Erratum: “Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b” (2022, ApJL, 935, L18)

Betti, S. K.; Follette, Katherine B.; Ward-Duong, Kimberly; Aoyama, Yuhiko; Marleau, Gabriel-Dominique; Bary, Jeffrey S.; Robinson, C.; Janson, Markus; Balmer, William O.; Chauvin, G.; Palma-Bifani, P.

doi:10.3847/2041-8213/aca331

Cited by 6 publications

(7 citation statements)

References 5 publications

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“…The major difference is that this is roughly 1.7 dex smaller than the average L acc as inferred from planetary models. This is in line with the conclusions of Aoyama et al (2021) or, for Delorme 1(AB)b, Betti et al (2022aBetti et al ( , 2022b.…”

Section: Accretion Luminositysupporting

confidence: 91%

“…While several hundreds of substellar objects display convincing evidence of ongoing accretion (Betti et al 2023), only a few have masses below M p ≈ 10 M J and have been studied extensively in the last few years: PDS 70 b and c (Wagner et al 2018;Haffert et al 2019) and Delorme 1(AB)b (Eriksson et al 2020;Betti et al 2022aBetti et al , 2022bRingqvist et al 2023). It is therefore capital to enlarge this population to study the dependence of the accretion rate on object mass and age, with the prospect of better understanding the differences in formation processes from stars down to planets.…”

Section: Introductionmentioning

confidence: 99%

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Revisiting the Helium and Hydrogen Accretion Indicators at TWA 27B: Weak Mass Flow at Near-freefall Velocity

Marleau,

Aoyama,

Hashimoto

et al. 2024

ApJ

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TWA 27B (2M1207b) is the first directly imaged planetary-mass (M p ≈ 5 M J) companion and was observed at 0.9–5.3 μm with JWST/NIRSpec. To understand the accretion properties of TWA 27B, we search for continuum-subtracted near-infrared helium and hydrogen emission lines and measure their widths and luminosities. We detect the He i triplet at 4.3σ and all Paschen-series lines covered by NIRSpec (Paα, Paβ, Paγ, Paδ) at 4σ–5σ. The three brightest Brackett-series lines (Brα, Brβ, Brγ) as well as Pfγ and Pfδ are tentative detections at 2σ–3σ. We provide upper limits on the other hydrogen lines, including on Hα through Hubble Space Telescope archival data. Three lines can be reliably deconvolved to reveal an intrinsic width Δv intrsc = (67 ± 9) km s−1, which is 60% of the surface freefall velocity. The line luminosities seem significantly too high to be due to chromospheric activity. Converting line luminosities to an accretion rate yields M ̇ ≈ 5 × 10 − 9 M J yr − 1 when using scaling relationships for planetary masses, and M ̇ ≈ 0.1 × 10 − 9 M J yr − 1 with extrapolated stellar scalings. Several of these lines represent the first detections at an accretor of such low mass. The weak accretion rate implies that formation is likely over. This analysis shows that JWST can be used to measure low line-emitting mass accretion rates onto planetary-mass objects, motivates deeper searches for the mass reservoir feeding TWA 27B, and hints that other young directly imaged objects might—hitherto unbeknownst—also be accreting.

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Section: Accretion Luminositysupporting

confidence: 91%

Section: Introductionmentioning

confidence: 99%

Revisiting the Helium and Hydrogen Accretion Indicators at TWA 27B: Weak Mass Flow at Near-freefall Velocity

Marleau,

Aoyama,

Hashimoto

et al. 2024

ApJ

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“…Other hydrogen lines. Other hydrogen lines such as Hβ, Paβ, or Brγ have been observed at a few planetary-mass objects such as Delorme 1(AB)b (Eriksson et al 2020;Betti et al 2022aBetti et al , 2022b. These lines also require a similar minimum shock velocity v crit ≈ v Hα, crit = 30 km s −1 to be emitted, since their excitation energies are similar (Aoyama et al 2018).…”

