升级高对比度成像设施领域：科学驱动力和仪器选择

论文标题

升级高对比度成像设施领域：科学驱动力和仪器选择

Upgrading the high contrast imaging facility SPHERE: science drivers and instrument choices

论文作者

Boccaletti, A., Chauvin, G., Wildi, F., Milli, J., Stadler, E., Diolaiti, E., Gratton, R., Vidal, F., Loupias, M., Langlois, M., Cantalloube, F., N'Diaye, M., Gratadour, D., Ferreira, F., Tallon, M., Mazoyer, J., Segransan, D., Mouillet, D., Beuzit, J. -L., Bonnefoy, M., Galicher, R., Vigan, A., Snellen, I., Feldt, M., Desidera, S., Rousseau, S., Baruffolo, A., Goulas, C., Baudoz, P., Bechet, C., Benisty, M., Bianco, A., Carry, B., Cascone, E., Charnay, B., Choquet, E., Christiaens, V., Cortecchia, F., de Caprio, V., De Rosa, A., Desgrange, C., D'Orazi, V., Douté, S., Frangiamore, M., Gendron, E., Ginski, C., Huby, E., Keller, C., Kulcsár, C., Landman, R., Lagarde, S., Lagadec, E., Lagrange, A. -M., Kasper, M. Lombini M., Ménard, F., Magnard, Y., Malaguti, G., Maurel, D., Mesa, D., Morgante, G., Pantin, E., Pichon, T., Potier, A., Rabou, P., Rochat, S., Terenzi, L., Thiébaut, E., Tallon-Bosc, I., Raynaud, H. -F., Rouan, D., Sevin, A., Schiavone, F., Schreiber, L., Zanutta, A.

论文摘要

Sphere+是VLT处的Sphere仪器提出的升级，旨在促进当前的外系和磁盘的检测和表征性能。 Sphere+还将作为欧洲ELT的未来星球查找器（PC）的演示者。 Sphere+的主要科学驱动因素是1/是进入雪线的大部分年轻巨型行星人口（$ 3-10 $ au），以用互补的技术（径向速度，天文学）弥合差距； 2/与与球体观察到的最年轻的（$ 1-10 $ \，MYR）的关联中的淡淡和红色目标相比，可以直接研究其出生环境中巨型行星的形成； 3/通过增加频谱分辨率以打破巨型行星大气模型中的脱落性，以提高外部大气的表征水平。实现这些目标需要增加XAO系统的带宽（从$ \ sim $ 1到3 \，kHz）以及红外线（2至3 \，mag）中的灵敏度。这些功能将由使用金字塔波前传感器在红外线中优化的第二阶段AO系统带来。作为一种新的科学仪器，中型分辨率积分光谱仪将在J和H频段中提供1000至5000的光谱分辨率。本文概述了科学驱动力，需求和关键工具权衡取舍，这些权衡为Sphere+达到最终选择的基线概念。

SPHERE+ is a proposed upgrade of the SPHERE instrument at the VLT, which is intended to boost the current performances of detection and characterization for exoplanets and disks. SPHERE+ will also serve as a demonstrator for the future planet finder (PCS) of the European ELT. The main science drivers for SPHERE+ are 1/ to access the bulk of the young giant planet population down to the snow line ($3-10$ au), to bridge the gap with complementary techniques (radial velocity, astrometry); 2/ to observe fainter and redder targets in the youngest ($1-10$\,Myr) associations compared to those observed with SPHERE to directly study the formation of giant planets in their birth environment; 3/ to improve the level of characterization of exoplanetary atmospheres by increasing the spectral resolution in order to break degeneracies in giant planet atmosphere models. Achieving these objectives requires to increase the bandwidth of the xAO system (from $\sim$1 to 3\,kHz) as well as the sensitivity in the infrared (2 to 3\,mag). These features will be brought by a second stage AO system optimized in the infrared with a pyramid wavefront sensor. As a new science instrument, a medium resolution integral field spectrograph will provide a spectral resolution from 1000 to 5000 in the J and H bands. This paper gives an overview of the science drivers, requirements and key instrumental trade-off that were done for SPHERE+ to reach the final selected baseline concept.

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