V830 Tau VI light curves and RV curves

DOI

Detecting and characterising exoworlds around very young stars (age<=10Myr) are key aspects of exoplanet demographic studies, especially for understanding the mechanisms and timescales of planet formation and migration. Any reliable theory for such physical phenomena requires a robust observational database to be tested. However, detection using the radial velocity method alone can be very challenging because the amplitude of the signals caused by the magnetic activity of such stars can be orders of magnitude larger than those induced even by massive planets. We observed the very young (~2Myr) and very active star V830 Tau with the HARPS-N spectrograph between October 2017 and March 2020 to independently confirm and characterise the previously reported hot Jupiter V830 Tau b (K_b_=68+/-11ms; m_b_sini_b_=0.57+/-0.10M_jup_; P_b_=4.927+/-0.008d). Because of the observed ~1km/s radial velocity scatter that can clearly be attributed to the magnetic activity of V830 Tau, we analysed radial velocities extracted with different pipelines and modelled them using several state-of-the-art tools. We devised injection-recovery simulations to support our results and characterise our detection limits. The analysis of the radial velocities was aided by a characterisation of the stellar activity using simultaneous photometric and spectroscopic diagnostics. Despite the high quality of our HARPS-N data and the diversity of tests we performed, we were unable to detect the planet V830 Tau b in our data and cannot confirm its existence. Our simulations show that a statistically significant detection of the claimed planetary Doppler signal is very challenging. It is important to continue Doppler searches for planets around young stars, but utmost care must be taken in the attempt to overcome the technical difficulties to be faced in order to achieve their detection and characterisation. This point must be kept in mind when assessing their occurrence rate, formation mechanisms, and migration pathways, especially without evidence of their existence from photometric transits.

Identifier
DOI http://doi.org/10.26093/cds/vizier.36420133
Source https://dc.g-vo.org/rr/q/lp/custom/CDS.VizieR/J/A+A/642/A133
Related Identifier https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/642/A133
Related Identifier http://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/642/A133
Metadata Access http://dc.g-vo.org/rr/q/pmh/pubreg.xml?verb=GetRecord&metadataPrefix=oai_b2find&identifier=ivo://CDS.VizieR/J/A+A/642/A133
Provenance
Creator Damasso M.; Lanza A.F.; Benatti S.; Rajpaul V.M.; Mallonn M.; Desidera S.; Biazzo K.; D'Orazi V.; Malavolta L.; Nardiello D.; Rainer M.; Borsa F.; Affer L.; Bignamini A.; Bonomo A.S.; Carleo I.; Claudi R.; Cosentino R.; Covino E.; Giacobbe P.; Gratton R.; Harutyunyan A.; Knapic C.; Leto G.; Maggio A.; Maldonado J.; Mancini L.; Micela G.; Molinari E.; Nascimbeni V.; Pagano I.; Piotto G.; Poretti E.; Scandariato G.; Sozzetti A.; Capuzzo Dolcetta R.; Di Mauro M.P.; Carosati D.; Fiorenzano A.; Frustagli G.; Pedani M.; Pinamonti M.; Stoev H.; Turrini D.
Publisher CDS
Publication Year 2020
Rights https://cds.unistra.fr/vizier-org/licences_vizier.html
OpenAccess true
Contact CDS support team <cds-question(at)unistra.fr>
Representation
Resource Type Dataset; AstroObjects
Discipline Astrophysics and Astronomy; Exoplanet Astronomy; Natural Sciences; Observational Astronomy; Physics; Stellar Astronomy