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Investigating the presence of two belts in the HD 15115 system

Engler, N. and Boccaletti, A. and Schmid, H. M. and Milli, J. and Augereau, J.-C. and Mazoyer, J. and Maire, A.-L. and Henning, T. and Avenhaus, H. and Baudoz, P. and Feldt, M. and Galicher, R. and Hinkley, S. and Lagrange, A.-M. and Mawet, D. and Olofsson, J. and Pantin, E. and Perrot, C. and Stapelfeldt, K. (2019) Investigating the presence of two belts in the HD 15115 system. Astronomy and Astrophysics, 622 . Art. No. A192. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20190228-135738094

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Abstract

Context. High-contrast instruments like SPHERE (Spectro- Polarimetric High-contrast Exoplanet REsearch) enable spatial resolution of young planetary systems and allow us to study the connection between planets and the dust contained in debris discs by the gravitational influence a planet can have on its environment. Aims. We present new observations of the edge-on debris disc around HD 15115 (F star at 48.2 pc) obtained in the near-IR. We search for observational evidence for a second inner planetesimal ring in the system. Methods. We obtained total intensity and polarimetric data in the broad bands J and H and processed the data with differential imaging techniques achieving an angular resolution of about 40 mas. A grid of models describing the spatial distribution of the grains in the disc is generated to constrain the geometric parameters of the disc and to explore the presence of a second belt. We perform a photometric analysis of the data and compare disc brightness in two bands in scattered and in polarized light. Results. We observe an axisymmetric planetesimal belt with a radius of ~2′′, an inclination of 85.8° ± 0.7° and position angle of 278.9° ± 0.1°. The photometric analysis shows that the west side is ~2.5 times brighter in total intensity than the east side in both bands, while for polarized light in the J band this ratio is only 1.25. We also find that the J–H colour of the disc appears to be red for the radial separations r ≲ 2′′ and is getting bluer for the larger separations. The maximum polarization fraction is 15–20% at r ~ 2.5′′. The polarized intensity image shows some structural features inside the belt which can be interpreted as an additional inner belt. Conclusions. The apparent change of disc colour from red to blue with an increasing radial separation from the star could be explained by the decreasing average grain size with distance. The presence of an inner belt slightly inclined with respect to the main planetesimal belt is suspected from the data but the analysis and modelling presented here cannot establish a firm conclusion due to the faintness of the disc and its high inclination.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361/201833542DOIArticle
https://arxiv.org/abs/1812.02750arXivDiscussion Paper
ORCID:
AuthorORCID
Engler, N.0000-0002-2719-2925
Milli, J.0000-0001-9325-2511
Mazoyer, J.0000-0002-9133-3091
Hinkley, S.0000-0001-8074-2562
Mawet, D.0000-0002-8895-4735
Additional Information:© 2019 ESO. Article published by EDP Sciences. Received 31 May 2018; Accepted 6 December 2018; Published online 20 February 2019. Based on data collected at the European Southern Observatory, Chile under programs 098.C-0686 and 096.C-0640. We would like to thank the referee for many thoughtful comments which helped to improve this paper. This work issupported by the Swiss National Science Foundation through the grant number 200020 - 162630. We acknowledge the financial support from the Programme National de Planétologie (PNP) of CNRS-INSU co-funded by the CNES, and by the Agence Nationale de la Recherche (ANR-14-CE33-0018). J.O. acknowledges financial support from the ICM (Iniciativa Científica Milenio) via the Núcleo Milenio de Formación Planetaria grant, from the Universidad de Valparaíso, and from Fondecyt (grant 1180395). J.M. acknowledges support from the NASA through the NASA Hubble Fellowship grant HST-HF2-51414.001 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.
Funders:
Funding AgencyGrant Number
Swiss National Science Foundation (SNSF)200020-162630
Programme National de Planétologie (PNP)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Institut national des sciences de l'Univers (INSU)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Agence Nationale pour la Recherche (ANR)ANR-14-CE33-0018
Iniciativa Científica MilenioUNSPECIFIED
Universidad de ValparaísoUNSPECIFIED
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1180395
NASA Hubble FellowshipHST-HF2-51414.001
NASANAS5-26555
NASA Sagan FellowshipUNSPECIFIED
Record Number:CaltechAUTHORS:20190228-135738094
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20190228-135738094
Official Citation:Investigating the presence of two belts in the HD 15115 system. N. Engler, A. Boccaletti, H. M. Schmid, J. Milli, J.-C. Augereau, J. Mazoyer, A.-L. Maire, T. Henning, H. Avenhaus, P. Baudoz, M. Feldt, R. Galicher, S. Hinkley, A.-M. Lagrange, D. Mawet, J. Olofsson, E. Pantin, C. Perrot and K. Stapelfeldt. A&A, 622 (2019) A192. DOI: https://doi.org/10.1051/0004-6361/201833542
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:93358
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:28 Feb 2019 22:22
Last Modified:28 Feb 2019 22:22

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