Detection of Continuum Submillimeter Emission Associated with Candidate Protoplanets

Isella, Andrea; Benisty, M.; Teague, Richard; Bae, Jaehan; Keppler, M.; Facchini, Stefano; Pérez, Laura

doi:10.3847/2041-8213/ab2a12

Cited by 176 publications

(217 citation statements)

References 35 publications

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“…For the CPD, simplified to a disc of 1R Hill radius centred at the planet and 0.24 R Hill high (i.e. the region around the planet with a disc-shaped overdensity), we obtain a dust mass of M CPD dust ≈ 0.003M ⊕ , which is compa- rable to the CPD measurements in PDS 70b (Isella et al 2019). Assuming a constant CPD temperature of 121 K, the continuum emission in ALMA Band 7 would be 0.07 mJy if emission is assumed optically thin, and 0.23 mJy if optically thick.…”

Section: Application To Observed Systemssupporting

confidence: 67%

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Detectability of embedded protoplanets from hydrodynamical simulations

Sanchís

Picogna

Ercolano

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We predict magnitudes for young planets embedded in transition discs, still affected by extinction due to material in the disc. We focus on Jupiter-size planets at a late stage of their formation, when the planet has carved a deep gap in the gas and dust distributions and the disc starts being transparent to the planet flux in the infrared (IR). Column densities are estimated by means of three-dimensional hydrodynamical models, performed for several planet masses. Expected magnitudes are obtained by using typical extinction properties of the disc material and evolutionary models of giant planets. For the simulated cases located at 5.2 AU in a disc with local unperturbed surface density of 127 g · cm −2 , a 1 M J planet is highly extincted in J-, H-and Kbands, with predicted absolute magnitudes ≥ 50 mag. In L-and M-bands extinction decreases, with planet magnitudes between 25 and 35 mag. In the N-band, due to the silicate feature on the dust opacities, the expected magnitude increases to ∼ 40 mag. For a 2 M J planet, the magnitudes in J-, H-and K-bands are above 22 mag, while for L-, M-and N-bands the planet magnitudes are between 15 and 20 mag. For the 5 M J planet, extinction does not play a role in any IR band, due to its ability to open deep gaps. Contrast curves are derived for the transition discs in CQ Tau, PDS 70, HL Tau, TW Hya and HD 163296. Planet mass upper-limits are estimated for the known gaps in the last two systems.

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Section: Application To Observed Systemssupporting

confidence: 67%

“…Recent H α line observations using VLT/MUSE confirmed a 8σ detection from a second companion (PDS 70c) at 240 mas (Haffert et al 2019). Dust continuum emission (likely from its CPD) has been also observed (Isella et al 2019). This second source is very close to an extended disc feature, consequently its photometry should be done with caution.…”

Section: Pds70mentioning

confidence: 95%

Detectability of embedded protoplanets from hydrodynamical simulations

Sanchís

Picogna

Ercolano

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…In the left panel we compare young companions (FU Tau b, DH Tau b, CT Cha b, ROXs 42B b, GQ Lup b) with the F disk -M relation of young star-forming regions (Taurus, Chamaeleon I, Lupus). In the right panel we compare older companions (2M1207 b, ROXs 12 b, 1RXS 1609 b, GSC 6214-210 b), as well as the the tentative ALMA detections of PDS 70 b, c (Isella et al 2019), with the relation of Upper Scorpius. Our observations tentatively suggest that young PMC disks are systematically fainter, as no disks are seen between the mean relation and the upper boundary of the intrinsic scatter.…”

Section: Disk Flux-host Mass Relationshipmentioning

confidence: 99%

“…tions of circumplanetary disks around PDS 70 b and c (73 ± 19 µJy and 106 ± 19 µJy; Isella et al 2019), with planet masses adopted from Keppler et al (2018) and Haffert et al (2019). Disk fluxes of stars and brown dwarfs are compiled from millimeter studies of starforming regions, including Taurus (Andrews et al 2013;Ricci et al 2014;Ward-Duong et al 2018), Chamaeleon I (Pascucci et al 2016;Long et al 2018), Lupus (Ansdell et al 2016;Sanchis et al 2020), and Upper Scorpius 1 (Barenfeld et al 2016;van der Plas et al 2016).…”

