2020A&A...642A.133D


Query : 2020A&A...642A.133D

2020A&A...642A.133D - Astronomy and Astrophysics, volume 642A, 133-133 (2020/10-1)

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. and TURRINI D.

Abstract (from CDS):


Context. 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.
Aims. We observed the very young (∼2 Myr) 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±11m/s; mbsinib=0.57±0.10MJup; Pb=4.927±0.008d).
Methods. 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.
Results. 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.
Conclusions. 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.

Abstract Copyright: © ESO 2020

Journal keyword(s): stars: individual: V830 Tau - stars: individual: EPIC 247822311 - planets and satellites: detection - techniques: radar astronomy - techniques: photometric

VizieR on-line data: <Available at CDS (J/A+A/642/A133): tablea1.dat tablea2.dat tableb1.dat tablec1.dat>

Simbad objects: 21

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Number of rows : 21
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 V* V1298 Tau TT* 04 05 19.5912137335 +20 09 25.563534185   11.11 10.12 9.57   K1 57 0
2 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1264 0
3 UCAC4 573-011607 * 04 32 54.469416 +24 34 53.06628       15.27   ~ 1 0
4 UCAC4 573-011610 * 04 33 02.233152 +24 33 57.79800   16.45 15.07 15.29   ~ 1 0
5 V* V830 Tau TT* 04 33 10.0299730541 +24 33 43.255853678   13.91 12.08 11.30   M0-1 187 1
6 NAME V830 Tau b Pl 04 33 10.0299730541 +24 33 43.255853678           ~ 27 0
7 UCAC4 574-011176 * 04 33 17.420544 +24 37 15.86424   15.37 14.09 14.00   ~ 1 0
8 UCAC4 573-011630 * 04 33 49.071888 +24 35 33.32508   16.23 14.62 14.55   ~ 1 0
9 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3787 0
10 NAME AB Dor Moving Group MGr 06 38 53.4 -42 50 04           ~ 406 0
11 BD+20 1790 BY* 07 23 43.5892690689 +20 24 58.654590844   11.08 10.001 9.43 8.522 K5e 84 0
12 BD+20 2465 Er* 10 19 36.2808024653 +19 52 12.014037746   10.82 9.52 9.19   dM3 1199 0
13 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1657 1
14 NAME Ursa Major Moving Group MGr 12 32 +57.0           ~ 399 2
15 NAME HIP 67522 b Pl? 13 50 06.2796267125 -40 50 08.878258161           ~ 7 0
16 K2-33 Y*O 16 10 14.7378782154 -19 19 09.407200797   17.353       dM3.0 44 0
17 NAME Upper Sco Association As* 16 12 -23.4           ~ 1128 1
18 NAME AU Mic b Pl? 20 45 09.5323695486 -31 20 27.241710746           ~ 22 0
19 V* AU Mic LM* 20 45 09.5323695486 -31 20 27.241710746   10.05 8.627 9.078 6.593 M1VeBa1 965 0
20 NAME Cep Cloud SFR 22 00.0 +76 30           ~ 118 0
21 NAME Coma Berenices Moving Group MGr ~ ~           ~ 65 0

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2021.10.18-23:39:46

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