The GAPS Programme at TNG. LIX. A characterisation study of the $\sim$300 Myr old multi-planetary system orbiting the star BD+40 2790 (TOI-2076)

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Main Authors:	Damasso, M., Locci, D., Benatti, S., Maggio, A., Baratella, M., Desidera, S., Biazzo, K., Palle, E., Wang, S., Nardiello, D., Borsato, L., Bonomo, A. S., Messina, S., Nowak, G., Goyal, A., Bejar, V. J. S., Bignamini, A., Cabona, L., Carleo, I., Claudi, R., Cosentino, R., Filomeno, S., Knapic, C., Lodieu, N., Lorenzi, V., Malavolta, L., Mallorquin, M., Mancini, L., Mantovan, G., Micela, G., Murgas, F., Orell-Miquel, J., Pedani, M., Pinamonti, M., Sozzetti, A., Spinelli, R., Osorio, M. R. Zapatero, Zingales, T.
Format:	Preprint
Published:	2024
Subjects:	Earth and Planetary Astrophysics
Online Access:	Acceder al recurso
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author	Damasso, M. Locci, D. Benatti, S. Maggio, A. Baratella, M. Desidera, S. Biazzo, K. Palle, E. Wang, S. Nardiello, D. Borsato, L. Bonomo, A. S. Messina, S. Nowak, G. Goyal, A. Bejar, V. J. S. Bignamini, A. Cabona, L. Carleo, I. Claudi, R. Cosentino, R. Filomeno, S. Knapic, C. Lodieu, N. Lorenzi, V. Malavolta, L. Mallorquin, M. Mancini, L. Mantovan, G. Micela, G. Murgas, F. Orell-Miquel, J. Pedani, M. Pinamonti, M. Sozzetti, A. Spinelli, R. Osorio, M. R. Zapatero Zingales, T.
author_facet	Damasso, M. Locci, D. Benatti, S. Maggio, A. Baratella, M. Desidera, S. Biazzo, K. Palle, E. Wang, S. Nardiello, D. Borsato, L. Bonomo, A. S. Messina, S. Nowak, G. Goyal, A. Bejar, V. J. S. Bignamini, A. Cabona, L. Carleo, I. Claudi, R. Cosentino, R. Filomeno, S. Knapic, C. Lodieu, N. Lorenzi, V. Malavolta, L. Mallorquin, M. Mancini, L. Mantovan, G. Micela, G. Murgas, F. Orell-Miquel, J. Pedani, M. Pinamonti, M. Sozzetti, A. Spinelli, R. Osorio, M. R. Zapatero Zingales, T.
contents	We collected more than 300 high-resolution spectra of the 300 Myr old star BD+40 2790 (TOI-2076) over ~3 years. This star hosts three transiting planets discovered by TESS, with orbital periods ~10, 21, and 35 days. BD+40 2790 shows an activity-induced scatter larger than 30 m/s in the radial velocities. We employed different methods to measure the stellar radial velocities and several models to filter out the dominant stellar activity signal, in order to bring to light the planet-induced signals which are expected to have semi-amplitudes one order of magnitude lower. We evaluated the mass loss rate of the planetary atmospheres using photoionization hydrodynamic modeling. The dynamical analysis confirms that the three sub-Neptune-sized companions (our radius measurements are $R_b$=2.54$\pm$0.04, $R_c$=3.35$\pm$0.05, and $R_d$=3.29$\pm$0.06 $R_{\rm Earth}$) have masses in the planetary regime. We derive 3$σ$ upper limits below or close to the mass of Neptune for all the planets: 11--12, 12--13.5, and 14--19 $M_{\rm Earth}$ for planet $b$, $c$, and $d$ respectively. In the case of planet $d$, we found promising clues that the mass could be between ~7 and 8 $M_{\rm Earth}$, with a significance level between 2.3--2.5$σ$ (at best). This result must be further investigated using other analysis methods or using high-precision near-IR spectrographs to collect new radial velocities, which could be less affected by stellar activity. Atmospheric photo-evaporation simulations predict that BD+40~2790 b is currently losing its H-He gaseous envelope, which will be completely lost at an age within 0.5--3 Gyr if its current mass is lower than 12 $M_{\rm Earth}$. BD+40 2790 c could have a lower bulk density than $b$, and it could retain its atmosphere up to an age of 5 Gyr. For the outermost planet $d$, we predict almost negligible evolution of its mass and radius induced by photo-evaporation.
format	Preprint
id	arxiv_https___arxiv_org_abs_2408_10629
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	The GAPS Programme at TNG. LIX. A characterisation study of the $\sim$300 Myr old multi-planetary system orbiting the star BD+40 2790 (TOI-2076) Damasso, M. Locci, D. Benatti, S. Maggio, A. Baratella, M. Desidera, S. Biazzo, K. Palle, E. Wang, S. Nardiello, D. Borsato, L. Bonomo, A. S. Messina, S. Nowak, G. Goyal, A. Bejar, V. J. S. Bignamini, A. Cabona, L. Carleo, I. Claudi, R. Cosentino, R. Filomeno, S. Knapic, C. Lodieu, N. Lorenzi, V. Malavolta, L. Mallorquin, M. Mancini, L. Mantovan, G. Micela, G. Murgas, F. Orell-Miquel, J. Pedani, M. Pinamonti, M. Sozzetti, A. Spinelli, R. Osorio, M. R. Zapatero Zingales, T. Earth and Planetary Astrophysics We collected more than 300 high-resolution spectra of the 300 Myr old star BD+40 2790 (TOI-2076) over ~3 years. This star hosts three transiting planets discovered by TESS, with orbital periods ~10, 21, and 35 days. BD+40 2790 shows an activity-induced scatter larger than 30 m/s in the radial velocities. We employed different methods to measure the stellar radial velocities and several models to filter out the dominant stellar activity signal, in order to bring to light the planet-induced signals which are expected to have semi-amplitudes one order of magnitude lower. We evaluated the mass loss rate of the planetary atmospheres using photoionization hydrodynamic modeling. The dynamical analysis confirms that the three sub-Neptune-sized companions (our radius measurements are $R_b$=2.54$\pm$0.04, $R_c$=3.35$\pm$0.05, and $R_d$=3.29$\pm$0.06 $R_{\rm Earth}$) have masses in the planetary regime. We derive 3$σ$ upper limits below or close to the mass of Neptune for all the planets: 11--12, 12--13.5, and 14--19 $M_{\rm Earth}$ for planet $b$, $c$, and $d$ respectively. In the case of planet $d$, we found promising clues that the mass could be between ~7 and 8 $M_{\rm Earth}$, with a significance level between 2.3--2.5$σ$ (at best). This result must be further investigated using other analysis methods or using high-precision near-IR spectrographs to collect new radial velocities, which could be less affected by stellar activity. Atmospheric photo-evaporation simulations predict that BD+40~2790 b is currently losing its H-He gaseous envelope, which will be completely lost at an age within 0.5--3 Gyr if its current mass is lower than 12 $M_{\rm Earth}$. BD+40 2790 c could have a lower bulk density than $b$, and it could retain its atmosphere up to an age of 5 Gyr. For the outermost planet $d$, we predict almost negligible evolution of its mass and radius induced by photo-evaporation.
title	The GAPS Programme at TNG. LIX. A characterisation study of the $\sim$300 Myr old multi-planetary system orbiting the star BD+40 2790 (TOI-2076)
topic	Earth and Planetary Astrophysics
url	https://arxiv.org/abs/2408.10629