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First light of the VLT planet finder SPHERE III. New spectrophotometry and astrometry of the HR8799 exoplanetary system

Zurlo, A. and Mawet, D. (2016) First light of the VLT planet finder SPHERE III. New spectrophotometry and astrometry of the HR8799 exoplanetary system. Astronomy and Astrophysics, 587 . Art. No. A57. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20160503-085018443

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Abstract

Context. The planetary system discovered around the young A-type HR 8799 provides a unique laboratory to: a) test planet formation theories; b) probe the diversity of system architectures at these separations, and c) perform comparative (exo)planetology. Aims. We present and exploit new near-infrared images and integral-field spectra of the four gas giants surrounding HR 8799 obtained with SPHERE, the new planet finder instrument at the Very Large Telescope, during the commissioning and science verification phase of the instrument (July–December 2014). With these new data, we contribute to completing the spectral energy distribution (SED) of these bodies in the 1.0–2.5 μm range. We also provide new astrometric data, in particular for planet e, to further constrain the orbits. Methods. We used the infrared dual-band imager and spectrograph (IRDIS) subsystem to obtain pupil-stabilized, dual-band H2H3 (1.593 μm, 1.667 μm), K1K2 (2.110 μm, 2.251 μm), and broadband J (1.245 μm) images of the four planets. IRDIS was operated in parallel with the integral field spectrograph (IFS) of SPHERE to collect low-resolution (R ~ 30), near-infrared (0.94–1.64 μm) spectra of the two innermost planets HR 8799 d and e. The data were reduced with dedicated algorithms, such as the Karhunen-Loève image projection (KLIP), to reveal the planets. We used the so-called negative planets injection technique to extract their photometry, spectra, and measure their positions. We illustrate the astrometric performance of SPHERE through sample orbital fits compatible with SPHERE and literature data. Results. We demonstrated the ability of SPHERE to detect and characterize planets in this kind of systems, providing spectra and photometry of its components. The spectra improve upon the signal-to-noise ratio of previously obtained data and increase the spectral coverage down to the Y band. In addition, we provide the first detection of planet e in the J band. Astrometric positions for planets HR 8799 bcde are reported for the epochs of July, August, and December 2014. We measured the photometric values in J, H2H3, K1K2 bands for the four planets with a mean accuracy of 0.13 mag. We found upper limit constraints on the mass of a possible planet f of 3–7 M_(Jup). Our new measurements are more consistent with the two inner planets d and e being in a 2d:1e or 3d:2e resonance. The spectra of HR 8799 d and e are well matched by those of L6-8 field dwarfs. However, the SEDs of these objects are redder than field L dwarfs longward of 1.6 μm.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201526835DOIArticle
http://www.aanda.org/articles/aa/abs/2016/03/aa26835-15/aa26835-15.htmlPublisherArticle
http://arxiv.org/abs/1511.04083arXivDiscussion Paper
ORCID:
AuthorORCID
Mawet, D.0000-0002-8895-4735
Additional Information:© 2016 ESO. Received 25 June 2015. Accepted 2 November 2015. We acknowledge the two anonymous referees for their constructive comments. We are grateful to the SPHERE team and all the people at Paranal for the great effort during SPHERE commissioning runs. We especially thank A. Bellini and J. Anderson for the HST astrometric measurements. A.Z. acknowledges support from the Millennium Science Initiative (Chilean Ministry of Economy), through grant “Nucleus RC130007”. D.M., A.-L.M., R.G., R.U.C., S.D. acknowledge support from the “Progetti Premiali” funding scheme of the Italian Ministry of Education, University, and Research. We acknowledge support from the French National Research Agency (ANR) through the GUEPARD project grant ANR10-BLANC0504-01 and the Programmes Nationaux de Planétologie et de Physique Stellaire (PNP and PNPS). Part of this work has been carried out within the frame of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation. S.P.Q. and M.R.M. acknowledge the financial support of the SNSF. The author thanks Sebastián Peréz for his help in solving unsolvable latex problems. SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France), INAF – Osservatorio di Padova (Italy), Observatoire de Genève (Switzerland), ETH Zurich (Switzerland), NOVA (Netherlands), ONERA (France), and ASTRON (Netherlands), in collaboration with ESO. SPHERE was funded by ESO, with additional contributions from CNRS (France), MPIA (Germany), INAF (Italy), FINES (Switzerland), and NOVA (Netherlands). SPHERE also received funding from the European Commission Sixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (2004–2008), grant number 226604 for FP7 (2009-2012) and grant number 312430 for FP7 (2013–2016).
Funders:
Funding AgencyGrant Number
Millennium Science Initiative, Chilean ministry of EconomyNucleus RC130007
Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)UNSPECIFIED
Agence Nationale de la Recherche (ANR)ANR10-BLANC0504-01
Programmes Nationaux de Planétologie et de Physique Stellaire (PNP and PNPS)UNSPECIFIED
Swiss National Science Foundation (SNSF)UNSPECIFIED
European Southern Observatory (ESO)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Max Planck Institute for Astronomy (MPIA)UNSPECIFIED
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
FINES (Switzerland)UNSPECIFIED
Nederlandse Onderzoekschool voor de Astronomie (NOVA)UNSPECIFIED
European Commission Sixth and Seventh Framework ProgrammesRII3-Ct-2004-001566 (OPTICON)
European Commission FP7226604
European Commission FP7312430
Subject Keywords:techniques: image processing – astrometry – techniques: high angular resolution – techniques: spectroscopic – methods: data analysis
Record Number:CaltechAUTHORS:20160503-085018443
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20160503-085018443
Official Citation:First light of the VLT planet finder SPHERE - III. New spectrophotometry and astrometry of the HR 8799 exoplanetary system A. Zurlo, A. Vigan, R. Galicher, A.-L. Maire, D. Mesa, R. Gratton, G. Chauvin, M. Kasper, C. Moutou, M. Bonnefoy, S. Desidera, L. Abe, D. Apai, A. Baruffolo, P. Baudoz, J. Baudrand, J.-L. Beuzit, P. Blancard, A. Boccaletti, F. Cantalloube, M. Carle, E. Cascone, J. Charton, R. U. Claudi, A. Costille, V. de Caprio, K. Dohlen, C. Dominik, D. Fantinel, P. Feautrier, M. Feldt, T. Fusco, P. Gigan, J. H. Girard, D. Gisler, L. Gluck, C. Gry, T. Henning, E. Hugot, M. Janson, M. Jaquet, A.-M. Lagrange, M. Langlois, M. Llored, F. Madec, Y. Magnard, P. Martinez, D. Maurel, D. Mawet, M. R. Meyer, J. Milli, O. Moeller-Nilsson, D. Mouillet, A. Origné, A. Pavlov, C. Petit, P. Puget, S. P. Quanz, P. Rabou, J. Ramos, G. Rousset, A. Roux, B. Salasnich, G. Salter, J.-F. Sauvage, H. M. Schmid, C. Soenke, E. Stadler, M. Suarez, M. Turatto, S. Udry, F. Vakili, Z. Wahhaj, F. Wildi and J. Antichi A&A, 587 (2016) A57 DOI: http://dx.doi.org/10.1051/0004-6361/201526835
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:66608
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:03 May 2016 17:34
Last Modified:03 May 2016 17:34

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