Section: Disk Flux-host Mass Relationshipmentioning

confidence: 99%

ALMA 0.88 mm Survey of Disks around Planetary-mass Companions

Bowler

Sheehan

et al. 2020

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Characterizing the physical properties and compositions of circumplanetary disks can provide important insights into the formation of giant planets and satellites. We report ALMA 0.88 mm (Band 7) continuum observations of six planetary-mass (10-20 M Jup ) companions: CT Cha b, 1RXS 1609 b, ROXs 12 b, ROXs 42B b, DH Tau b, and FU Tau b. No continuum sources are detected at the locations of the companions down to 3σ limits of 120-210 µJy. Given these non-detections, it is not clear whether disks around planetary-mass companions indeed follow the disk flux-host mass trend in the stellar regime. The faint radio brightness of these companion disks may result from a combination of fast radial drift and a lack of dust traps. Alternatively, as disks in binary systems are known to have significantly lower millimeter fluxes due to tidal interactions, these companion disks may instead follow the relationship of moderate-separation binary stars. This scenario can be tested with sensitive continuum imaging at rms levels of 10 µJy.

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“…A good example of robustly detected accreting planets at tens of au from a central star is the PDS 70 planetary system. This system includes a weakly accreting young star (spectral type of K7, mass of 0.8 M ⊙ , accretion rate of 6 × 10 −11 M ⊙ yr −1 , age of 5 Myr, distance of 113 pc; Pecaut & Mamajek 2016;Keppler et al 2019;Haffert et al 2019;Müller et al 2018;Gaia Collaboration et al 2018) associated with two planetary-mass companions (Haffert et al 2019;Isella et al 2019;Christiaens et al 2019a,b;Keppler et al 2018;Müller et al 2018;Wagner et al 2018). Aoyama & Ikoma (2019) estimated that PDS 70b's mass and mass accretion rate are ∼12 M Jup and ∼4 × 10 −8 M Jup yr −1 , respectively, while the values for PDS 70c are ∼10 M Jup and ∼1 × 10 −8 M Jup yr −1 .…”

Section: Introductionmentioning

confidence: 99%

Accretion Properties of PDS 70b with MUSE*

et al. 2020

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We report a new evaluation of the accretion properties of PDS 70b obtained with VLT/MUSE. The main difference from previous studies in Haffert et al. (2019) and Aoyama & Ikoma (2019) is in the mass accretion rate. Simultaneous multiple line observations, such as Hα and Hβ, can better constrain the physical properties of an accreting planet. While we clearly detected Hα emissions from PDS 70b, no Hβ emissions were detected. We estimate the line flux of Hβ with a 3-σ upper limit to be 2.3 × 10 −16 erg s −1 cm −2 . The flux ratio F Hβ /F Hα for PDS 70b is < 0.28. Numerical investigations by Aoyama et al. (2018) suggest that F Hβ /F Hα should be close to unity if the extinction is negligible. We attribute the reduction of the flux ratio to the extinction, and estimate the extinction of Hα (A Hα ) for PDS 70b to be > 2.0 mag using the interstellar extinction value. By combining with the Hα linewidth and the dereddening line luminosity of Hα, we derive the PDS 70b mass accretion rate to be 5 × 10 −7 M Jup yr −1 . The PDS 70b mass accretion rate is an order of magnitude larger than that of PDS 70. We found that the filling factor f f (the fractional area of the planetary surface emitting Hα) is 0.01, which is similar to the typical stellar value. The small value of f f indicates that the Hα emitting areas are localized at the surface of PDS 70b.

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Detection of Continuum Submillimeter Emission Associated with Candidate Protoplanets

Cited by 176 publications

References 35 publications

Detectability of embedded protoplanets from hydrodynamical simulations

Detectability of embedded protoplanets from hydrodynamical simulations

ALMA 0.88 mm Survey of Disks around Planetary-mass Companions

Accretion Properties of PDS 70b with MUSE*

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