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Title: Science Case Reference: MUSE-MEM-SCI-052 Issue: 1.3 Date: 04/02/2004 Page: 5/100 1. Introduction This document presents the science case for the Multi Unit Spectroscopic Explorer (MUSE). Four scientific areas have been explored: formation of galaxies, nearby galaxies science, stars and resolved stellar populations and solar system applications. The formation of galaxies (section 2) is the most challenging scientifically and technically, and has been used as the most important driver for the instrument design. It has been developed in depth, using as much as possible quantitative estimators taken either from the literature or from extensive numerical simulations. The nearby galaxy science (section 3) and the stars and stellar population (section 4) have been significantly enhanced with respect to the pre-phase A document. We have also added a new section on solar system science (section 5), although it has not been considered as a driver for the instrument. Apart from these science goals, we stress the large potential of serendipitous discoveries of MUSE (section 6). We then summarize instrument requirements in section 7 and discuss MUSE competitiveness with respect to existing or planned similar facilities in section 8.
2. Formation of galaxies Title: Science Case Reference: MUSE-MEM-SCI-052 Issue: 1.3 Date: 04/02/2004 Page: 6/100 2.1. Introduction The advent of 10-m class telescopes and high throughput instrumentation has fully opened a new research area in astronomy: the study of the overall populations of galaxies at high redshifts. At redshift 3, when the universe was 15 % of its current age, and the typical separations between objects were 1/4 of the current values, the galaxies that are unveiled by the deep surveys like the HDFs seem to be quite different from the local, giant galaxies of the Hubble sequence. Whereas, in the early nineties, only extreme objects were known in the distant universe 1 , recent deep surveys based on broad-band magnitude selection can now collect large populations of galaxies from z=2 to z=3–4 (e.g., Steidel et al 1996, 1999, 2003, Madau et al. 1996). The strong spectral features of the so-called Lyman-break galaxies allow us to derive fairly accurate photometric redshifts from precise photometry. Hence deep ground-based and HST photometry can be used to sample and study fainter galaxies than can be observed spectroscopically. The ground-based studies have produced a wealth of information which we are still slowly digesting: the correlation function of Lyman break galaxies (Giavalisco et al. 1997), the existence of galactic size winds (Franx et al 1998, Pettini et al 1998, Shapley et al 2003), the interaction of winds with the IGM, the photoionizing flux (Steidel et al, 1998), the rest-frame optical properties of Lyman break galaxies, their optical emission lines, etc. These pioneering studies are now being extended to larger samples: e.g., VDSS survey (Le Fevre et al, 2003), Cosmos survey (Scoville et al, 2003), in order to obtain better statistics, and to describe the environmental dependencies. These large surveys will yield the z=3–4 equivalent of the 2DF or Sloan survey at much lower redshift. However it is clear that the current ongoing and planned surveys have intrinsic limitations that follow naturally from the capabilities of current telescopes and instruments. In order to obtain large enough samples in a reasonable time, they use integration times of typically 2 hours, and sample galaxies to a magnitude of R AB =25.5 (e.g., Steidel et al 1999), with incompleteness setting in above that limit. The consequence of this limit is that we study only the bright end of the luminosity function, and probe only a factor 10 in luminosity under the brightest objects, in a regime where the luminosity function is still rising. Furthermore, the galaxies are a very biased population of the full population, with a very strong correlation function (Giavalisco et al 1998). Even though their number density is similar to that of nearby normal galaxies (Steidel et al 1996), they are likely not the progenitors of the latter. The clustering strength is expected to depend on the number density of the halos in which galaxies reside. Assuming a simple relation between galaxy brightness and halo mass, we expect that faint galaxies cluster less than bright galaxies, and that faint galaxies are the true progenitors of normal nearby galaxies. As Lyman-break galaxies seem to be the progenitors of current giant elliptical galaxies that reside in clusters (Baugh et al 1998), we need to go a factor of 10 deeper in order to access the galaxies that are the progenitors of normal galaxies. 1 Active nuclei with very strong emission lines
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5. Solar system Title: Science Case
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Exposure Time Calculator and Perfor
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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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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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