Dynamical traceback age of the<i>β</i>Pictoris moving group

Miret-Roig, N.; Galli, P. A. B.; Brandner, W.; Bouy, H.; Barrado, D.; Olivares, J.; Antoja, T.; Romero-Gómez, M.; Figueras, F.; Lillo-Box, J.

doi:10.1051/0004-6361/202038765

Cited by 100 publications

(85 citation statements)

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“…In Section 3 we describe the high cadence observations carried out with the three observatories, and then search these photometric time series for a transiting CPD and for a repeat of the 1981 transit event seen towards the star. Our discussion and conclusions in Section 5 cov- 1 The Lorentz Center workshop "Rocks, Rubble and Rings" held 25-30 September 2016 in Leiden, the Netherlands 2017), (4) adopted estimated which is consistent with the combination of recent estimates based on kinematics (Crundall et al 2019;Miret-Roig et al 2020), Li depletion boundary (Binks & Jeffries 2016;Shkolnik et al 2017), and isochrones (Mamajek & Bell 2014;Bell et al 2015).…”

Section: Introductionsupporting

confidence: 67%

The β Pictoris b Hill sphere transit campaign

Kenworthy

Mellon

Bailey

et al. 2021

A&A

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Aims. Photometric monitoring of β Pic in 1981 showed anomalous fluctuations of up to 4% over several days, consistent with foreground material transiting the stellar disk. The subsequent discovery of the gas giant planet β Pic b and the predicted transit of its Hill sphere to within a 0.1 au projected separation of the planet provided an opportunity to search for the transit of a circumplanetary disk (CPD) in this 21 ± 4 Myr-old planetary system. We aim to detect, or put an upper limit on, the density and nature of the material in the circumplanetary environment of the planet via the continuous photometric monitoring of the Hill sphere transit that occurred in 2017 and 2018. Methods. Continuous broadband photometric monitoring of β Pic requires ground-based observatories at multiple longitudes to provide redundancy and to provide triggers for rapid spectroscopic follow-up. These include the dedicated β Pic monitoring bRing observatories in Sutherland and Siding Springs, the ASTEP400 telescope at Concordia, and the space observatories BRITE and the Hubble Space Telescope (HST). We search the combined light curves for evidence of short-period transient events caused by rings as well as for longer-term photometric variability due to diffuse circumplanetary material. Results. We find no photometric event that matches with the event seen in November 1981, and there is no systematic photometric dimming of the star as a function of the Hill sphere radius. Conclusions. We conclude that the 1981 event was not caused by the transit of a CPD around β Pic b. The upper limit on the long-term variability of β Pic places an upper limit of 1.8 × 1022 g of dust within the Hill sphere (comparable to the ~100 km radius asteroid 16 Psyche). Circumplanetary material is either condensed into a disk that does not transit β Pic, condensed into a disk with moons that has an obliquity that does not intersect with the path of β Pic behind the Hill sphere, or is below our detection threshold. This is the first time that a dedicated international campaign has mapped the Hill sphere transit of an extrasolar gas giant planet at 10 au.

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Section: Introductionsupporting

confidence: 67%

The β Pictoris b Hill sphere transit campaign

Kenworthy

Mellon

Bailey

et al. 2021

A&A

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“…10 )) and has an age similar to that of Beta Pictoris (20 ± 10 Myr (ref. 63 )). The rotation period of V1298 Tau (2.865 ± 0.012 d (ref.…”

Section: K2 Photometrymentioning

confidence: 99%

Rapid contraction of giant planets orbiting the 20-million-year-old star V1298 Tau

