High-resolution ALMA Observations of HD 100546: Asymmetric Circumstellar Ring and Circumplanetary Disk Upper Limits
AuthorPineda, Jaime E.
Quanz, Sascha P.
van Dishoeck, Ewine F.
Mulders, Gijs D.
Meyer, Michael R.
AffiliationUniv Arizona, Lunar & Planetary Lab
stars: individual (HD 100546)
stars: pre-main sequence
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationJaime E. Pineda et al 2019 ApJ 871 48
Rights© 2019. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractWe present long-baseline Atacama Large Millimeter/submillimeter Array observations of the 870 mu m dust continuum emission and CO (3-2) from the protoplanetary disk around the Herbig Ae/Be star HD 100546, which is one of the few systems claimed to have two young embedded planets. These observations achieve a resolution of 4 au (3.8 mas), an rms noise of 66 mu Jy beam(-1), and reveal an asymmetric ring between similar to 20 and 40 au with largely optically thin dust continuum emission. This ring is well fit by two concentric and overlapping Gaussian rings of different widths and a Vortex. In addition, an unresolved component is detected at a position consistent with the central star, which may trace the central inner disk (<2 au in radius). We report a lack of compact continuum emission at the positions of both claimed protoplanets. We use this result to constrain the circumplanetary disk (CPD) mass and size of 1.44M(circle plus) and 0.44 au in the optically thin and thick regimes, respectively, for the case of the previously directly imaged protoplanet candidate at similar to 55 au (HD 100546 b). We compare these empirical CPD constraints to previous numerical simulations. This suggests that HD 100546 b is inconsistent with several planet accretion models, while gas-starved models are also still compatible. We estimate the planetary mass as 1.65 M-J using the relation between planet, circumstellar, and circumplanetary masses derived from numerical simulations. Finally, the CO-integrated intensity map shows a possible spiral arm feature that could match the spiral features identified in near-infrared scattered light polarized emission, which suggests a real spiral feature in the disk surface that needs to be confirmed with further observations.
VersionFinal published version
SponsorsEuropean Research Council (ERC) [PALs 320620]; Swiss National Science Foundation (SNSF) Ambizione grant [PZ00P2_174115]; SNSF; Leverhulme Trust; Isaac Newton Trust; Royal Society Dorothy Hodgkin Fellowship