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تسجيل مستخدم جديدمونز: طيف طيفي متعدد الأجسام والبصري والقريب من الأشعة فوق البنفسجية للفيت ليت
MOONS: a Multi-Object Optical and Near-infrared Spectrograph for the VLT
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تم اختيار MOONS كتصميم مفهومي جديد لمجهر الطيف البصري والقريب الأشعة تحت الحمراء المتعدد الأجسام لمجهر العدسة الضخمة (VLT)، من قبل ESO لدراسة المرحلة A. يتألف التصميم الأساسي من 1000 أشعة قابلة للتوزيع على مجال من 500 مربع درجة زاوية، وهو أكبر مجال دوري مقدم من ناسمايث في مجهر العدسة الضخمة. يغطي التردد الإجمالي 0.8um-1.8um وطورين من الدقة: الدقة المتوسطة والدقة العالية. في وضع الدقة المتوسطة (R = 4,000-6,000)، يتم مراقبة النطاق الترددي الكامل 0.8um-1.8um في وقت واحد، في حين أن وضع الدقة العالية يغطي ثلاث مناطق ترددية محددة مشتركة: واحدة حول الثلاثية الكاليوم (بدقة R = 8,000) لقياس السرعات الشعاعية، واثنين في المنطقتين R = 20,000 في المنطقة J والمنطقة H، لقياسات مفصلة لتركيزات العناصر الكيميائية. سيوفر امتصاص 8.2m من مجهر العدسة الضخمة (VLT) مع عدد كبير من الترددات والتغطية الطيفية لMOONS - التي تمتد إلى الأشعة تحت الحمراء القريبة - القوة المراقبة اللازمة لدراسة تشكيل وتطور المجرات عبر كافة تاريخ الكون، من سفينة ميلكو، من خلال صحراء الإشعاع الأحمر، وحتى عصر الإعادة التشعيب في z> 8-9. في نفس الوقت، سيسمح وضع الدقة العالية للفلكيين بدراسة تركيزات العناصر الكيميائية للنجوم في مجرتنا، وخاصة في المناطق المظلمة بشدة في البولج، وتوفير المتابعة اللازمة لمهمة جايا. يجعل هذه الخصائص والتنوع MOONS المجهر الأشعة تحت الحمراء المتعدد الأجسام المتوقع لمجهر العدسة الضخمة، والذي سيؤدي تمامًا إلى تكميل الفلكيات البصرية التي يقوم بها FLAMES وVIMOS.
MOONS is a new conceptual design for a Multi-Object Optical and Near-infrared Spectrograph for the Very Large Telescope (VLT), selected by ESO for a Phase A study. The baseline design consists of 1000 fibers deployable over a field of view of 500 square arcmin, the largest patrol field offered by the Nasmyth focus at the VLT. The total wavelength coverage is 0.8um-1.8um and two resolution modes: medium resolution and high resolution. In the medium resolution mode (R=4,000-6,000) the entire wavelength range 0.8um-1.8um is observed simultaneously, while the high resolution mode covers simultaneously three selected spectral regions: one around the CaII triplet (at R=8,000) to measure radial velocities, and two regions at R=20,000 one in the J-band and one in the H-band, for detailed measurements of chemical abundances. The grasp of the 8.2m Very Large Telescope (VLT) combined with the large multiplex and wavelength coverage of MOONS - extending into the near-IR - will provide the observational power necessary to study galaxy formation and evolution over the entire history of the Universe, from our Milky Way, through the redshift desert and up to the epoch of re-ionization at z>8-9. At the same time, the high spectral resolution mode will allow astronomers to study chemical abundances of stars in our Galaxy, in particular in the highly obscured regions of the Bulge, and provide the necessary follow-up of the Gaia mission. Such characteristics and versatility make MOONS the long-awaited workhorse near-IR MOS for the VLT, which will perfectly complement optical spectroscopy performed by FLAMES and VIMOS.
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