et al. 2021

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Current theories of planetary evolution predict that infant giant planets have large radii and very low densities before they slowly contract to reach their final size after about several hundred million years 1,2 . These theoretical expectations remain untested so far as the detection and characterization of very young planets is extremely challenging due to the intense stellar activity of their host stars 3,4 . Only the recent discoveries of young planetary transiting systems allow initial constraints to be placed on evolutionary models [5][6][7] . With an estimated age of 20 million years, V1298 Tau is one of the youngest solar-type stars known to host transiting planets; it harbours a system composed of four planets, two Neptune-sized, one Saturn-sized and one Jupiter-sized 8,9 .Here we report a multi-instrument radial velocity campaign of V1298 Tau, which allowed us to determine the masses of two of the planets in the system. We find that the two outermost giant planets, V1298 Tau b and e (0.64 ± 0.19 and 1.16 ± 0.30 Jupiter masses, respectively), seem to contradict our knowledge of early-stages planetary evolution. According to models, they should reach their mass-radius combination only hundreds of millions of years after formation. This result suggests that giant planets can contract much more quickly than usually assumed.V1298 Tau is a relatively bright (V = 10.1), very young K1 star with a mass of 1.170 ± 0.060 M ⊙ (where M ⊙ is the solar mass), a radius of 1.278 ± 0.070 R ⊙ (where R ⊙ is the solar radius), an effective temperature of 5,050 ± 100 K and solar metallicity (Table 1 and Extended Data Fig. 1). It is the physical companion of the G2 star HD 284154. The pair belongs to the Group 29 stellar association 10 and has an age of 20 ± 10 Myr (Extended Data Figs. 1 and 2). V1298 Tau was observed by Kepler's 'Second Light' K2 mission 11 . The analysis of the K2 data revealed the presence of four transiting planets in the system 9 . The three inner planets (b, c and d) were determined to have orbital periods of 24.1396 ± 0.0018, 8.24958 ± 0.00072 and 12.4032 ± 0.0015 days, and radii of 0.916 +0.052 −0.047 , 0.499 +0.032 −0.029 and 0.572 +0.040 −0.035 R Jup (where R Jup is the Jupiter radius). The fourth planet, e, was identified with only a single transit event, with a radius of 0.780 +0.075 −0.064 R Jup and orbital period estimated to be between 40 and 120 days. A previous study constrained the mass of V1298 Tau b to be less than 2.2 M Jup (ref. 12 ) (where M Jup is the Jupiter mass).To measure the planetary masses, we performed an intensive spectroscopic campaign, collecting more than 260 radial velocity (RV) measurements of V1298 Tau using the high-resolution spectrographs HARPS-N, CARMENES, SES and HERMES between April 2019 and April 2020. To monitor its stellar activity variations, we performed contemporaneous V-band photometry using the Las Cumbres Observatory Global Telescope (LCOGT) network 13 .V1298 Tau is a very active star that induces large RV activity variations. To extract the planetary sig...

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“…6). In the remainder of this paper, we assume an age of 30 Myr for the cluster, but we believe that more study using alternative methods, such as the traceback (see Miret-Roig et al 2020) and lithium depletion boundary (see Binks & Jeffries 2014) methods, is required to provide a more robust result for the age.…”

Section: Mist Modelsmentioning

confidence: 99%

χ¹ Fornacis cluster DANCe

Galli

Bouy

Olivares

et al. 2021

A&A

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Context. The χ1 Fornacis cluster (Alessi 13) is one of a few open clusters of its age and distance in the Solar neighbourhood that ought to benefit from more attention as it can serve as a cornerstone for numerous future studies related to star and planet formation. Aims. We take advantage of the early installment of the third data release of the Gaia space mission in combination with archival data and our own observations, to expand the census of cluster members and revisit some properties of the cluster. Methods. We applied a probabilistic method to infer membership probabilities over a field of more than 1000 deg2 to select the most likely cluster members and derive the distances, spatial velocities, and physical properties of the stars in this sample. Results. We identify 164 high-probability cluster members (including 61 new members) covering the magnitude range from 5.1 to 19.6 mag in the G-band. Our sample of cluster members is complete down to 0.04 M⊙. We derive the distance of 108.4 ± 0.3 pc from Bayesian inference and confirm that the cluster is comoving with the Tucana-Horologium, Columba, and Carina young stellar associations. We investigate the kinematics of the cluster from a subsample of stars with measured radial velocities and we do not detect any significant expansion or rotation effects in the cluster. Our results suggest that the cluster is somewhat younger (about 30 Myr) than previously thought. Based on spectroscopic observations, we argue that the cluster is mass-segregated and that the distribution of spectral types shows little variation compared to other young stellar groups. Conclusions. In this study, we deliver the most complete census of cluster members that can be done with Gaia data alone and we use this new sample to provide an updated picture on the 6D structure of the cluster.

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Dynamical traceback age of theβPictoris moving group

Cited by 100 publications

References 84 publications

The β Pictoris b Hill sphere transit campaign

The β Pictoris b Hill sphere transit campaign

Rapid contraction of giant planets orbiting the 20-million-year-old star V1298 Tau

χ¹ Fornacis cluster DANCe

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Dynamical traceback age of theβPictoris moving group

Cited by 100 publications

References 84 publications

The β Pictoris b Hill sphere transit campaign

The β Pictoris b Hill sphere transit campaign

Rapid contraction of giant planets orbiting the 20-million-year-old star V1298 Tau

χ1 Fornacis cluster DANCe

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χ¹ Fornacis cluster DANCe