Section: Further Aspects Within and Beyond Our Modelmentioning

confidence: 99%

“…It is a robust theoretical prediction that gas undergoing a shock at a velocity v 0 above a critical value, v 0 > v Hα, crit ≈ 30 km s −1 , will emit hydrogen lines as the hydrogen ionized by the shock recombines and cools in the geometrically thin postshock region (Aoyama et al 2018(Aoyama et al , 2020. There are only a few planetary-mass companions with observed line emission clearly linked to a shock: PDS 70 b and c (Wagner et al 2018;Haffert et al 2019) at Hα and Delorme 1(AB)b at several lines (Eriksson et al 2020;Betti et al 2022aBetti et al , 2022bRingqvist et al 2023). However, only the PDS 70 planets are found in a gas disk, and the others are effectively isolated.…”

Section: Introductionmentioning

confidence: 99%

The Planetary Accretion Shock. III. Smoothing-free 2.5D Simulations and Calculation of Hα Emission

Marleau

Kuiper

Béthune

et al. 2023

ApJ

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Surveys have looked for Hα emission from accreting gas giants but found very few objects. Analyses of the detections and nondetections have assumed that the entire gas flow feeding the planet is in radial freefall. However, hydrodynamical simulations suggest that this is far from reality. We calculate the Hα emission from multidimensional accretion onto a gas giant, following the gas flow from Hill sphere scales down to the circumplanetary disk (CPD) and the planetary surface. We perform azimuthally symmetric radiation hydrodynamics simulations around the planet and use modern tabulated gas and dust opacities. Crucially, contrasting with most previous simulations, we do not smooth the gravitational potential but do follow the flow down to the planetary surface, where grid cells are 0.01 Jupiter radii small. We find that roughly only 1% of the net gas inflow into the Hill sphere directly reaches the planet. As expected for ballistic infall trajectories, most of the gas falls at too large a distance on the CPD to generate Hα. Including radiation transport removes the high-velocity subsurface flow previously seen in hydrodynamics-only simulations, so that only the free planet surface and the inner regions of the CPD emit substantial Hα. Unless magnetospheric accretion, which we neglect here, additionally produces Hα, the corresponding Hα production efficiency is much smaller than usually assumed, which needs to be taken into account when analyzing (non)detection statistics.

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“…Other very low-mass YSOs, companions to T Tauri stars, have been found to exhibit similar, or even higher rates of mass accretion (Betti et al 2022;Zhou et al 2014, see Fig. 9).…”

Section: High Accretion In the Low-mass Regimementioning

confidence: 81%

New members of the Lupus I cloud based on Gaia astrometry

Majidi

Alcalá

Frasca

et al. 2023

A&A

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We characterize twelve young stellar objects (YSOs) located in the Lupus I region, spatially overlapping with the Upper Centaurus Lupus (UCL) sub-stellar association. The aim of this study is to understand whether the Lupus I cloud has more members than what has been claimed so far in the literature and gain a deeper insight into the global properties of the region. We selected our targets using Gaia DR2 catalog, based on their consistent kinematic properties with the Lupus I bona fide members. In our sample of twelve YSOs observed by X-Shooter, we identified ten Lupus I members. We could not determine the membership status of two of our targets, namely Gaia DR2 6014269268967059840 and 2MASS J15361110-3444473 due to technical issues. We found out that four of our targets are accretors, among them 2MASS J15551027-3455045, with a mass of ∼0.03 M , is one of the least massive accretors in the Lupus complex to date. Several of our targets (including accretors) are formed in-situ and off-cloud with respect to the main filaments of Lupus I, hence, our study may hint that there are diffused populations of M-dwarfs around Lupus I main filaments. In this context, we would like to emphasize that our kinematic analysis with Gaia catalogs played a key role in identifying the new members of the Lupus I cloud.

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Erratum: “Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b” (2022, ApJL, 935, L18)

Cited by 6 publications

References 5 publications

Revisiting the Helium and Hydrogen Accretion Indicators at TWA 27B: Weak Mass Flow at Near-freefall Velocity

Revisiting the Helium and Hydrogen Accretion Indicators at TWA 27B: Weak Mass Flow at Near-freefall Velocity

The Planetary Accretion Shock. III. Smoothing-free 2.5D Simulations and Calculation of Hα Emission

New members of the Lupus I cloud based on Gaia astrometry

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