J/A+A/690/A235 Spectroscopic data of BD+40 2790 (TOI-2076) (Damasso+, 2024)
The GAPS programme at TNG. LIX. Characterisation study of the ∼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., Zapatero Osorio M.R., Zingales T.
<Astron. Astrophys. 690, A235 (2024)>
=2024A&A...690A.235D 2024A&A...690A.235D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Radial velocities ;
Optical
Keywords: techniques: photometric - techniques: radial velocities -
planets and satellites: general - stars: individual: BD+40 2790
Abstract:
The long-term Global Architecture of Planetary Systems (GAPS)
programme has been characterising a sample of young systems with
transiting planets via spectroscopic and photometric follow-up
observations. One of the main goals of GAPS is measuring planets'
dynamical masses and bulk densities to help build a picture of how
planets evolve in the early stages of their formation via a comparison
between the fundamental physical properties of young and mature
exoplanets.
We collected more than 300 high-resolution spectra of the ∼300Myr old
star BD+40 2790 (TOI-2076) over about three years. This star hosts
three transiting planets discovered by TESS, with orbital periods of
∼10, 21, and 35 days. From our determined fundamental planetary
physical properties, we investigate the temporal evolution of the
planetary atmospheres by calculating the expected mass loss rate due
to photo-evaporation up to a system age of 5Gyr.
BD+40 2790 shows an activity-induced scatter larger than 30m/s in the
radial velocities. We employed different methods to measure the
stellar radial velocities, along with several models to filter out the
dominant stellar activity signal to bring to light the planet-induced
signals, which are expected to have semi-amplitudes that are lower by
one order of magnitude. We evaluated the mass loss rate of the
planetary atmospheres using photo-ionisation hydrodynamic modeling,
accounting for the temporal evolution of the stellar high-energy flux
through the adoption of different models for X-rays and EUV
irradiation.
The dynamical analysis confirms that the three sub-Neptune-sized
companions (with our radius measurements of Rb=2.54±0.04,
R_c=3.35±0.05, and Rd=3.29±0.06R⊕) have masses that
situate them in the planetary regime. We derived 3σ upper limits
below or close to the mass of Neptune for all the planets in our
sample: 11-12, 12-13.5, and 14-19M⊕ for planets b, c, and d,
respectively. In the case of planet d, we found promising clues that
the mass could be between ∼7 and 8M⊕, with a significance
level between 2.3-2.5σ (at best). This result must be further
investigated using other analysis methods and techniques or using
high-precision near-infrared (nIR) 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 and that it will be
completely lost at an age within 0.5-3Gyr if its current mass is lower
than 12M⊕. Furthermore, BD+40 2790c could have a lower bulk
density than b and might be able to retain its atmosphere up to an age
of 5Gyr. For the outermost object, planet d, we predicted an almost
negligible evolution of its mass and radius, induced by
photo-evaporation.
Description:
Radial velocities and activity diagnostics derived from HARPS-N
spectra.
Objects:
----------------------------------------------------
RA (2000) DE Designation(s)
----------------------------------------------------
14 29 34.24 +39 47 25.5 BD+40 2790 = TOI-2076
----------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
rv.dat 80 293 HARPS-N radial velocity (multiple algorithms)
activity.dat 64 293 Activity diagnostics from HARPS-N spectra
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See also:
J/A+A/664/A156 : Young sub-Neptunes orbiting TOI-2076 light curves
(Osborn+, 2022)
Byte-by-byte Description of file: rv.dat
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Bytes Format Units Label Explanations
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1- 12 F12.6 d Epoch Epoch of observation (BJD-2450000)
15- 23 F9.2 m/s RVDRS Radial velocity calculated with the DRS
26- 30 F5.2 m/s e_RVDRS DRS RV error
34- 39 F6.2 m/s RVall Radial velocity SERVAL (all orders)
43- 46 F4.2 m/s e_RVall SERVAL RV error (all orders)
50- 55 F6.2 m/s RV5393-6916 Radial velocity SERVAL (5393-6916Å)
58- 62 F5.2 m/s e_RV5393-6916 SERVAL RV error (5393-6916Å)
65- 73 F9.2 m/s RVLBL Radial velocity calculated with LBL
77- 80 F4.2 m/s e_RVLBL LBL RV error
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Byte-by-byte Description of file: activity.dat
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Bytes Format Units Label Explanations
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1- 12 F12.6 d Epoch Epoch of observation (BJD-2450000)
16- 21 F6.2 m/s BIS CCF bisector span
24- 28 F5.2 m/s e_BIS CCF bisector span error
33- 39 F7.2 m/s FWHM CCF FWHM
42- 46 F5.2 m/s e_FWHM CCF FWHM error
49- 55 F7.4 [-] logR'HK Chromospheric index (Ca H&K lines)
59- 64 F6.4 [-] e_logR'HK Chromospheric index (Ca H&K lines) error
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Acknowledgements:
Mario Damasso, mario.damasso(at)inaf.it
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(End) Mario Damasso [INAF, Italy], Patricia Vannier [CDS] 29-Aug-2024