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SCIENCE DOCUMENTS SECTION Title Version Reference Date Coordinator Page Executive summary and fast facts 1.0 MUSE-MEM-GEN-056 04/02/2004 R. Bacon 003/007 Science case 1.3 MUSE-MEM-SCI-052 04/02/2004 R. Bacon 008/107 Exposure time calculator and performance analysis 1.2 MUSE-MEM-SCI-051 15/01/2004 R. Bacon 108/165 Science preparation and science team organisation 1.0 MUSE-MEM-SCI-053 02/02/04 R. Bacon 166/190 Data analysis software 2.2 MUSE-MEM-SCI-054 29/01/2003 E. Emsellem 190/197
This report summarizes the results of the Phase A study of the Multi Unit Spectroscopic Explorer (MUSE), a second generation VLT panoramic integral-field spectrograph operating in the visible wavelength range. MUSE has a field of 1x1 arcmin², sampled at 0.2x0.2 arcsec (Wide Field Mode, hereafter WFM), and of 7.5x7.5 arcsec², sampled at 25 milli-arcsec (Narrow Field Mode, hereafter NFM), both assisted by adaptive optics. The simultaneous spectral range is 0.465-0.93 µm, at a resolution of R~3000. MUSE couples the discovery potential of a large imaging device to the measuring capabilities of a high-quality spectrograph, while taking advantage of the increased spatial resolution provided by adaptive optics. This makes MUSE a unique and tremendously powerful instrument for discovering and characterizing objects that lie beyond the reach of even the deepest imaging surveys. The most challenging scientific and technical application, and the most important driver for the instrument design, is the study of the progenitors of normal Simulated MUSE deep field. Galaxies are coloured according to their apparent redshift. Galaxies detected by their continuum (I AB < 26.7 ) and/or by their Ly α emission (Flux > 3.9 10 -19 erg.s -1 .cm -2 ) are shown. Sampled area (in arcmin²) and sampled volume (comoving Mpc 3 ) of MUSE deep fields (red circles) versus the current Ly α surveys (cross). nearby galaxies out to redshifts beyond 6. These systems are extremely faint and can only be found by their Ly α emission. MUSE will be able detect these in large numbers (~15,000) through a set of nested surveys of different area and depth. The deepest survey will require very long integrations (80 hrs each field) and will reach a limiting flux of 3.9 10 -19 erg.s -1 .cm -2 , a factor 100 better than is achieved currently with narrow band imaging. These surveys will simultaneously address the following science goals: (i) study of intrinsically faint galaxies at high redshift, including determination of their luminosity function and clustering properties, (ii) detection of Ly α emission out to the epoch of reionization, study of the cosmic web, and determination of the nature of the reionization, (iii) study of the physics of Lyman break galaxies, including their winds and feedback to the intergalactic medium, (iv) spatially resolved spectroscopy of luminous distant galaxies, including lensed objects (v) search of lateforming population III objects, (vi) study of active nuclei at intermediate and high redshifts, (vii) mapping of the growth of MUSE Phase A Executive Summary version 1.0 page 1/4
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to achieve. To show the importance
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ANNEX - ETC mathcad sheet Roland Ba
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Science preparation and key personn
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Title: Science preparation and key
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If we interpret the broad width of
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5. Science team organization Title:
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8. Curriculum vitae We give here sh
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Reference: MUSE-MEM-SCI-054 Issue:
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