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Discovery of a directly imaged disk in scattered light around the Sco-Cen member Wray 15-788

Bohn, A. J. and Kenworthy, M. A. and Ginski, C. and Benisty, M. and De Boer, J. and Keller, C. U. and Mamajek, E. E. and Meshkat, T. and Muro-Arena, G. A. and Pecaut, M. J. and Snik, F. and Wolff, S. G. and Reggiani, M. (2019) Discovery of a directly imaged disk in scattered light around the Sco-Cen member Wray 15-788. Astronomy and Astrophysics, 624 . Art. No. A87. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20190503-133931082

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Abstract

Context. Protoplanetary disks are the birth environments of planetary systems. Therefore, the study of young, circumstellar environments is essential in understanding the processes taking place in planet formation and the evolution of planetary systems. Aims. We detect and characterize circumstellar disks and potential companions around solar-type, pre-main sequence stars in the Scorpius-Centaurus association (Sco-Cen). Methods. As part of our ongoing survey we carried out high-contrast imaging with VLT/SPHERE/IRDIS to obtain polarized and total intensity images of the young (11_(−7)^(+16) Myr old) K3IV star Wray 15-788 within the Lower Centaurus Crux subgroup of Sco-Cen. For the total intensity images, we remove the stellar halo via an approach based on reference star differential imaging in combination with principal component analysis. Results. Both total intensity and polarimetric data resolve a disk around the young, solar-like Sco-Cen member Wray 15-788. Modeling of the stellar spectral energy distribution suggests that this is a protoplanetary disk at a transition stage. We detect a bright outer ring at a projected separation of ~370 mas (≈56 au), hints of inner substructures at ~170 mas (≈28 au), and a gap in between. Within a position angle range of only 60° < ϕ < 240°, we are confident at the 5σ level that we detect actual scattered light flux from the outer ring of the disk; the remaining part is indistinguishable from background noise. For the detected part of the outer ring we determine a disk inclination of i = 21° ± 6° and a position angle of φ = 76° ± 16°. Furthermore, we find that Wray 15-788 is part of a binary system with the A2V star HD 98363 at a separation of ~50′′ (≈6900 au). Conclusions. The detection of only half of the outer ring might be due to shadowing by a misaligned inner disk. A potential substellar companion can cause the misalignment of the inner structures and can be responsible for clearing the detected gap from scattering material. However, we cannot rule out the possibility of a non-detection due to our limited signal-to-noise ratio (S/N), combined with brightness azimuthal asymmetry. From our data we can exclude companions more massive than 10 M_(jup) within the gap at a separation of ~230 mas (≈35 au). Additional data are required to characterize the disk’s peculiar morphology and to set tighter constraints on the potential perturber’s orbital parameters and mass.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361/201834523DOIArticle
https://arxiv.org/abs/1902.07723arXivDiscussion Paper
ORCID:
AuthorORCID
Bohn, A. J.0000-0003-1401-9952
Kenworthy, M. A.0000-0002-7064-8270
Mamajek, E. E.0000-0003-2008-1488
Meshkat, T.0000-0001-6126-2467
Reggiani, M.0000-0003-2911-0898
Additional Information:© 2019 ESO. Article published by EDP Sciences. Received 28 October 2018; Accepted 20 February 2019; Published online 16 April 2019. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programs 099.C-0698(A), 0101.C-0153(A), and 0101.C-0464(A). We thank C. Dominik for his extremely valuable input on infrared excesses of circumstellar disks and the anonymous referee for providing useful feedback that helped to improve the quality of this article. The research of A.J.B. and F.S. leading to these results has received funding from the European Research Council under ERC Starting Grant agreement 678194 (FALCONER). M.B. acknowledges funding from ANR of France under contract number ANR-16-CE31-0013 (Planet Forming disks). Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This publication makes use of VOSA, developed under the Spanish Virtual Observatory project supported from the Spanish MINECO through grant AyA2017-84089. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France (Wenger et al. 2000). To achieve the scientific results presented in this article we made use of the Python programming language4, especially the SciPy (Jones et al. 2001–), NumPy (Oliphant 2006), Matplotlib (Hunter 2007), scikit-image (Van der Walt et al. 2014), scikit-learn (Pedregosa et al. 2012), photutils (Bradley et al. 2016), and astropy (Astropy Collaboration 2013, 2018) packages.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
European Research Council (ERC)678194
Agence Nationale pour la Recherche (ANR)ANR-16-CE31-0013
NASA/JPL/CaltechUNSPECIFIED
Ministerio de Economía, Industria y Competitividad (MINECO)AyA2017-84089
Subject Keywords:protoplanetary disks – planets and satellites: formation – planet-disk interactions – techniques: image processing – stars: individual: Wray 15-788 – stars: individual: HD 98363
Record Number:CaltechAUTHORS:20190503-133931082
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190503-133931082
Official Citation:Discovery of a directly imaged disk in scattered light around the Sco-Cen member Wray 15-788. A. J. Bohn, M. A. Kenworthy, C. Ginski, M. Benisty, J. de Boer, C. U. Keller, E. E. Mamajek, T. Meshkat, G. A. Muro-Arena, M. J. Pecaut, F. Snik, S. G. Wolff and M. Reggiani A&A, 624 (2019) A87. DOI: https://doi.org/10.1051/0004-6361/201834523
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:95210
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:03 May 2019 21:16
Last Modified:01 Nov 2019 22:43

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