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Constraining the Nature of the PDS 70 Protoplanets with VLTI/GRAVITY
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Constraining the Nature of the PDS 70 Protoplanets with VLTI/GRAVITY
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We present K-band interferometric observations of the PDS 70 protoplanets along with their host star using VLTI/GRAVITY. We obtained K-band spectra and 100 $\mu$as precision astrometry of both PDS 70 b and c in two epochs, as well as spatially resolving the hot inner disk around the star. Rejecting unstable orbits, we found a nonzero eccentricity for PDS 70 b of $0.17 \pm 0.06$, a near-circular orbit for PDS 70 c, and an orbital configuration that is consistent with the planets migrating into a 2:1 mean motion resonance. Enforcing dynamical stability, we obtained a 95% upper limit on the mass of PDS 70 b of 10 $M_\textrm{Jup}$, while the mass of PDS 70 c was unconstrained. The GRAVITY K-band spectra rules out pure blackbody models for the photospheres of both planets. Instead, the models with the most support from the data are planetary atmospheres that are dusty, but the nature of the dust is unclear. Any circumplanetary dust around these planets is not well constrained by the planets' 1-5 $\mu$m spectral energy distributions (SEDs) and requires longer wavelength data to probe with SED analysis. However with VLTI/GRAVITY, we made the first observations of a circumplanetary environment with sub-au spatial resolution, placing an upper limit of 0.3~au on the size of a bright disk around PDS 70 b.
Forward citations
Cited by 3 Pith papers
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Interpreting ALMA Multiwavelength Continuum Observations of PDS 70 c: An Optically Thick Dust Ring in the Circumplanetary Disk
An optically thick dust ring in the CPD of PDS 70 c reproduces the observed near-flat spectral index under reasonable parameters, while a ring-less drift model requires implausibly high dust inflow.
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Interpreting ALMA Multiwavelength Continuum Observations of PDS 70 c: An Optically Thick Dust Ring in the Circumplanetary Disk
An optically thick dust ring around PDS 70 c can explain the observed flat radio spectrum, whereas a smooth dust disk would require implausibly high dust inflow rates.
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Extending dynamical mass measurements: probing GI as a possible origin of mm-dust spirals
Dynamical rotation-curve fits give M_disk ≈ 0.30 M_sun for HD 97048 and ≈ 0.21 M_sun for WaOph 6, and indicate disks with mm-dust spirals have systematically lower Toomre Q.
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