Direct Detection of Giant Extrasolar Planets with SPHERE on the VLT

被引：0

作者：

Beuzit, J-L ^{[1
]}

Boccaletti, A. ^{[7
]}

Feldt, M. ^{[2
]}

Dohlen, K. ^{[3
]}

Mouillet, D. ^{[1
]}

Puget, P. ^{[1
]}

Wildi, F. ^{[4
]}

Abe, L. ^{[5
]}

Antichi, J. ^{[6
]}

Baruffolo, A. ^{[6
]}

Baudoz, P. ^{[7
]}

Carbillet, M. ^{[5
]}

Charton, J. ^{[1
]}

Claudi, R. ^{[6
]}

Desidera, S. ^{[6
]}

Downing, M. ^{[8
]}

Fabron, C. ^{[3
]}

Feautrier, P. ^{[1
]}

Fedrigo, E. ^{[8
]}

Fusco, T. ^{[9
]}

Gach, J-L ^{[3
]}

Giro, E. ^{[6
]}

Gratton, R. ^{[6
]}

Henning, T. ^{[2
]}

Hubin, N. ^{[8
]}

Joos, F. ^{[11
]}

Kasper, M. ^{[8
]}

Lagrange, A-M ^{[1
]}

Langlois, M. ^{[3
]}

Lenzen, R. ^{[2
]}

Moutou, C. ^{[3
]}

Pavlov, A. ^{[2
]}

Petit, C. ^{[9
]}

Pragt, J. ^{[10
]}

Rabou, P. ^{[1
]}

Rigal, F. ^{[10
]}

Rochat, S. ^{[1
]}

Roelfsema, R. ^{[10
]}

Rousset, G. ^{[7
]}

Saisse, M. ^{[3
]}

Schmid, H-M ^{[11
]}

Stadler, E. ^{[1
]}

Thalmann, C. ^{[2
]}

Turatto, M. ^{[6
]}

Udry, S. ^{[4
]}

Vakili, F. ^{[5
]}

Vigan, A. ^{[3
]}

Waters, R. ^{[12
]}

机构：

[1] Univ Grenoble 1, CNRS, LAOG, BP 53, Grenoble, France

[2] Max Planck Inst Astron, Heidelberg, Germany

[3] Univ Aix Marseille 1, CNRS, LAM, Marseille, France

[4] Observ Geneva, Sauverny, Switzerland

[5] UNS, CNRS, OCA, Nice, France

[6] INAF, Osservatorio Astron Padova, Padua, Italy

[7] CNRS Observ Paris, LESIA, Meudon, France

[8] European So Observ, Garching, Germany

[9] Off Natl Etud & Rech Aerosp, Chatillon, France

[10] NOVA ASTRON, Dwingeloo, Netherlands

[11] ETH, Astron Inst, Zurich, Switzerland

[12] Univ Amsterdam, Amsterdam, Netherlands

来源：

PATHWAYS TOWARDS HABITABLE PLANETS | 2010年 / 430卷

关键词：

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Direct detection and spectral characterization of extra-solar planets is one of the most exciting but also one of the most challenging areas in modern astronomy. The challenge consists in the very large contrast between the host star and the planet, larger than 12.5 magnitudes at very small angular separations, typically inside the seeing halo. The whole design of a "Planet Finder" instrument is therefore optimized towards reaching the highest contrast in a limited field of view and at; short distances from the central star. Both evolved and young planetary systems can be detected, respectively through their reflected light and through the intrinsic planet emission. We present the science objectives, conceptual design, and expected performance of the SPHERE instrument.

引用

页码：231 / +

页数：2

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