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Simultaneous Spectral Energy Distribution and Near-infrared Interferometry Modeling of HD 142666

Davies, Claire L. and Kraus, Stefan and Harries, Tim J. and Kreplin, Alexander and Monnier, John D. and Labdon, Aaron and Kloppenborg, Brian and Acreman, David M. and Baron, Fabien and Millan-Gabet, Rafael and Sturmann, Judit and Sturmann, Laszlo and ten Brummelaar, Theo A. (2018) Simultaneous Spectral Energy Distribution and Near-infrared Interferometry Modeling of HD 142666. Astrophysical Journal, 866 (1). Art. No. 23. ISSN 1538-4357. doi:10.3847/1538-4357/aade51.

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We present comprehensive models of the Herbig Ae star, HD 142666, which aim to simultaneously explain its spectral energy distribution (SED) and near-infrared (NIR) interferometry. Our new submilliarcsecond resolution CHARA (CLASSIC and CLIMB) interferometric observations, supplemented with archival shorter baseline data from VLTI/PIONIER and the Keck Interferometer, are modeled using centrosymmetric geometric models and an axisymmetric radiative transfer code. CHARA's 330 m baselines enable us to place strong constraints on the viewing geometry, revealing a disk inclined at 58° from face-on with a 160° major axis position angle. Disk models imposing vertical hydrostatic equilibrium provide poor fits to the SED. Models accounting for disk scale height inflation, possibly induced by turbulence associated with magnetorotational instabilities, and invoking grain growth to gsim1 μm size in the disk rim are required to simultaneously reproduce the SED and measured visibility profile. However, visibility residuals for our best model fits to the SED indicate the presence of unexplained NIR emission, particularly along the apparent disk minor axis, while closure phase residuals indicate a more centrosymmetric emitting region. In addition, our inferred 58° disk inclination is inconsistent with a disk-based origin for the UX Ori-type variability exhibited by HD 142666. Additional complexity, unaccounted for in our models, is clearly present in the NIR-emitting region. We propose that the disk is likely inclined toward a more edge-on orientation and/or an optically thick outflow component also contributes to the NIR circumstellar flux.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Davies, Claire L.0000-0001-9764-2357
Kraus, Stefan0000-0001-6017-8773
Harries, Tim J.0000-0001-8228-9503
Kreplin, Alexander0000-0002-0911-9505
Monnier, John D.0000-0002-3380-3307
Labdon, Aaron0000-0001-8837-7045
Kloppenborg, Brian0000-0003-0350-5453
Acreman, David M.0000-0002-4881-7584
Baron, Fabien0000-0002-8376-8941
Millan-Gabet, Rafael0000-0003-0447-5866
ten Brummelaar, Theo A.0000-0002-0114-7915
Additional Information:© 2018. The American Astronomical Society. Received 2018 August 10; accepted 2018 August 28; published 2018 October 5. C.L.D., S.K., A.K., and A.L. acknowledge support from the ERC Starting Grant "ImagePlanetFormDiscs" (grant agreement No. 639889), STFC Rutherford fellowship/grant (ST/J004030/1, ST/K003445/1), and Philip Leverhulme Prize (PLP-2013-110). J.D.M., F.B., and B.K. acknowledge support from NSF grants AST-1210972 and AST-1506540. We would like to thank Bernard Lazareff, Jean-Baptiste Le Bouquin, and Rachel Akeson for their assistance in acquiring archival data for HD 142666. This work is based upon observations obtained with the Georgia State University Center for High Angular Resolution Astronomy Array at Mount Wilson Observatory. The CHARA Array is supported by the National Science Foundation under grant No. AST-1211929. Institutional support has been provided from the GSU College of Arts and Sciences and the GSU Office of the Vice President for Research and Economic Development. The calculations for this paper were performed on the University of Exeter Supercomputer, a DiRAC Facility jointly funded by STFC, the Large Facilities Capital Fund of BIS, and the University of Exeter. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration; the Jean-Marie Mariotti Center OiDBservice11 ; NASA's Astrophysics Data System; the VizieR catalog access tool, CDS, Strasbourg, France; the SIMBAD database, operated at CDS, Strasbourg, France; NumPy (Van Der Walt et al. 2011); matplotlib, a Python library for publication quality graphics (Hunter 2007); Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013); the Jean-Marie Mariotti Center SearchCal service12 co-developed by LAGRANGE and IPAG; and the CDS Astronomical Databases SIMBAD and VIZIER.13 This work has made use of services produced by the NASA Exoplanet Science Institute at the California Institute of Technology. Facilities: VLTI - The Very Large Telescope Interferometer, CHARA - , Keck: Interferometer - . Software: TORUS (Harries 2000; Harries et al. 2004; Kurosawa et al. 2006; Tannirkulam et al. 2007), pysynphot (STScI Development Team 2013), NumPy (Van Der Walt et al. 2011), matplotlib (Hunter 2007), Astropy (Astropy Collaboration et al. 2013).
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
European Research Council (ERC)639889
Science and Technology Facilities Council (STFC)ST/J004030/1
Science and Technology Facilities Council (STFC)ST/K003445/1
Leverhulme TrustPLP-2013-110
Georgia State UniversityUNSPECIFIED
Subject Keywords:infrared: stars; protoplanetary disks; stars: formation; stars: individual (HD 142666 ) ; stars: variables: T Tauri, Herbig Ae/Be; techniques: interferometric
Issue or Number:1
Record Number:CaltechAUTHORS:20181005-141405698
Persistent URL:
Official Citation:Claire L. Davies et al 2018 ApJ 866 23
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:90145
Deposited By: George Porter
Deposited On:05 Oct 2018 22:51
Last Modified:16 Nov 2021 00:41

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