Dream

Bourrier, V.; Attia, O.; Mallonn, M.; Marret, A.; Lendl, M.; König, Pierre-Cécil; Krenn, A.; Cretignier, M.; Allart, R.; Henry, Gregory W.; Bryant, Edward M.; Leleu, Adrien; Nielsen, L. D.; Hébrard, G.; Hara, N.; Ehrenreich, D.; Seidel, J. V.; Santos, Louis D.; Bayliss, Daniel; Cegla, H. M.; Dumusque, X.; Boisse, I.; Boucher, Anne; Bouchy, F.; Pepe, F.; Lavie, B.; Cerda, J. Rey; Ségransan, D.; Udry, S.; Vrignaud, T.

doi:10.1051/0004-6361/202245004

Cited by 24 publications

(10 citation statements)

References 239 publications

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“…The series of synthetic+analytical intensity spectra is then interpolated over the whole stellar grid, and Doppler-shifted according to the local radial velocity set by the projected stellar rotational velocity (Bourrier et al 2023). Subsequently, intensity spectra are scaled into local flux spectra using the surface of the stellar grid cells, and summed over the whole grid to derive a simulated disk-integrated spectrum of the target star.…”

Section: Accurate Stellar Line Profilesmentioning

confidence: 99%

“…high-eccentricity orbital migration followed by tidal interaction with the star (e.g., Matsakos & Königl 2016) are the most likely explanations to date, but their interplay remains to be explored. Among questions that need to be addressed are the range of mass and period over which these processes are at play and whether they also shape the Neptunian "savanna" that is represented by a lighter deficit of Neptune-size planets at longer periods and lower irradiation, as highlighted by Bourrier et al (2023).…”

Section: Introductionmentioning

confidence: 99%

“…Investigating this complex puzzle is the goal of the Desert-Rim Exoplanets Atmosphere and Migration (DREAM) program. In DREAM I (Bourrier et al 2023), we measured the orbital architectures of a large sample of exoplanets spanning the borders of the Neptunian desert and savanna. This work revealed a high fraction of misaligned orbits, strengthening the importance of high-eccentricity orbital migration for close-in planets.…”

Section: Introductionmentioning

confidence: 99%

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Dream

Guilluy¹,

Bourrier²,

Jaziri³

et al. 2023

A&A

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Context. The population of close-in exoplanets features a desert of hot Neptunes whose origin remains uncertain. These planets may have lost their atmosphere, eroding into mini-Neptunes and rocky super-Earths below the desert. Direct observations of evaporating atmospheres are essential to derive mass-loss estimates and constrain this scenario. The metastable He I triplet at 1083.3 nm represents a powerful diagnostic of atmospheric evaporation because it traces the hot gas in extended exoplanet atmospheres while being observed from the ground. In addition, it is located at the bright near-infrared stellar continuum and is very weakly affected by interstellar medium (ISM) absorption. Aims. We carried out a homogeneous He I transmission spectroscopy survey, targeting a selected sample of nine planets along the different edges of the desert, to interpret the absorption line profile with evaporation models and to better understand the role of photoevaporation in the desert formation. Methods. We observed one transit per planet using the high-resolution, near-infrared spectrograph GIANO-B mounted on the Telescopio Nazionale Galileo telescope. We focused our analysis on the He I triplet, based on a comparison of the in-transit and out-of-transit observations, and we computed high-resolution transmission spectra. We then employed the 1D p-winds model to calculate the planetary thermospheric structures and to interpret the observed transmission spectra. Results. We found no signatures of planetary absorption in the He I triplet in any of the investigated targets. We thus provided 3 σ upper-limit estimations on the thermosphere absorption, temperature and mass loss, and combined them with past measurements to search for correlations with parameters such as the stellar mass and XUV flux, which are thought to be key drivers in the formation of the He I triplet. Conclusions. These results strengthen the importance of performing homogeneous surveys and analyses in bringing clarity to He I detections and (thereby) to plausible Neptunian desert origins. Our findings corroborate literature expectations that state the He I absorption signal is correlated with the stellar mass and the received XUV flux. However, when translated in terms of mass-loss rates, these trends seem to disappear. Thus, further studies are essential to shed light on this aspect and to better understand the photoevaporation process.

