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Register a new userMOONS: a Multi-Object Optical and Near-infrared Spectrograph for the VLT
مونز: طيف طيفي متعدد الأجسام والبصري والقريب من الأشعة فوق البنفسجية للفيت ليت
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Added by
Michele Cirasuolo Dr
Publication date
2012
fields
Physics
and research's language is
English
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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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The Gemini Infrared Multi-Object Spectrograph (GIRMOS) is a powerful new instrument being built to facility-class standards for the Gemini telescope. It takes advantage of the latest developments in adaptive optics and integral field spectrographs. GIRMOS will carry out simultaneous high-angular-resolution, spatially-resolved infrared ($1-2.4$ $mu$m) spectroscopy of four objects within a two-arcminute field-of-regard by taking advantage of multi-object adaptive optics. This capability does not currently exist anywhere in the world and therefore offers significant scientific gains over a very broad range of topics in astronomical research. For example, current programs for high redshift galaxies are pushing the limits of what is possible with infrared spectroscopy at $8-10$-meter class facilities by requiring up to several nights of observing time per target. Therefore, the observation of multiple objects simultaneously with adaptive optics is absolutely necessary to make effective use of telescope time and obtain statistically significant samples for high redshift science. With an expected commissioning date of 2023, GIRMOSs capabilities will also make it a key followup instrument for the James Webb Space Telescope when it is launched in 2021, as well as a true scientific and technical pathfinder for future Thirty Meter Telescope (TMT) multi-object spectroscopic instrumentation. In this paper, we will present an overview of this instruments capabilities and overall architecture. We also highlight how this instrument lays the ground work for a future TMT early-light instrument.
This paper presents the latest optical design for the MOONS triple-arm spectrographs. MOONS will be a Multi-Object Optical and Near-infrared Spectrograph and will be installed on one of the European Southern Observatory (ESO) Very Large Telescopes (VLT). Included in this paper is a trade-off analysis of different types of collimators, cameras, dichroics and filters.
This paper is a response to a call for white papers solicited by Gemini Observatory and its Science and Technology Advisory Committee, to help define the science case and requirements for a new Gemini instrument, envisaged to consist of a single-object spectrograph at medium resolution simultaneously covering optical and near-infrared wavelengths. In this white paper we discuss the science case for an alternative new instrument, consisting instead of a multi-object, medium-resolution, high-throughput spectrograph, covering simultaneously the optical and near-infrared slices of the electromagnetic spectrum. We argue that combination of wide wavelength coverage at medium resolution with moderate multiplexing power is an innovative path that will enable the pursuit of fundamental science questions in a variety of astrophysical topics, without compromise of the science goals achievable by single-object spectroscopy on a wide baseline. We present a brief qualitative discussion of the main features of a notional hardware design that could conceivably make such an instrument viable.
Wide-field multi-object spectroscopy is a high priority for European astronomy over the next decade. Most 8-10m telescopes have a small field of view, making 4-m class telescopes a particularly attractive option for wide-field instruments. We present a science case and design drivers for a wide-field multi-object spectrograph (MOS) with integral field units for the 4.2-m William Herschel Telescope (WHT) on La Palma. The instrument intends to take advantage of a future prime-focus corrector and atmospheric-dispersion corrector that will deliver a field of view 2 deg in diameter, with good throughput from 370 to 1,000 nm. The science programs cluster into three groups needing three different resolving powers R: (1) high-precision radial-velocities for Gaia-related Milky Way dynamics, cosmological redshift surveys, and galaxy evolution studies (R = 5,000), (2) galaxy disk velocity dispersions (R = 10,000) and (3) high-precision stellar element abundances for Milky Way archaeology (R = 20,000). The multiplex requirements of the different science cases range from a few hundred to a few thousand, and a range of fibre-positioner technologies are considered. Several options for the spectrograph are discussed, building in part on published design studies for E-ELT spectrographs. Indeed, a WHT MOS will not only efficiently deliver data for exploitation of important imaging surveys planned for the coming decade, but will also serve as a test-bed to optimize the design of MOS instruments for the future E-ELT.
The Large Ultraviolet / Optical / Infrared Surveyor (LUVOIR) is one of four large mission concepts currently undergoing community study for consideration by the 2020 Astronomy and Astrophysics Decadal Survey. The LUVOIR Ultraviolet Multi-Object Spectrograph, LUMOS, is being designed to support all of the UV science requirements of LUVOIR, from exoplanet host star characterization to tomography of circumgalactic halos to water plumes on outer solar system satellites. LUMOS offers point source and multi-object spectroscopy across the UV bandpass, with multiple resolution modes to support different science goals. The instrument will provide low (R = 8,000-18,000) and medium (R = 30,000-65,000) resolution modes across the far-ultraviolet (FUV: 100-200 nm) and near-ultraviolet (NUV: 200-400 nm) windows, and a very low resolution mode (R = 500) for spectroscopic investigations of extremely faint objects in the FUV. Imaging spectroscopy will be accomplished over a 3 x 1.6 arcminute field-of-view by employing holographically-ruled diffraction gratings to control optical aberrations, microshutter arrays (MSA), advanced optical coatings for high-throughput in the FUV, and next generation large-format photon-counting detectors. The spectroscopic capabilities of LUMOS are augmented by an FUV imaging channel (100-200nm, 13 milliarcsecond angular resolution, 2 x 2 arcminute field-of-view) that will employ a complement of narrow and medium-band filters. We present an overview of LUMOS observing modes and estimated performance curves for effective area, spectral resolution, and imaging performance. Example LUMOS 100-hour Highlights observing programs are presented to demonstrate the potential power of LUVOIRs ultraviolet spectroscopic capabilities.
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