The GAPS Programme at TNG

Carleo, I.; Desidera, S.; Nardiello, D.; Malavolta, L.; Lanza, A. F.; Livingston, John H.; Locci, Daniele; Marzari, F.; Messina, S.; Turrini, D.; Baratella, M.; Borsa, F.; D’Orazi, V.; Nascimbeni, V.; Pinamonti, M.; Rainer, M.; Alei, Eleonora; Bignamini, A.; Gratton, R.; Micela, G.; Montalto, M.; Sozzetti, A.; Squicciarini, Vito; Affer, L.; Benatti, S.; Biazzo, K.; Bonomo, A. S.; Claudi, R.; Cosentino, R.; Covino, E.; Damasso, M.; Esposito, M.; Fiorenzano, A. F. Martínez; Frustagli, G.; Giacobbe, P.; Harutyunyan, A.; Leto, G.; Magazzù, A.; Maggio, A.; Mainella, Giovanni; Maldonado, J.; Mallonn, M.; Mancini, L.; Molinari, E.; Molinaro, M.; Pagano, I.; Pedani, M.; Piotto, G.; Poretti, E.; Redfield, Seth; Scandariato, G.

doi:10.1051/0004-6361/202039042

Cited by 36 publications

(36 citation statements)

References 134 publications

(109 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Stellar age is a key parameter in several astrophysical contexts, from exo-planetary science, where the derived values of the planet's physical parameters depend on the age of the host star (see e.g. Carleo et al 2021), to Milky Way studies, where Galactic formation and evolution models can be constrained if the age of numerous field and cluster stars is known (see e.g. Hayden et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Gyrochronological dating of the stellar moving group Group X

Messina

Nardiello

Desidera

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

Context. Gyrochronology is one of the methods currently used to estimate the age of stellar open clusters. Hundreds of new clusters, associations, and moving groups unveiled by Gaia and complemented by accurate rotation period measurements provided by recent space missions such as Kepler and TESS are allowing us to significantly improve the reliability of this method. Aims. We use gyrochronology, that is, the calibrated age-mass-rotation relation valid for low-mass stars, to measure the age of the recently discovered moving group Group X. Methods. We extracted the light curves of all candidate members from the TESS full frame images and measured their rotation periods using different period search methods. Results. We measured the rotation period of 168 of a total of 218 stars and compared their period-colour distribution with those of two age-benchmark clusters, the Pleiades (125 Myr) and Praesepe (625 Myr), as well as with the recently characterised open cluster NGC 3532 (300 Myr). Conclusions. As result of our analysis, we derived a gyro age of 300 ± 60 Myr. We also applied as independent methods the fitting of the entire isochrone and of the three brightest candidate members individually with the most precise stellar parameters, deriving comparable values of 250 Myr and 290 Myr, respectively. Our dating of Group X allows us to definitively rule out the previously proposed connection with the nearby but much older Coma Berenices cluster.

show abstract

Section: Introductionmentioning

confidence: 99%

Gyrochronological dating of the stellar moving group Group X

Messina

Nardiello

Desidera

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…In particular, [264] and [320] have shown how the information provided by normalized angular momentum deficit (NAMD), an architecture-agnostic measure of the dynamical excitation of planetary systems, allows to build a relative scale of violence of their past histories. Intuitively, the NAMD can be interpreted as the "dynamical temperature" of planetary systems: the higher the value, the more excited is the dynamical state of the system.…”

Section: Planetary Architectures: Dynamical Context To Compositionmentioning

confidence: 99%

“…As discussed by [264] and [320], Trappist-1 and the Solar System provide two such reference values, the first as a system characterized by an orderly and stable evolution [321,322] while the second as the boundary between orderly and chaotic evolution [323]. As shown in Fig.…”

Section: Planetary Architectures: Dynamical Context To Compositionmentioning

confidence: 99%

Exploring the link between star and planet formation with Ariel

et al. 2021

View full text Add to dashboard Cite

The goal of the Ariel space mission is to observe a large and diversified population of transiting planets around a range of host star types to collect information on their atmospheric composition. The planetary bulk and atmospheric compositions bear the marks of the way the planets formed: Ariel’s observations will therefore provide an unprecedented wealth of data to advance our understanding of planet formation in our Galaxy. A number of environmental and evolutionary factors, however, can affect the final atmospheric composition. Here we provide a concise overview of which factors and effects of the star and planet formation processes can shape the atmospheric compositions that will be observed by Ariel, and highlight how Ariel’s characteristics make this mission optimally suited to address this very complex problem.

show abstract

“…It would be preferable to observe atmospheric escape in young planetary systems, as this would allow us to test our understanding of mass-loss physics during the epoch when most atmopsheric mass loss is predicted to occur. There are currently only seven confirmed young (<100 Myr) transiting planet systems: K2-33 (David et al 2016;Mann et al 2016), V1298 Tau (David et al 2019a(David et al , 2019b, DS Tuc A (Newton et al 2019), TOI 837 (Bouma et al 2020), AU Mic (Plavchan et al 2020), TOI 942 (Carleo et al 2021;Zhou et al 2021), and HIP 67522 (Rizzuto et al 2020). The expected magnitude of the outflows from these young planets depends on their gravitational potentials (e.g., Hirano et al 2020), which can be calculated using their measured masses and radii.…”

Section: Introductionmentioning

confidence: 99%

A Search for Planetary Metastable Helium Absorption in the V1298 Tau System

Vissapragada¹,

Stefánsson

Greklek-McKeon³

et al. 2021

View full text Add to dashboard Cite

Early in their lives, planets endure extreme amounts of ionizing radiation from their host stars. For planets with primordial hydrogen and helium-rich envelopes, this can lead to substantial mass loss. Direct observations of atmospheric escape in young planetary systems can help elucidate this critical stage of planetary evolution. In this work, we search for metastable helium absorption—a tracer of tenuous gas in escaping atmospheres—during transits of three planets orbiting the young solar analog V1298 Tau. We characterize the stellar helium line using HET/HPF, and find that it evolves substantially on timescales of days to months. The line is stable on hour-long timescales except for one set of spectra taken during the decay phase of a stellar flare, where absoprtion increased with time. Utilizing a beam-shaping diffuser and a narrowband filter centered on the helium feature, we observe four transits with Palomar/WIRC: two partial transits of planet d (P = 12.4 days), one partial transit of planet b (P = 24.1 days), and one full transit of planet c (P = 8.2 days). We do not detect the transit of planet c, and we find no evidence of excess absorption for planet b, with ΔR b/R ⋆ < 0.019 in our bandpass. We find a tentative absorption signal for planet d with ΔR d/R ⋆ = 0.0205 ± 0.054, but the best-fit model requires a substantial (−100 ± 14 minutes) transit-timing offset on a two-month timescale. Nevertheless, our data suggest that V1298 Tau d may have a high present-day mass-loss rate, making it a priority target for follow-up observations.

show abstract

The GAPS Programme at TNG

Cited by 36 publications

References 134 publications

Gyrochronological dating of the stellar moving group Group X

Gyrochronological dating of the stellar moving group Group X

Exploring the link between star and planet formation with Ariel

A Search for Planetary Metastable Helium Absorption in the V1298 Tau System

Contact Info

Product

Resources

About