Orbital Motion of the Wide Planetary-Mass Companion GSC 6214-210 b: No Evidence for Dynamical Scattering

Pearce, Logan; Kraus, Adam L.; Dupuy, Trent J.; Ireland, Michael; Rizzuto, Aaron C.; Bowler, Brendan P.; Birchall, Eloise K.; Wallace, A.

doi:10.48550/arxiv.1812.08860

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“…10, we show r Hill /3 as a function of orbital distance for a selection of wide-orbit CPD candidates (all show signs of ongoing accretion) and for companions with different masses orbiting a one solar-mass star. The data to calculate the Hill radius of the CPD candidates were collected from the literature (Schmidt et al 2008;Bowler et al 2011;Wu et al 2015aWu et al ,b, 2017aWolff et al 2017;Ginski et al 2018;Pearce et al 2018). For CT Cha and GSC 06214-00210 we used the new GAIA DR2 distances of d = 192 pc (Dzib et al 2018) and d = 109 pc (Pearce et al 2018), respectively.…”

Section: Observing Wide-orbit Circumplanetary Disksmentioning

confidence: 99%

“…The data to calculate the Hill radius of the CPD candidates were collected from the literature (Schmidt et al 2008;Bowler et al 2011;Wu et al 2015aWu et al ,b, 2017aWolff et al 2017;Ginski et al 2018;Pearce et al 2018). For CT Cha and GSC 06214-00210 we used the new GAIA DR2 distances of d = 192 pc (Dzib et al 2018) and d = 109 pc (Pearce et al 2018), respectively. For all other targets the distances are d ≈ 140 − 160 pc.…”

Section: Observing Wide-orbit Circumplanetary Disksmentioning

confidence: 99%

“…leading to less massive and smaller disks. For 1RXS 1609 b an age of 10 Myr (Wu et al 2017a) is suggested and for GSC 6214-210 b the age was recently revised to 17 Myr (Pearce et al 2018). Hence they might not be the ideal candidates for a detection experiment.…”

Section: Observing Wide-orbit Circumplanetary Disksmentioning

confidence: 99%

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Observing the gas component of circumplanetary disks around wide-orbit planet-mass companions in the (sub)mm regime

Rab

Kamp

Ginski

et al. 2019

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Context. Several detections of wide-orbit planet-mass/substellar companions around young solar-like stars were reported in the last decade. The origin of those possible planets is still unclear, but accretion tracers and VLT/SPHERE observations indicate that they are surrounded by circumplanetary material or even a circumplanetary disk (CPD). Aims. We want to investigate if the gas component of disks around wide-orbit companions is detectable with current (ALMA) and future (ngVLA) (sub)mm telescopes and what constraints such gas observations can provide on the nature of the circumplanetary material and the mass of the companion. Methods. We applied the radiation thermochemical disk code PRODIMO to model the dust and gas component of passive CPDs and produced realistic synthetic observables. We considered different companion properties (mass, luminosity), disk parameters (mass, size, dust properties) and radiative environments (background fields) and compared the resulting synthetic observables to telescope sensitivities and existing dust observations. Results. The main criterion for a successful detection is the size of the CPD. At a distance of about 150 pc, a CPD with an outer radius of about 10 au is detectable with ALMA in about six hours in optically thick CO lines. Other aspects, such as the luminosity, disk inclination, and background radiation fields of the companion, are also relevant and should be considered to optimize the observing strategy for detection experiments.Conclusions. For most of the known wide-orbit planet-mass companions, their maximum theoretical disk size of one-third of the Hill radius would be sufficient to allow detection of CO lines. It is therefore feasible to detect their gas disks and constrain the mass of the companion through the kinematic signature. Even in the case of non-detections such observations provide stringent constraints on disk size and gas mass, and this information is crucial for formation theories.

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