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Author Sedaghati, E.; MacDonald, R.J.; Casasayas-Barris, N.; Hoeijmakers, H.J.; Boffin, H.M.J.; Rodler, F.; Brahm, R.; Jones, M.; Sanchez-Lopez, A.; Carleo, I.; Figueira, P.; Mehner, A.; Lopez-Puertas, M. doi  openurl
  Title A spectral survey of WASP-19b with ESPRESSO Type
  Year 2021 Publication Monthly Notices Of The Royal Astronomical Society Abbreviated Journal Mon. Not. Roy. Astron. Soc.  
  Volume 505 Issue 1 Pages 435-458  
  Keywords methods: data analysis; techniques: spectroscopic; planets and satellites: atmospheres; planets and satellites: individual: WASP-19b; stars: activity; stars: individual: WASP-19  
  Abstract High-resolution precision spectroscopy provides a multitude of robust techniques for probing exoplanetary atmospheres. We present multiple VLT/ESPRESSO transit observations of the hot-Jupiter exoplanet WASP-19b with previously published but disputed atmospheric features from low resolution studies. Through spectral synthesis and modelling of the Rossiter-McLaughlin (RM) effect we calculate stellar, orbital and physical parameters for the system. From narrow-band spectroscopy we do not detect any of Hi, Fei, Mgi, Cai, Nai, and Ki neutral species, placing upper limits on their line contrasts. Through cross-correlation analyses with atmospheric models, we do not detect Fei and place a 3 sigma upper limit of on its mass fraction, from injection and retrieval. We show the inability to detect the presence of H2O for known abundances, owing to lack of strong absorption bands, as well as relatively low S/N ratio. We detect a barely significant peak (3.02 +/- 0.15 sigma) in the cross-correlation map for TiO, consistent with the sub-solar abundance previously reported. This is merely a hint for the presence of TiO and does not constitute a confirmation. However, we do confirm the presence of previously observed enhanced scattering towards blue wavelengths, through chromatic RM measurements, pointing to a hazy atmosphere. We finally present a reanalysis of low-resolution transmission spectra of this exoplanet, concluding that unocculted starspots alone cannot explain previously detected features. Our reanalysis of the FORS2 spectra of WASP-19b finds a similar to 100x sub-solar TiO abundance, precisely constrained to , consistent with the TiO hint from ESPRESSO. We present plausible paths to reconciliation with other seemingly contradicting results.  
  Address  
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  Series Editor Series Title Abbreviated Series Title  
  Series Volume Series Issue Edition  
  ISSN 0035-8711 ISBN Medium  
  Area Expedition Conference  
  Notes WOS:000671453100031 Approved  
  Call Number UAI @ alexi.delcanto @ Serial 1438  
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Author Zakhozhay, O.V.; Launhardt, R.; Trifonov, T.; Kunster, M.; Reffert, S.; Henning, T.; Brahm, R.; Vines, J.I.; Marleau, G.D.; Patel, J.A. doi  openurl
  Title Radial velocity survey for planets around young stars (RVSPY) A transiting warm super-Jovian planet around HD 114082, a young star with a debris disk Type
  Year 2022 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.  
  Volume 667 Issue Pages L14  
  Keywords methods: observational; techniques: radial velocities; techniques: photometric; planets and satellites: detection; planets and satellites: formation; stars: activity  
  Abstract Aims. We aim to detect planetary companions to young stars with debris disks via the radial velocity method.

Methods. We observed HD114082 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 2.2mtelescope 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 HD114082 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 +/- 1.0M(Jup) companion with a radius of 1.00 +/- 0.03 R-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 similar to 28 au. HD114082 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.
 
  Address  
  Corporate Author Thesis  
  Publisher Place of Publication Editor  
  Language Summary Language Original Title  
  Series Editor Series Title Abbreviated Series Title  
  Series Volume Series Issue Edition  
  ISSN 0004-6361 ISBN Medium  
  Area Expedition Conference  
  Notes WOS:000892293400011 Approved  
  Call Number UAI @ alexi.delcanto @ Serial 1707  
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