MADYS: the Manifold Age Determination for Young Stars

Bonavita, M.

doi:10.1051/0004-6361/202244193

Cited by 9 publications

(8 citation statements)

References 102 publications

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“…The interstellar extinction correction was obtained from the Leike & Enßlin (2019) 3D dust map, based on Gaia Data Release 2 (DR2). Using the MADYS toolkit (Squicciarini & Bonavita 2022), the extinction was integrated in a column out to the position of Delorme 1 (AB)b, resulting in A V = 0.009 ± 0.003 mag. This is a negligible contribution.…”

Section: Appendix A: Uves Observationsmentioning

confidence: 99%

Resolved near-UV hydrogen emission lines at 40-Myr super-Jovian protoplanet Delorme 1 (AB)b

Ringqvist

Viswanath

Aoyama

et al. 2023

A&A

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Context. Accretion at planetary-mass companions (PMCs) suggests the presence of a protoplanetary disc in the system, likely accompanied by a circumplanetary disc. High-resolution spectroscopy of accreting PMCs is very difficult due to their proximity to bright host stars. For well-separated companions, however, such spectra are feasible and they are unique windows into accretion. Aims. We have followed up on our observations of the 40-Myr, and still accreting, circumbinary PMC Delorme 1 (AB)b. We used high-resolution spectroscopy to characterise the accretion process further by accessing the wealth of emission lines in the near-UV. Methods. We have used the UVES spectrograph on the ESO VLT/UT2 to obtain R λ ≈ 50000 spectroscopy, at 3300-4520 Å, of Delorme 1 (AB)b. After separating the emission of the companion from that of the M5 low-mass binary, we performed a detailed emission-line analysis, which included planetary accretion shock modelling. Results. We reaffirm ongoing accretion in Delorme 1 (AB)b and report the first detections in a (super-Jovian) protoplanet of resolved hydrogen line emission in the near-UV (Hγ, Hδ, H , H8, and H9). We tentatively detect H11, H12, He i, and Ca ii H/K. The analysis strongly favours a planetary accretion shock with a line-luminosity-based accretion rate of Ṁ = 2 × 10 −8 M J yr −1 . The lines are asymmetric and are well described by sums of narrow and broad components with different velocity shifts. The overall line shapes are best explained by a pre-shock velocity of v 0 = 170 ± 30 km s −1 , implying a planetary mass of M P = 13 ± 5 M J , and number densities of n 0 10 13 cm −3 or n 0 ∼ 10 11 cm −3 . The higher density implies a small line-emitting area of ∼ 1% relative to the planetary surface. This favours magnetospheric accretion, a case potentially strengthened by the presence of blueshifted emission in the line profiles. Conclusions. High-resolution spectroscopy offers the opportunity to resolve line profiles, which are crucial for studying the accretion process in depth. The super-Jovian protoplanet Delorme 1 (AB)b is still accreting at ∼ 40 Myr. Thus, Delorme 1 belongs to the growing family of 'Peter Pan disc' systems with (a) protoplanetary and/or circumplanetary disc(s) far beyond the typically assumed disc lifetimes. Further observations of this benchmark companion and its presumed disc(s) will help answer key questions about the accretion geometry in PMCs.

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Section: Appendix A: Uves Observationsmentioning

confidence: 99%

Resolved near-UV hydrogen emission lines at 40-Myr super-Jovian protoplanet Delorme 1 (AB)b

Ringqvist

Viswanath

Aoyama

et al. 2023

A&A

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“…Here we assume "classical" PMS evolutionary tracks as initially calculated byIben (1965) and more recently by many other researchers(Squicciarini & Bonavita 2022). There are substantial differences among the tracks, and the evolution may further differ when the effects of accretion, internal magnetic fields, and surface star spots are considered(Baraffe & Chabrier 2010;Feiden & Chaboyer 2013;Somers & Pinsonneault 2015;Kunitomo et al 2017).…”

