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Characterization of the Inner Disk around HD 141569 A from Keck/NIRC2 L-Band Vortex Coronagraphy

Mawet, Dimitri and Choquet, Élodie and Absil, Olivier and Huby, Elsa and Bottom, Michael and Serabyn, Eugene and Femenia, Bruno and Lebreton, Jérémy and Matthews, Keith and Gomez Gonzalez, Carlos A. and Wertz, Olivier and Carlomagno, Brunella and Christiaens, Valentin and Defrère, Denis and Delacroix, Christian and Forsberg, Pontus and Habraken, Serge and Jolivet, Aissa and Karlsson, Mikael and Milli, Julien and Pinte, Christophe and Piron, Pierre and Reggiani, Maddalena and Surdej, Jean and Vargas Catalan, Ernesto (2017) Characterization of the Inner Disk around HD 141569 A from Keck/NIRC2 L-Band Vortex Coronagraphy. Astronomical Journal, 153 (1). Art. No. 44. ISSN 0004-6256. https://resolver.caltech.edu/CaltechAUTHORS:20170104-111050993

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Abstract

HD 141569 A is a pre-main sequence B9.5 Ve star surrounded by a prominent and complex circumstellar disk, likely still in a transition stage from protoplanetary to debris disk phase. Here, we present a new image of the third inner disk component of HD 141569 A made in the L' band (3.8 μm) during the commissioning of the vector vortex coronagraph that has recently been installed in the near-infrared imager and spectrograph NIRC2 behind the W.M. Keck Observatory Keck II adaptive optics system. We used reference point-spread function subtraction, which reveals the innermost disk component from the inner working distance of sime23 au and up to ≃70 au. The spatial scale of our detection roughly corresponds to the optical and near-infrared scattered light, thermal Q, N, and 8.6 μm PAH emission reported earlier. We also see an outward progression in dust location from the L' band to the H band (Very Large Telescope/SPHERE image) to the visible (Hubble Space Telescope (HST)/STIS image), which is likely indicative of dust blowout. The warm disk component is nested deep inside the two outer belts imaged by HST-NICMOS in 1999 (at 406 and 245 au, respectively). We fit our new L'-band image and spectral energy distribution of HD 141569 A with the radiative transfer code MCFOST. Our best-fit models favor pure olivine grains and are consistent with the composition of the outer belts. While our image shows a putative very faint point-like clump or source embedded in the inner disk, we did not detect any true companion within the gap between the inner disk and the first outer ring, at a sensitivity of a few Jupiter masses.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.3847/1538-3881/153/1/44DOIArticle
http://iopscience.iop.org/article/10.3847/1538-3881/153/1/44PublisherArticle
https://arxiv.org/abs/1612.03091arXivDiscussion Paper
ORCID:
AuthorORCID
Mawet, Dimitri0000-0002-8895-4735
Choquet, Élodie0000-0002-9173-0740
Absil, Olivier0000-0002-4006-6237
Bottom, Michael0000-0003-1341-5531
Lebreton, Jérémy0000-0003-1476-5963
Gomez Gonzalez, Carlos A.0000-0003-2050-1710
Christiaens, Valentin0000-0002-0101-8814
Defrère, Denis0000-0003-3499-2506
Karlsson, Mikael0000-0002-2011-0851
Milli, Julien0000-0001-9325-2511
Pinte, Christophe0000-0001-5907-5179
Reggiani, Maddalena0000-0003-2911-0898
Surdej, Jean0000-0002-7005-1976
Additional Information:© 2017. The American Astronomical Society. Received 2016 September 22; revised 2016 October 31; accepted 2016 November 16; published 2017 January 4. Based on observations made at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We would like to acknowledge J.-C. Augereau for the development and the sharing of the GRaTer disk modeling tool. Support for this work was provided by NASA through Hubble Fellowship grant #HST-HF2-51355.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Facilities: W.M. Keck Observatory - , Keck II - . Software: GRaTer (Augereau et al. 1999; Lebreton et al. 2012), MCFOST (Pinte et al. 2006, 2009).
Funders:
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
NASA Hubble FellowshipHST-HF2-51355.001-A
NASANAS5-26555
Subject Keywords:planet–disk interactions; planetary systems; planets and satellites: formation; protoplanetary disks; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be
Issue or Number:1
Record Number:CaltechAUTHORS:20170104-111050993
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170104-111050993
Official Citation:Dimitri Mawet et al 2017 AJ 153 44
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:73205
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:04 Jan 2017 20:44
Last Modified:01 Nov 2019 16:46

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