J/A+A/642/A133      V830 Tau VI light curves and RV curves      (Damasso+, 2020)

The GAPS Programme at TNG. XXVII. Reassessment of a young planetary system with HARPS-N: is the hot Jupiter V830 Tau b really there? 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. <Astron. Astrophys. 642, A133 (2020)> =2020A&A...642A.133D 2020A&A...642A.133D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Photometry ; Optical ; Radial velocities Keywords: stars: individual: V830 Tau - stars: individual: EPIC 247822311 - planets and satellites: detection - techniques: radial velocities - techniques: photometric Abstract: 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 (Kb=68±11ms; mbsinib=0.57±0.10Mjup; Pb=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. Description: Photometry collected with the STELLA telescope; radial velocities and stellar activity diagnostics extracted from HARPS-N spectra. Objects: ---------------------------------------------------------- RA (ICRS) DE Designation(s) ---------------------------------------------------------- 04 33 10.03 +24 33 43.3 V830 Tau = EPIC 247822311 ---------------------------------------------------------- File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tablea1.dat 25 125 STELLA V-band photometry (relative flux) tablea2.dat 25 122 STELLA I-band photometry (relative flux) tableb1.dat 54 144 Spectroscopic activity diagnostics tablec1.dat 51 144 Radial velocities (m/s) -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablea1.dat tablea2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 11 F11.6 d Time Epoch of observation (BJD-2450000) 13- 18 F6.4 --- Flux Relative photometry 20- 25 F6.4 --- e_Flux Relative photometry error ------------------------------------------------------------------------------- Byte-by-byte Description of file: tableb1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 11 F11.6 d Time Epoch of observation (BJD-2450000) 13- 19 F7.1 m/s FWHM CCF FWHM 21- 30 F10.1 m/s BIS CCF bisector span 32- 36 F5.3 --- CaHK Chromospheric CaHK index 38- 42 F5.3 --- e_CaHK Chromospheric CaHK index error 44- 48 F5.3 --- Halpha Chromospheric H-alpha index 50- 54 F5.3 --- e_Halpha Chromospheric H-alpha index error -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablec1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 11 F11.6 d Time Epoch of observation (BJD-2450000) 13- 19 F7.1 m/s RVTerra TERRA radial velocity 21- 24 F4.1 m/s e_RVTerra TERRA radial velocity error 26- 32 F7.1 m/s RVDRS DRS radial velocity 34- 37 F4.1 m/s e_RVDRS DRS radial velocity error 39- 45 F7.1 m/s RVRaj20 Rajpaul et al. (2020MNRAS.492.3960R 2020MNRAS.492.3960R) radial velocity 47- 51 F5.1 m/s e_RVRaj20 Rajpaul et al. (2020MNRAS.492.3960R 2020MNRAS.492.3960R) radial velocity error -------------------------------------------------------------------------------- Acknowledgements: Mario Damasso, mario.damasso(at)inaf.it References: Covino et al., Paper I 2013A&A...554A..28C 2013A&A...554A..28C, Cat. J/A+A/554/A28 Desidera et al., Paper II 2013A&A...554A..29D 2013A&A...554A..29D Esposito et al., Paper III 2014A&A...564L..13E 2014A&A...564L..13E Desidera et al., Paper IV 2014A&A...567L...6D 2014A&A...567L...6D Damasso et al., Paper V 2015A&A...575A.111D 2015A&A...575A.111D, Cat. J/A+A/575/A111 Sozzetti et al., Paper VI 2015A&A...575L..15S 2015A&A...575L..15S, Cat. J/A+A/575/L15 Borsa et al., Paper VII 2015A&A...578A..64B 2015A&A...578A..64B, Cat. J/A+A/578/A64 Mancini et al., Paper VIII 2015A&A...579A.136M 2015A&A...579A.136M, Cat. J/A+A/579/A136 Damasso et al., Paper IX 2015A&A...581L...6D 2015A&A...581L...6D Biazzo et al., Paper X 2015A&A...583A.135B 2015A&A...583A.135B, Cat. J/A+A/583/A135 Malavolta et al., Paper XI 2016A&A...588A.118M 2016A&A...588A.118M, Cat. J/A+A/588/A118 Benatti et al., Paper XII 2017A&A...599A..90B 2017A&A...599A..90B, Cat. J/A+A/599/A90 Esposito et al., Paper XIII 2017A&A...601A..53E 2017A&A...601A..53E Bonomo et al., Paper XIV 2017A&A...602A.107B 2017A&A...602A.107B, Cat. J/A+A/602/A107 Gonzalez-Alvarez et al., Paper XV 2017A&A...606A..51G 2017A&A...606A..51G Mancini et al., Paper XVI 2018A&A...613A..41M 2018A&A...613A..41M, Cat. J/A+A/613/A41 Lanza et al., Paper XVII 2018A&A...616A.155L 2018A&A...616A.155L, Cat. J/A+A/616/A155 Barbato et al., Paper XVIII 2019A&A...621A.110B 2019A&A...621A.110B, Cat. J/A+A/621/A110 Borsa et al., Paper XIX 2019A&A...631A..34B 2019A&A...631A..34B, Cat. J/A+A/631/A34 Pino et al., Paper XX 2020ApJ...894L..27P 2020ApJ...894L..27P Carleo et al., Paper XXI 2020A&A...638A...5C 2020A&A...638A...5C, Cat. J/A+A/638/A5 Guilluy et al., Paper XXII 2020A&A...639A..49G 2020A&A...639A..49G Benatti et al., Paper XXIII 2020A&A...639A..50B 2020A&A...639A..50B, Cat. J/A+A/639/A50
(End) Mario Damasso [INAF, Italy], Patricia Vannier [CDS] 31-Aug-2020
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