2014A&A...572A..85Z


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST03:18:28

2014A&A...572A..85Z - Astronomy and Astrophysics, volume 572A, 85-85 (2014/12-1)

Performance of the VLT Planet Finder SPHERE. I. Photometry and astrometry precision with IRDIS and IFS in laboratory.

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. and WILDI R.F.

Abstract (from CDS):

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. 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. 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. We deduced from our analysis, for example, that β Pic b, a 12Myr old planet of ∼10MJup and semi-major axis of 9-10AU, would be detected with IRDIS with a photometric error of 0.16mag and with a relative astrometric position error of 1.1mas. With IFS, we could retrieve a spectrum with error bars of about 0.15mag on each channel and astrometric relative position error of 0.6mas. For a fainter object such as HR8799d, a 13MJup planet at a distance of 27AU, IRDIS could obtain a relative astrometric error of 3mas.

Abstract Copyright:

Journal keyword(s): instrumentation: high angular resolution - instrumentation: spectrographs - techniques: imaging spectroscopy - methods: data analysis - planetary systems

Simbad objects: 2

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Number of rows : 2

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 8049 PM* 01 19 14.8611137526 -43 37 47.429802304   10.09 9.37 9.29   K2V 42 0
2 HD 218396 El* 23 07 28.7156905667 +21 08 03.302133882   6.21 5.953     F0+VkA5mA5 896 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-03:18:28

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