Polarimetric imaging mode of VLT/SPHERE/IRDIS I. Description, data reduction, and observing strategy

被引：68

作者：

de Boer, J. ^{[1
]}

Langlois, M. ^{[2
,3
]}

van Holstein, R. G. ^{[1
,4
]}

Girard, J. H. ^{[5
]}

Mouillet, D. ^{[6
]}

Vigan, A. ^{[3
]}

Dohlen, K. ^{[3
]}

Snik, F. ^{[1
]}

Keller, C. U. ^{[1
]}

Ginski, C. ^{[1
,7
]}

Stam, D. M. ^{[8
]}

Milli, J. ^{[4
]}

Wahhaj, Z. ^{[4
]}

Kasper, M. ^{[9
]}

Schmid, H. M. ^{[10
]}

Rabou, P. ^{[6
]}

Gluck, L. ^{[6
]}

Hugot, E. ^{[3
]}

Perret, D. ^{[11
]}

Martinez, P. ^{[12
]}

Weber, L. ^{[13
]}

Pragt, J. ^{[14
]}

Sauvage, J-F ^{[15
]}

Boccaletti, A. ^{[11
]}

Le Coroller, H. ^{[3
]}

Dominik, C. ^{[7
]}

Henning, T. ^{[16
]}

Lagadec, E. ^{[12
]}

Menard, F. ^{[6
]}

Turatto, M. ^{[17
]}

Udry, S. ^{[13
]}

Chauvin, G. ^{[6
]}

Feldt, M. ^{[16
]}

Beuzit, J-L ^{[3
]}

机构：

[1] Leiden Univ, Leiden Observ, Pob 9513, NL-2300 Leiden, Netherlands

[2] Univ Lyon, Ecole Normale Super Lyon, CNRS, CRAL,UMR 5574, 46 Allee Italie, F-69364 Lyon 07, France

[3] Aix Marseille Univ, LAM, CNES, CNRS, Marseille, France

[4] European Southern Observ, Alonso Cordova 3107, Santiago 19001, Chile

[5] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[6] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

[7] Univ Amsterdam, Anton Pannekoek Inst, Sci Pk 904, Amsterdam, Netherlands

[8] Delft Univ Technol, Fac Aerosp Engn, Kluyverweg 1, NL-2629 Delft, Netherlands

[9] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[10] Swiss Fed Inst Technol, Inst Particle Phys & Astrophys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland

[11] Univ Paris Diderot, Observ Paris, CNRS, LESIA,UPMC, 5 Pl J Janssen, F-92190 Meudon, France

[12] Univ Cote dAzur, CNRS, OCA, Lagrange, France

[13] Univ Geneva, Geneva Observ, Chemin Maillettes 51, CH-1290 Versoix, Switzerland

[14] NOVA Opt Infrared Instrumentat Grp, Oude Hoogeveensedijk 4, Dwingeloo, Netherlands

[15] Off Natl Etud & Rech Aerosp, 29 Ave Div Leclerc, F-92322 Chatillon, France

[16] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[17] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 633卷

基金：

欧洲研究理事会;

关键词：

polarization; techniques: polarimetric; techniques: high angular resolution; techniques: image processing; protoplanetary disks; SPECKLE NOISE; LIGHT; DISK; POLARIZATION; PERFORMANCE;

D O I：

10.1051/0004-6361/201834989

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Polarimetric imaging is one of the most effective techniques for high-contrast imaging and for the characterization of protoplanetary disks, and it has the potential of becoming instrumental in the characterization of exoplanets. The Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) instrument installed on the Very Large Telescope (VLT) contains the InfraRed Dual-band Imager and Spectrograph (IRDIS) with a dual-beam polarimetric imaging (DPI) mode, which offers the capability of obtaining linear polarization images at high contrast and resolution. Aims. We aim to provide an overview of the polarimetric imaging mode of VLT/SPHERE/IRDIS and study its optical design to improve observing strategies and data reduction. Methods. For H-band observations of TW Hydrae, we compared two data reduction methods that correct for instrumental polarization effects in different ways: a minimization of the "noise" image (U phi), and a correction method based on a polarimetric model that we have developed, as presented in Paper II of this study. Results. We use observations of TW Hydrae to illustrate the data reduction. In the images of the protoplanetary disk around this star, we detect variability in the polarized intensity and angle of linear polarization that depend on the pointing-dependent instrument configuration. We explain these variations as instrumental polarization effects and correct for these effects using our model-based correction method. Conclusions. The polarimetric imaging mode of IRDIS has proven to be a very successful and productive high-contrast polarimetric imaging system. However, the instrument performance is strongly dependent on the specific instrument configuration. We suggest adjustments to future observing strategies to optimize polarimetric efficiency in field-tracking mode by avoiding unfavorable derotator angles. We recommend reducing on-sky data with the pipeline called IRDAP, which includes the model-based correction method (described in Paper II) to optimally account for the remaining telescope and instrumental polarization effects and to retrieve the true polarization state of the incident light.

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