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confidence: 99%

Magnetic Activity–Rotation–Age–Mass Relations in Late-pre-main-sequence Stars

Getman

Feigelson

Garmire

2023

ApJ

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We study the four-dimensional relationships between magnetic activity, rotation, mass, and age for solar-type stars in the age range 5–25 Myr. This is the late-pre-main-sequence (l-PMS) evolutionary phase when rapid changes in a star's interior may lead to changes in the magnetic dynamo mechanisms. We carefully derive rotational periods and spot sizes for 471 members of several l-PMS open clusters using photometric light curves from the Zwicky Transient Facility. Magnetic activity was measured in our previous Chandra-based study, and additional rotational data were obtained from other work. Several results emerge. Mass-dependent evolution of rotation through the l-PMS phase agrees with astrophysical models of stellar angular momentum changes, although the data suggest a subpopulation of stars with slower initial rotations than commonly assumed. There is a hint of the onset of unsaturated tachoclinal dependency of X-ray activity on rotation, as reported by Argiroffi et al., but this result is not confidently confirmed. Both X-ray luminosity and starspot area decrease approximately as t −1 for solar-mass stars, suggesting that spot magnetic fields are roughly constant and l-PMS stars follow the universal solar-scaling law between the X-ray luminosity and surface magnetic flux. Assuming convective dynamos are dominant, theoretical magnetic fluxes fail to reveal the universal law for l-PMS stars that enter late Henyey tracks. Altogether we emerge with a few lines of evidence suggesting that the transition from the turbulent to solar-type dynamo occurs at the later stages of l-PMS evolution as stars approach the zero-age main sequence.

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“…Inset: Relative motion between Cb and C, with C set as the primary; the error bar associated with Cb is small enough to be hidden behind the diamond. madys tool (Squicciarini & Bonavita 2022): we combined PACO (K1, K2) contrasts, the 2MASS K s magnitude of the primary (Cutri et al 2003), plus the system's color excess (E(B − V) = 0.011 ± 0.021 mag) and age (17 +3 −4 Myr). For the purpose of accounting for theoretical uncertainties on the final estimates, the computation was performed by comparison with two different models suited for the age and mass range of interest: the Ames-Dusty models (Allard et al 2001) and the BT-Settl models (Allard 2016).…”

Section: Physical Propertiesmentioning

confidence: 99%

An imaged 15 M_Jup companion within a hierarchical quadruple system

Chomez¹,

Lagrange²,

P.³

et al. 2023

A&A

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Context. Since 2019, the direct imaging B-star Exoplanet Abundance STudy (BEAST) at SPHERE@VLT has been scanning the surroundings of young B-type stars in order to ascertain the ultimate frontiers of giant planet formation. Recently, the 17−4+3 Myr HIP 81208 was found to host a close-in (∼50 au) brown dwarf and a wider (∼230 au) late M star around the central 2.6 M⊙ primary. Aims. Alongside the continuation of the survey, we are undertaking a complete reanalysis of archival data aimed at improving detection performances so as to uncover additional low-mass companions. Methods. We present here a new reduction of the observations of HIP 81208 using the patch covariance algorithm (PACO), a recent and powerful algorithm dedicated to processing high-contrast imaging datasets, as well as more classical algorithms and a dedicated point spread function subtraction approach. The combination of different techniques allowed for a reliable extraction of astrometric and photometric parameters. Results. A previously undetected source was recovered at a short separation from the C component of the system. Proper motion analysis provided robust evidence for the gravitational bond of the object to HIP 81208 C. Orbiting C at a distance of ∼20 au, this 15 MJup brown dwarf becomes the fourth object of the hierarchical HIP 81208 system. Conclusions. Among the several BEAST stars which are being found to host substellar companions, HIP 81208 stands out as a particularly striking system. As the first stellar binary system with substellar companions around each component ever found by direct imaging, it yields exquisite opportunities for thorough formation and dynamical follow-up studies.

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MADYS: the Manifold Age Determination for Young Stars

Cited by 9 publications

References 102 publications

Resolved near-UV hydrogen emission lines at 40-Myr super-Jovian protoplanet Delorme 1 (AB)b

Resolved near-UV hydrogen emission lines at 40-Myr super-Jovian protoplanet Delorme 1 (AB)b

Magnetic Activity–Rotation–Age–Mass Relations in Late-pre-main-sequence Stars

An imaged 15 M_Jup companion within a hierarchical quadruple system

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MADYS: the Manifold Age Determination for Young Stars

Cited by 9 publications

References 102 publications

Resolved near-UV hydrogen emission lines at 40-Myr super-Jovian protoplanet Delorme 1 (AB)b

Resolved near-UV hydrogen emission lines at 40-Myr super-Jovian protoplanet Delorme 1 (AB)b

Magnetic Activity–Rotation–Age–Mass Relations in Late-pre-main-sequence Stars

An imaged 15 MJup companion within a hierarchical quadruple system

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An imaged 15 M_Jup companion within a hierarchical quadruple system