The GAPS programme at TNG LXXIX. New mass constraints for the infant planets in the V1298 Tau system through a long-term radial velocity monitoring with HARPS-N
Abstract
We aim to constrain the dynamical masses of the four confirmed transiting planets orbiting the infant (20±10 Myr) star V1298,Tau (orbital periods Pb∼24.1 d, Pc∼8.2 d, Pd∼12.4 d, and Pe∼48.7 d), through a new analysis of a homogeneous radial velocity dataset. This system is a key benchmark for testing formation and early-stage evolutionary models of planets. We analysed more than 380 high-resolution spectra collected with the HARPS-N spectrograph over a time span of 4.5,yr. To account for dominant stellar activity and transit-timing-derived planet-planet interactions, we analysed radial velocities extracted using two different approaches, and combined N-body simulations with multi-dimensional Gaussian process regression. We tested a set of spectroscopic and photometric activity diagnostics to mitigate the variability due to the stellar magnetic activity in the radial velocity time series. The mass determinations are sensitive to the choice of the radial velocity extraction method and activity diagnostics. For some specific models, we measured masses with a significance of 3.5--4σ for planets b (0.52+0.12−0.14, 0.65+0.21−0.18, 0.67±0.16, and 0.78+0.19−0.20 MJup) and e (0.40+0.14−0.13, 0.66+0.17−0.18, and 0.71±0.20 MJup). These values are compatible with masses of giant planets, and are notably higher than those recently derived from transit timing variations alone, which indicate that these are low-density ``super-puffy'' planets. Injection-and-recovery simulations moderately support this conclusion for planet b. For planets c and d, we primarily provide updated mass upper limits. Our analysis represents an exploratory study to address the complex issue of mass measurement in a multi-planetary system characterised by high levels of stellar activity.
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BibTeX
@misc{damasso2026gaps,
title = {{The GAPS programme at TNG LXXIX. New mass constraints for the infant planets in the V1298 Tau system through a long-term radial velocity monitoring with HARPS-N}},
author = {M. Damasso and P. Leonardi and L. Borsato and S. Benatti and A. Suárez Mascareño and A. Bonfanti and C. Di Maio and M. Mallorquín and L. Fossati and F. Marzari and D. Nardiello and S. Desidera and L. Naponiello and A. Sozzetti and G. Andreuzzi and M. Basilicata and A. Bignamini and A. S. Bonomo and M. Brogi and P. Giacobbe and G. Guilluy and A. F. Lanza and M. Lodi and L. Malavolta and L. Mancini and S. Messina and G. Micela and V. Nascimbeni and T. Zingales},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.30038},
eprint = {2609.30038},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.30038},
note = {CC BY-NC-ND 4.0},
}
RIS
TY - UNPB
TI - The GAPS programme at TNG LXXIX. New mass constraints for the infant planets in the V1298 Tau system through a long-term radial velocity monitoring with HARPS-N
AU - M. Damasso
AU - P. Leonardi
AU - L. Borsato
AU - S. Benatti
AU - A. Suárez Mascareño
AU - A. Bonfanti
AU - C. Di Maio
AU - M. Mallorquín
AU - L. Fossati
AU - F. Marzari
AU - D. Nardiello
AU - S. Desidera
AU - L. Naponiello
AU - A. Sozzetti
AU - G. Andreuzzi
AU - M. Basilicata
AU - A. Bignamini
AU - A. S. Bonomo
AU - M. Brogi
AU - P. Giacobbe
AU - G. Guilluy
AU - A. F. Lanza
AU - M. Lodi
AU - L. Malavolta
AU - L. Mancini
AU - S. Messina
AU - G. Micela
AU - V. Nascimbeni
AU - T. Zingales
PY - 2026
DA - 2026/09/24
PB - arXiv
DO - 10.48550/arxiv.2609.30038
UR - https://arxiv.org/abs/2609.30038
AB - We aim to constrain the dynamical masses of the four confirmed transiting planets orbiting the infant (20±10 Myr) star V1298,Tau (orbital periods P_b∼24.1 d, P_c∼8.2 d, P_d∼12.4 d, and P_e∼48.7 d), through a new analysis of a homogeneous radial velocity dataset. This system is a key benchmark for testing formation and early-stage evolutionary models of planets. We analysed more than 380 high-resolution spectra collected with the HARPS-N spectrograph over a time span of 4.5,yr. To account for dominant stellar activity and transit-timing-derived planet-planet interactions, we analysed radial velocities extracted using two different approaches, and combined N-body simulations with multi-dimensional Gaussian process regression. We tested a set of spectroscopic and photometric activity diagnostics to mitigate the variability due to the stellar magnetic activity in the radial velocity time series. The mass determinations are sensitive to the choice of the radial velocity extraction method and activity diagnostics. For some specific models, we measured masses with a significance of 3.5--4σ for planets b (0.52^+0.12−0.14, 0.65^+0.21−0.18, 0.67±0.16, and 0.78^+0.19−0.20 M_Jup) and e (0.40^+0.14−0.13, 0.66^+0.17−0.18, and 0.71±0.20 M_Jup). These values are compatible with masses of giant planets, and are notably higher than those recently derived from transit timing variations alone, which indicate that these are low-density ``super-puffy'' planets. Injection-and-recovery simulations moderately support this conclusion for planet b. For planets c and d, we primarily provide updated mass upper limits. Our analysis represents an exploratory study to address the complex issue of mass measurement in a multi-planetary system characterised by high levels of stellar activity.
ER -