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Observing the Gas Component of Circumplanetary Disks Around Wide-Orbit Planet-Mass Companions in the (Sub)Mm Regime

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Observing the Gas Component of Circumplanetary Disks Around Wide-Orbit Planet-Mass Companions in the (Sub)Mm Regime UvA-DARE (Digital Academic Repository) Observing the gas component of circumplanetary disks around wide-orbit planet-mass companions in the (sub)mm regime Rab, Ch.; Kamp, I.; Ginski, C.; Oberg, N.; Muro-Arena, G.A.; Dominik, C.; Waters, L.B.F.M.; Thi, W.-F.; Woitke, P. DOI 10.1051/0004-6361/201834899 Publication date 2019 Document Version Final published version Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Rab, C., Kamp, I., Ginski, C., Oberg, N., Muro-Arena, G. A., Dominik, C., Waters, L. B. F. M., Thi, W-F., & Woitke, P. (2019). Observing the gas component of circumplanetary disks around wide-orbit planet-mass companions in the (sub)mm regime. Astronomy & Astrophysics, 624, [A16]. https://doi.org/10.1051/0004-6361/201834899 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:07 Oct 2021 A&A 624, A16 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834899 & © ESO 2019 Astrophysics Observing the gas component of circumplanetary disks around wide-orbit planet-mass companions in the (sub)mm regime Ch. Rab1, I. Kamp1, C. Ginski2,3, N. Oberg1, G. A. Muro-Arena2, C. Dominik2, L. B. F. M. Waters4,2, W.-F. Thi5, and P. Woitke6 1 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands e-mail: [email protected] 2 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands 3 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands 4 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands 5 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany 6 SUPA, School of Physics & Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS, UK Received 17 December 2018 / Accepted 6 February 2019 ABSTRACT 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, and 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. Key words. planets and satellites: formation – submillimeter: planetary systems – stars: pre-main sequence – accretion, accretion disks – methods: numerical – planetary systems 1. Introduction CPD candidate on a wide orbit (a 215 au) around the close- binary system CS Cha. Their measured≈ polarization degree pro- In the last decade several detections of substellar or planet- vides strong evidence for the presence of dusty circumplanetary mass companions (PMCs; i.e. Mp . 20 MJ) orbiting young material around the PMC CS Cha c and is also consistent with ( 1 10 Myr) solar-like stars on wide orbits (a & 100 au) were the presence of a CPD. Their observations indicate that the com- ≈ − reported. Most of those companions show or were even detected panion is not embedded in the disk of the primary system, which via accretion tracers such as Hα or Pγ lines (e.g. Neuhäuser et al. also seems to be the case for other wide-orbit PMCs (Wu et al. 2005; Ireland et al. 2011; Bowler et al. 2011; Zhou et al. 2014; 2017a). This makes PMCs ideal targets to hunt for CPDs. Currie et al. 2014; Kraus et al. 2014; Wu et al. 2015a; Santamaría- Wu et al.(2017a) observed several wide-orbit PMCs with Miranda et al. 2018). This indicates that those objects are likely ALMA (Atacama Large Millimeter Array) but did not detect embedded in circumplanetary material and possibly host a cir- any millimetre continuum emission at the location of the PMCs. cumplanetary disk (CPD). The origin of those PMCs is still These authors concluded that the millimetre emission of the unclear; they might have been formed in protoplanetary disks via possible CPDs might be optically thick and compact with an core accretion and subsequently scattered towards wider orbits, outer radius of only rout < 1000 RJ ( 0:5 au) and therefore the formed in gravitationally unstable disks, or followed a simi- CPDs were not detected. Applying similar≈ assumptions, Wolff lar formation pathway as wide binaries (see e.g. Boss 2006; et al.(2017) derived rout < 2:9 au for the potential CPD of the Vorobyov 2013; Stamatellos & Herczeg 2015; Rodet et al. 2017). DH Tau b companion from their NOrthern Extended Millime- Using polarized light observations with SPHERE at the Very ter Array (NOEMA) continuum non-detections. In contrast to Large Telescope (VLT/SPHERE), Ginski et al.(2018) detected a those observations, Bayo et al.(2017) detected a CPD around Article published by EDP Sciences A16, page 1 of 17 A&A 624, A16 (2019) the free-floating planet-mass object OTS 44 (Mp 6 17 MJ) PRODIMO (PROtoplanetary DIsk MOdel) to self-consistently with ALMA. Their observed continuum peak flux of≈ 101− µJy at model the gas and dust component of CPDs assuming that they 233 GHz is very close to the upper limits of 100–200 µJy derived are already separated from the disk of their host star. by Wu et al.(2017a) for their CPD sample. However, the CPD In Sect.2, we describe our model for the CPD and our proce- around OTS 44 is unresolved with a beam size of 1:600 1:600 dure to produce synthetic observables. Our results are presented × (rout . 130 au at a distance of 160 pc). in Sect.3, in which we discuss the impact of disk structure, dust Although the detection of CPDs in the dust is a very impor- properties, and the radiative environment on the resulting line tant first step it does not provide constraints on the nature of and dust emission. In Sect.4, we discuss the challenges to detect the companion (i.e. mass) and the properties of the gaseous those CPDs and what we can learn from deep observations in circumplanetary material. If the gaseous CPD emission can be the (sub)mm regime. We conclude with a summary of our main spectrally and spatially resolved, observed rotation would be a findings in Sect.5. clear sign of the presence of a disk-like structure and would allow us to measure the dynamical mass of the companion. MacGregor et al.(2017) reported CO J = 3 2 and dust con- 2. Methods tinuum observations of the GQ Lup system. Their− observations indicate that the PMC GQ Lup b might be still embedded in The knowledge about CPDs around wide-orbit PMCs is still the disk of the primary, but they did not detect any signature limited. Most theoretical studies focussed on early evolutionary of a CPD nor any disturbance in the Keplerian velocity field stages during which the CPD is still embedded in their par- of the disk of the primary. These authors concluded that ent protoplanetary disks (e.g. Ayliffe & Bate 2009; Shabram & higher spatial resolution and higher sensitivity observations Boley 2013; Pérez et al. 2015; Szulágyi et al. 2018a) and most of are required to constrain the nature of GQ Lup b. Another these works only considered orbits of tens of au. In this stage the interesting example is the companion FW Tau c (White & Ghez accretion of material from the surrounding protoplanetary disk 2001; Kraus et al.
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