AMBER : Instrument description and first astrophysical results Special feature AMBER , the near-infrared spectro-interferometric three-telescope VLTI instrument
AMBER : Instrument description and first astrophysical results Special feature AMBER , the near-infrared spectro-interferometric three-telescope VLTI instrument
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AMBER：仪器描述和第一个天体物理结果 特色 AMBER，近红外光谱干涉三望远镜 VLTI 仪器
DOI：
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发表时间：
2007
期刊：
影响因子：
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通讯作者：
N. Ventura
中科院分区：
文献类型：
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作者：
R. Petrov;F. Malbet;G. Weigelt;P. Antonelli;U. Beckmann;Y. Bresson;A. Chelli;M. Dugué;G. Duvert;S. Gennari;L. Glück;P. Kern;S. Lagarde;E. L. Coarer;F. Lisi;F. Millour;K. Perraut;P. Puget;F. Rantakyrö;S. Robbe;A. Roussel;P. Salinari;E. Tatulli;G. Zins;M. Accardo;B. Acke;K. Agabi;E. Altariba;B. Arezki;E. Aristidi;C. Ba;J. Behrend;T. Blöcker;S. Bonhomme;S. Busoni;F. Cassaing;J. Clausse;J. Colin;C. Connot;A. Delboulbé;A. D. D. Souza;T. Driebe;P. Feautrier;D. Ferruzzi;T. Forveille;E. Fossat;R. Foy;D. Fraix;A. Gallardo;E. Giani;C. Gil;A. Glentzlin;M. Heiden;M. Heininger;O. H. Utrera;K. Hofmann;D. Kamm;M. Kiekebusch;S. Kraus;D. L. Contel;J. L. Contel;T. Lesourd;B. López;M. Lopez;Y. Magnard;A. Marconi;G. Mars;G. Martinot‐Lagarde;P. Mathias;P. Mege;J. Monin;D. Mouillet;D. Mourard;E. Nussbaum;K. Ohnaka;J. Pacheco;C. Perrier;Y. Rabbia;S. Rebattu;F. Reynaud;A. Richichi;A. Robini;M. Sacchettini;D. Schertl;M. Schöller;W. Solscheid;A. Spang;P. Stee;P. Stefanini;M. Tallon;I. Tallon;D. Tasso;L. Testi;F. Vakili;O. Lühe;J. Valtier;M. Vannier;N. Ventura
上下文。随着配备大口径和百米基线设施的通用科学仪器的出现，光学长基线干涉术向前迈出了关键的一步，例如甚大望远镜干涉仪(VLTI)。目标。AMBER是VLTI仪器之一，它将最多三束具有低、中、高光谱分辨率的光束组合在一起，以便在近红外波长域为紧凑的天体物理源提供毫角秒的空间分辨率。它的主要规格是基于关于年轻恒星物体、活动星系核中心区域、质量和热的太阳系外行星光谱的三个关键计划。方法：研究方法。这些关键的科学目标导致了科学规范，这些规范被用来提出并验证仪器的概念。琥珀使用单模光纤对入射信号进行滤波，实现高精度的多轴三光束组合，产生三个基线和一个闭合相位、三个光谱色散元件和特定的自校准程序。结果。琥珀测量产生光谱分散的校准能见度、色差复杂能见度和闭合阶段，使天文学家可以考虑基本成像和高精度的能见度和相位差测量。琥珀于2004年安装在帕拉纳尔天文台。我们在此描述该仪器目前的实施情况，以使天文学团体能够使用它。结论。经过两年的调试测试和初步观察，琥珀公司已经出版了它的第一份参考出版物，使其能够评估其科学潜力。
Context. Optical long-baseline interferometry is moving a crucial step forward with the advent of general-user scientific instruments that equip large aperture and hectometric baseline facilities, such as the Very Large Telescope Interferometer (VLTI). Aims. AMBER is one of the VLTI instruments that combines up to three beams with low, moderate and high spectral resolutions in order to provide milli-arcsecond spatial resolution for compact astrophysical sources in the near-infrared wavelength domain. Its main specifications are based on three key programs on young stellar objects, active galactic nuclei central regions, masses, and spectra of hot extra-solar planets. Methods. These key science goals led to scientific specifications, which were used to propose and then validate the instrument concept. AMBER uses single-mode fibers to filter the entrance signal and to reach highly accurate, multiaxial three-beam combination, yielding three baselines and a closure phase, three spectral dispersive elements, and specific self-calibration procedures. Results. The AMBER measurements yield spectrally dispersed calibrated visibilities, color-differential complex visibilities, and a closure phase allows astronomers to contemplate rudimentary imaging and highly accurate visibility and phase differential measurements. AMBER was installed in 2004 at the Paranal Observatory. We describe here the present implementation of the instrument in the configuration with which the astronomical community can access it. Conclusions. After two years of commissioning tests and preliminary observations, AMBER has produced its first refereed publications, allowing assessment of its scientific potential.