Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b*

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/ac85ef

Cited by 22 publications

(24 citation statements)

References 49 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A spherical accretion geometry requires f fill ∼ 1 and would be ruled out at this n 0 , but not at n 0 ∼ 10 11 cm −3 . The higher n 0 is consistent with the estimate from Betti et al (2022).…”

Section: Discussionsupporting

confidence: 89%

“…Stellar scaling (a) Planetary scaling (b) Line Using the Aoyama et al ( 2021) planetary scaling relations and averaging the accretion rates across all H i lines yields an estimate of Ṁ = 2 × 10 −8 M J yr −1 for Delorme 1 (AB)b at this epoch (Table 1). This agrees well with the NIR-based estimate of Ṁ = (3-4) × 10 −8 M J yr −1 of Betti et al (2022), who used the same scaling relations and non-contemporaneous observations obtained within 1-5 months of the UVES epoch. Comparing these two data sets with the original MUSE detection of accretion in Eriksson et al (2020), it is possible that accretion in Delorme 1 (AB)b is variable by roughly an order of magnitude on a timescale of years.…”

Section: Discussionsupporting

confidence: 89%

“…Boucher et al 2016;Silverberg et al 2016;Murphy et al 2018;Lee et al 2020;Silverberg et al 2020). Betti et al (2022) In this Letter we present the results (Sect. 3) of our near-UV (3300-4520 Å), R λ = λ/∆λ ≈ 50000 VLT/Ultraviolet and Visual Echelle Spectrograph (UVES) observations (ID: 0108.C-0655(A)) of Delorme 1 (AB)b, which offer a unique window into an accreting protoplanet.…”

Section: Introductionmentioning

confidence: 88%

“…This is because the H7-H9 ratios hardly depend on density or temperature (set by v 0 ), due to the short collisional-transition timescale between highly excited electron levels. Therefore, unlike the lines analysed in Betti et al (2022), we cannot put constraints on n 0 or v 0 from line ratios of the higher-order lines.…”

Section: Characterising Line Profile Asymmetriesmentioning

confidence: 99%

“…Revisiting the 2018 September 18 MUSE epoch in Eriksson et al (2020) and using this planetary scaling for Hα and Hβ, we find an average log( Ṁ/M J yr −1 ) = −8.5 ± 0.1. Closest in time to the UVES epoch is the 2021 November 20 epoch near-infrared (NIR) spectrum by Betti et al (2022), for which they find an average log( Ṁ/M J yr −1 ) = −7.4 ± 0.2.…”

Section: Characterising the Near-uv H I Line Emissionmentioning

confidence: 99%

See 4 more Smart Citations

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

Ringqvist

Viswanath

Aoyama

et al. 2023

A&A

View full text Add to dashboard Cite

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.

show abstract

Section: Discussionsupporting

confidence: 89%

Section: Discussionsupporting

confidence: 89%

Section: Introductionmentioning

confidence: 88%

Section: Characterising Line Profile Asymmetriesmentioning

confidence: 99%

Section: Characterising the Near-uv H I Line Emissionmentioning

confidence: 99%

See 3 more Smart Citations

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

Ringqvist

Viswanath

Aoyama

et al. 2023

A&A

View full text Add to dashboard Cite

show abstract

New members of the Lupus I cloud based on Gaia astrometry

Majidi

Alcalá

Frasca

et al. 2023

A&A

View full text Add to dashboard Cite

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.

show abstract

Emission line variability of young 10–30 M_Jup companions

Demars,

Bonnefoy,

Dougados

et al. 2023

A&A

View full text Add to dashboard Cite

Context. Emission lines that are indicative of active accretion have been observed for a number of low-mass companions (M < 30 MJup) to stars. Line variability is ubiquitous on stellar accretors, but it has never been characterized in detail for low-mass companions. Such characterizations can offer insights into the accretion mechanism at play. Aims. We aim to characterize the short-to-long-term H I Paschen β emission line variability of two 10 to 30 MJup companions on wide orbits: GQ Lup b and GSC 06214-00210 b. We also aim to clarify their accretion mechanisms. Methods. We used J-band observations at R = 1800–2360, obtained with VLT/SINFONI in 2017, to record time-series investigations of the hours-to-weeks variability of the H I Paschen β emission line (1.282 µm). Contrary to H∝, it should be less affected by chromospheric activity contamination. The photospheric emission was analyzed at each epoch and removed with the ForMoSA forward-modeling tool, using new grids of ATMO models exploring different C/O and [M/H] values. The time series of line profiles and intensities were compared to those of more massive accretors and to predictions from the latest magnetospheric accretion and shock models. To complement these results, we also re-investigated archival spectroscopic observations at near-infrared wavelengths of each target to increase the time frame up to a decade and to build a more comprehensive understanding of the variability processes at play. Results. For GQ Lup b, we find line variability on timescales of several months to decades, whereas it is within the acceptable noise levels on shorter timescales. For GSC 06214-00210 b, we find line variability on timescales of tens of minutes all the way up to a decade. The line profiles of GSC 06214-00210 b are partially resolved in at least one epoch. Both objects show H I Paschen β flux variability that is moderate (<50%), on timescales that are below their rotation period, and that is more significant on longer timescales (up to ~1000% on decade-long timescales). This behavior resembles that of classical T Tauri stars. The line profiles of GQ Lup b are blue-shifted and can only be reproduced by magnetospheric accretion models, while those of GSC 06214-00210 b are fairly well reproduced by both magnetospheric accretion and shock models, except for one epoch for which the shock model is highly favored. The companions have C/O values broadly consistent with solar values. Conclusions. While magnetospheric accretion is favored for GQ Lup b, higher resolution (R > 10 000) observations are required to disentangle the two (non-exclusive) emitting mechanisms. The similar variability behavior observed in these low mass companions and in classical T Tauri stars may support similar accretion mechanisms. The high amplitude of variability on timescales of over a month and longer that is found for both objects could be key to explaining the low yield of H∝ imaging campaigns.

show abstract

Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b*

Cited by 22 publications

References 49 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

New members of the Lupus I cloud based on Gaia astrometry

Emission line variability of young 10–30 M_Jup companions

Contact Info

Product

Resources

About

Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b*

Cited by 22 publications

References 49 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

New members of the Lupus I cloud based on Gaia astrometry

Emission line variability of young 10–30 MJup companions

Contact Info

Product

Resources

About

Emission line variability of young 10–30 M_Jup companions