06-ДВ/5. Th.H. acknowledges support from the European Research Council under the European Union’s Horizon 2020 research and innovation program under grant agreement No. 832428-Origins. S.R. and G.-D.M. acknowledge support of the DFG (German Science Foundation) priority program SPP 1992 “Exploring the Diversity of Extrasolar Planets” (RE 2694/7-1 and MA 9185/1-1). R.B. acknowledges support from FONDECYT Project 11200751 and from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millenium Science Initiative. J.I.V. acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21191829. This research made use of the SIMBAD database, operated at the CDS, Strasbourg, France. G.-D.M. also acknowledges the support from the Swiss National Science Foundation under grant 200021_204847 “PlanetsInTime”. This work presents results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia MultiLateral Agreement (MLA). Parts of this work have been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. This research has made use of data obtained from or tools provided by the portal exoplanet.eu ( http://exoplanet.eu/ ) of The Extrasolar Planets Encyclopaedia. This work made use of tpfplotter by J. Lillo-Box (publicly available in www.github.com/jlillo/tpfplotter , which also made use of the python packages astropy , lightkurve , matplotlib and numpy . We also wish to thank the anonymous referee for constructive criticism that helped to improve the clarity of the paper.
Funding Information:
The authors thank Coryn Bailer-Jones, Christoph Mordasini and Remo Burn for helpful discussions and feedback. O.Z. acknowledges support within the framework of the Ukraine aid package for individual grants of the Max-Planck Society 2022. T.T. acknowledges support by the BNSF program "VIHREN-2021" project No. KP-06-DV/5. Th.H. acknowledges support from the European Research Council under the European Union’s Horizon 2020 research and innovation program under grant agreement No. 832428-Origins. S.R. and G.-D.M. acknowledge support of the DFG (German Science Foundation) priority program SPP 1992 "Exploring the Diversity of Extrasolar Planets" (RE 2694/7-1 and MA 9185/1-1). R.B. acknowledges support from FONDECYT Project 11200751 and from project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative. J.I.V. acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21191829. This research made use of the SIMBAD database, operated at the CDS, Strasbourg, France. G.-D.M. also acknowledges the support from the Swiss National Science Foundation under grant 200021_204847 "PlanetsInTime". This work presents results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia MultiLateral Agreement (MLA). Parts of this work have been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. This research has made use of data obtained from or tools provided by the portal exoplanet.eu (http://exoplanet.eu/) of The Extrasolar Planets Encyclopaedia. This work made use of tpfplotter by J. Lillo-Box (publicly available in www.github.com/jlillo/tpfplotter, which also made use of the python packages astropy, lightkurve, matplotlib and numpy. We also wish to thank the anonymous referee for constructive criticism that helped to improve the clarity of the paper.
Publisher Copyright:
© O. V. Zakhozhay et al. 2022.
PY - 2022/11/1
Y1 - 2022/11/1
N2 - 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 RVSPY 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 MJup companion with a radius of 1.00±0.03RJup 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.
AB - 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 RVSPY 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 MJup companion with a radius of 1.00±0.03RJup 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.
KW - Methods: observational
KW - Planets and satellites: detection
KW - Planets and satellites: formation
KW - Stars: activity
KW - Techniques: photometric
KW - Techniques: radial velocities
UR - http://www.scopus.com/inward/record.url?scp=85145255772&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202244747
DO - 10.1051/0004-6361/202244747
M3 - Article
AN - SCOPUS:85145255772
SN - 0004-6361
VL - 667
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
IS - 102
M1 - L14
ER -