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Section: Accurate Stellar Line Profilesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Dream

Guilluy¹,

Bourrier²,

Jaziri³

et al. 2023

A&A

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“…For systems with a single transiting planet, we see that highly misaligned planets are only seen for ages 200 Myr, where the Kepler-63b system-hosting a Saturn-size planet in a 9.4 day orbit around a young 210 MYr Sun-like star-is the youngest system hosting a highly misaligned planet with Bourrier et al 2023). For older systems (1 Gyr), there is a growing population of eccentric sub-Saturns that are on misaligned orbits, including WASP-107b (Rubenzahl et al 2021), GJ 436 b (Bourrier et al 2018(Bourrier et al , 2022, GJ 3470b (Stefansson et al 2022), HD 89345b (Bourrier et al 2023), and HAT-P-11b (Hirano et al 2011a;Winn et al 2010). Three of these systems-WASP-107b, GJ 3470b, and HAT-P-11bhave known outer companions or candidate outer companions that have been suggested as possible paths to explain the misalignments of the inner transiting planets via gravitational interactions.…”

Section: Obliquities As a Function Of Agementioning

confidence: 86%

NEID Reveals That the Young Warm Neptune TOI-2076 b Has a Low Obliquity

Frazier

Stefánsson

Mahadevan

et al. 2023

ApJL

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TOI-2076 b is a sub-Neptune-sized planet (R = 2.39 ± 0.10 R ⊕) that transits a young (204 ± 50 MYr) bright (V = 9.2) K-dwarf hosting a system of three transiting planets. Using spectroscopic observations obtained with the NEID spectrograph on the WIYN 3.5 m Telescope, we model the Rossiter–McLaughlin effect of TOI-2076 b, and derive a sky-projected obliquity of λ = − 3 − 15 + 16 ° . Using the size of the star (R = 0.775 ± 0.015 R ⊙), and the stellar rotation period (P rot = 7.27 ± 0.23 days), we estimate an obliquity of ψ = 18 − 9 + 10 ° (ψ < 34° at 95% confidence), demonstrating that TOI-2076 b is in a well-aligned orbit. Simultaneous diffuser-assisted photometry from the 3.5 m telescope at Apache Point Observatory rules out flares during the transit. TOI-2076 b joins a small but growing sample of young planets in compact multi-planet systems with well-aligned orbits, and is the fourth planet with an age ≲300 Myr in a multi-transiting system with an obliquity measurement. The low obliquity of TOI-2076 b and the presence of transit timing variations in the system suggest the TOI-2076 system likely formed via convergent disk migration in an initially well-aligned disk.

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“…Lately, there have been numerous measurements of the true 3D obliquities that require the stellar inclination to be measured in addition to the projected obliquity; see, e.g., Cegla et al (2016), Bourrier et al (2023), and Doyle et al (2023. Depending on the orientation of the stellar spin axis with regard to our line of sight to the observed system, the projected and 3D obliquity can be quite different from one another (see e.g., Hixenbaugh et al 2023).…”

Section: Introductionmentioning

confidence: 99%

The Orbit of Warm Jupiter WASP-106 b is Aligned with its Star

Harre,

Smith,

Hirano

et al. 2023

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Understanding orbital obliquities, or the misalignment angles between a star’s rotation axis and the orbital axis of its planets, is crucial for unraveling the mechanisms of planetary formation and migration. In this study, we present an analysis of Rossiter–McLaughlin (RM) observations of the warm Jupiter exoplanet WASP-106 b. The high-precision radial velocity measurements were made with HARPS and HARPS-N during the transit of this planet. We aim to constrain the orientation of the planet’s orbit relative to its host star’s rotation axis. The RM observations are analyzed using a code which models the RM anomaly together with the Keplerian orbit given several parameters in combination with a Markov chain Monte Carlo implementation. We measure the projected stellar obliquity in the WASP-106 system for the first time and find λ = (−1 ± 11)°, supporting the theory of quiescent migration through the disk.

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Dream

Cited by 24 publications

References 239 publications

Dream

Dream

NEID Reveals That the Young Warm Neptune TOI-2076 b Has a Low Obliquity

The Orbit of Warm Jupiter WASP-106 b is Aligned with its Star

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