Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 709671.0, MPI für Astronomie / Publikationen_mpia
Performance of the VLT Planet Finder SPHERE. I. Photometry and astrometry precision with IRDIS and IFS in laboratory
Authors:Zurlo, A.; Vigan, A.; Mesa, D.; Gratton, R.; Moutou, C.; Langlois, M.; Claudi, R. U.; Pueyo, L.; Boccaletti, A.; Baruffolo, A.; Beuzit, J. -. L.; Costille, A.; Desidera, S.; Dohlen, K.; Feldt, M.; Fusco, T.; Henning, T.; Kasper, M.; Martinez, P.; Moeller-Nilsson, O.; Mouillet, D.; Pavlov, A.; Puget, P.; Sauvage, J. -. F.; Turatto, M.; Udry, S.; Vakili, F.; Waters, R.; Wildi, R. F.
Date of Publication (YYYY-MM-DD):2014
Title of Journal:Astronomy and Astrophysics
Volume:572
Start Page:id. A85 (13 pp)
Audience:Not Specified
Abstract / Description:Context. The new planet finder for the Very Large Telescope (VLT), the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE), just had its first light in Paranal. A dedicated instrument for the direct detection of planets, SPHERE, is composed of a polametric camera in visible light, the Zurich IMager POLarimeter (ZIMPOL), and two near-infrared sub-systems: the Infra-Red Dual-beam Imager and Spectrograph (IRDIS), a multi-purpose camera for imaging, polarimetry, and long-slit spectroscopy, and the integral field spectrograph (IFS), an integral field spectrograph. <BR /> Aims: We present the results obtained from the analysis of data taken during the laboratory integration and validation phase, after the injection of synthetic planets. Since no continuous field rotation could be performed in the laboratory, this analysis presents results obtained using reduction techniques that do not use the angular differential imaging (ADI) technique. <BR /> Methods: To perform the simulations, we used the instrumental point spread function (PSF) and model spectra of L and T-type objects scaled in contrast with respect to the host star. We evaluated the expected error in astrometry and photometry as a function of the signal to noise of companions, after spectral differential imaging (SDI) reduction for IRDIS and spectral deconvolution (SD) or principal component analysis (PCA) data reductions for IFS. <BR /> Results: We deduced from our analysis, for example, that beta Picb, a 12 Myr old planet of ~10 MJup and semi-major axis of 9-10 AU, would be detected with IRDIS with a photometric error of 0.16 mag and with a relative astrometric position error of 1.1 mas. With IFS, we could retrieve a spectrum with error bars of about 0.15 mag on each channel and astrometric relative position error of 0.6 mas. For a fainter object such as HR 8799d, a 13 MJup planet at a distance of 27 AU, IRDIS could obtain a relative astrometric error of 3 mas.
Free Keywords:instrumentation: high angular resolution; instrumentation: spectrographs; techniques: imaging spectroscopy; methods: data analysis; planetary systems
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-6361 %R 10.1051/0004-6361/201424204
URL:http://cdsads.u-strasbg.fr/abs/2014A%26A...572A..8...
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.