First direct detection of a polarized companion outside a resolved circumbinary disk around CS Chamaeleonis

Ginski, C.; Benisty, M.; Holstein, R. van; Juhász, A.; Schmidt, T. O. B.; Chauvin, G.; Boer, J. de; Wilby, Michael J.; Manara, C. F.; Delorme, P.; Ménard, F.; Pinilla, P.; Birnstiel, T.; Flock, Mario; Keller, Christoph U.; Kenworthy, Matthew A.; Milli, J.; Olofsson, J.; Pérez, Laura; Snik, Frans; Vogt, N.

doi:10.1051/0004-6361/201732417

Cited by 44 publications

(80 citation statements)

References 93 publications

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“…The dust disk at 1.25 µm is only small enough to be unresolved with VLT/SPHERE if we use d/g = 10 −3 and our dust properties. Except for the apparent disk extension, all those models produce very similar photometric fluxes at micrometer wavelengths and are consistent with the SED presented in Ginski et al (2018).…”

Section: Cs Cha Companionsupporting

confidence: 86%

“…For the inclination we take i = 45 • except for our model of the CS Cha companion (Sect. 3.5), in which we use i = 80 • as reported by Ginski et al (2018).…”

Section: Synthetic Observablesmentioning

confidence: 99%

“…The 1.25 µm dust emission is concentrated to radii r 1 au. For a SPHERE beam of 0.031 (4.65 au at d = 150 pc) (Ginski et al 2018), the disk is therefore unresolved at distances of about 150 pc. Although the real disk size of the reference model is r out ≈ 11 au it appears as small as r out ≈ 2 au in VLT/SPHERE images.…”

Section: Observational Properties Of the Reference Modelmentioning

confidence: 99%

“…shielding of the CPD), and size of the CPD itself. For example Ginski et al (2018) concluded that for their compact CS Cha CPD model (r out = 2 au) the contribution from the stellar host is negligible. However, Wolff et al (2017) found for their model of the DH Tau system with a large CPD (r out ≈ 70 au) that the stellar radiation can efficiently heat the outer region of the CPD to temperatures of 22 K. To study the impact of enhanced background radiation, we show in Fig.…”

Section: Radiative Environmentmentioning

confidence: 99%

“…We therefore also constructed models with r out ≈ r Hill /3 by using a tapered outer edge disk structure. Assuming a semimajor axis a = 215 au (projected separation) for the orbit, a combined mass of the central binary of M * = 1 M and M p = 20 M J (Ginski et al 2018), we obtain r Hill /3 = 13.2 au for CS Cha C. To estimate r Hill we used a distance of d = 165 pc to be consistent with Ginski et al (2018). We note that recent GAIA distance estimates place the Chameleon I star formation region at 179±10 pc (GAIA DR1, Voirin et al 2018) or even at 192±6 pc (GAIA DR2, Dzib et al 2018), whereas the distance derived from the parallax reported in the GAIA DR2 catalogue (Gaia Collaboration et al 2016, 2018Lindegren et al 2018) of CS Cha is d = 176 ± 1 pc.…”

Section: Cs Cha Companionmentioning

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

A&A

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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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Section: Cs Cha Companionsupporting

confidence: 86%

“…For the inclination we take i = 45 • except for our model of the CS Cha companion (Sect. 3.5), in which we use i = 80 • as reported by Ginski et al (2018).…”

Section: Synthetic Observablesmentioning

confidence: 99%

Section: Observational Properties Of the Reference Modelmentioning

confidence: 99%

Section: Radiative Environmentmentioning

confidence: 99%

Section: Cs Cha Companionmentioning

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

A&A

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Signaturen des Lebens

Janjic

2019

Astrobiologie - Die Suche Nach Außerirdischem Leben

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The formation of planetary systems with SPICA

Kamp

Honda

Nomura

et al. 2021

Publ. Astron. Soc. Aust.

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In this era of spatially resolved observations of planet-forming disks with Atacama Large Millimeter Array (ALMA) and large ground-based telescopes such as the Very Large Telescope (VLT), Keck, and Subaru, we still lack statistically relevant information on the quantity and composition of the material that is building the planets, such as the total disk gas mass, the ice content of dust, and the state of water in planetesimals. SPace Infrared telescope for Cosmology and Astrophysics (SPICA) is an infrared space mission concept developed jointly by Japan Aerospace Exploration Agency (JAXA) and European Space Agency (ESA) to address these questions. The key unique capabilities of SPICA that enable this research are (1) the wide spectral coverage $10{-}220\,\mu\mathrm{m}$ , (2) the high line detection sensitivity of $(1{-}2) \times 10^{-19}\,\mathrm{W\,m}^{-2}$ with $R \sim 2\,000{-}5\,000$ in the far-IR (SAFARI), and $10^{-20}\,\mathrm{W\,m}^{-2}$ with $R \sim 29\,000$ in the mid-IR (SPICA Mid-infrared Instrument (SMI), spectrally resolving line profiles), (3) the high far-IR continuum sensitivity of 0.45 mJy (SAFARI), and (4) the observing efficiency for point source surveys. This paper details how mid- to far-IR infrared spectra will be unique in measuring the gas masses and water/ice content of disks and how these quantities evolve during the planet-forming period. These observations will clarify the crucial transition when disks exhaust their primordial gas and further planet formation requires secondary gas produced from planetesimals. The high spectral resolution mid-IR is also unique for determining the location of the snowline dividing the rocky and icy mass reservoirs within the disk and how the divide evolves during the build-up of planetary systems. Infrared spectroscopy (mid- to far-IR) of key solid-state bands is crucial for assessing whether extensive radial mixing, which is part of our Solar System history, is a general process occurring in most planetary systems and whether extrasolar planetesimals are similar to our Solar System comets/asteroids. We demonstrate that the SPICA mission concept would allow us to achieve the above ambitious science goals through large surveys of several hundred disks within $\sim\!2.5$ months of observing time.

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First direct detection of a polarized companion outside a resolved circumbinary disk around CS Chamaeleonis

Cited by 44 publications

References 93 publications

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

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

Signaturen des Lebens

The formation of planetary systems with SPICA

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