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Title: Science Case Reference: MUSE-MEM-SCI-052 Issue: 1.3 Date: 04/02/2004 Page: 19/100 Other properties can be measured for subsamples of the MUSE sources with complementary instruments such as JWST and ALMA, and subsequently SKA, to get a complete view on the extinction, gas and dust content (through the redshifted H α , CO, and HI 21 cm lines, and the submm/mm continuum emission (see more details in section 2-14 ). Even quite conservative assumptions on the expected sources demonstrate that MUSE will be the milestone instrument for the beginning of the next decade to study the properties of star forming galaxies in the distant universe. References Ajiki et al. 2003, AJ, 126, 2091 Barton et al. 2004, ApJ, submitted, astroph/0310514 Charlot & Fall 1991, ApJ, 378, 471 Charlot & Fall 1993, ApJ, 415, 580 Cole et al. 2000, MNRAS, 319, 168 Cowie & Hu 1998, AJ, 115, 1319 Devriendt et al. 1999, A&A, 350, 103 Ellis et al. 2001, ApJ, 560, 119 Franx et al 1997, ApJ, 486, 75 Fujita et al. 2003, AJ, 125, 13 Haiman & Spaans 1999, ApJ, 518, 138 Hatton et al. 2003, MNRAS, 343, 75 Hu et al. 1998, ApJ, 502, 99 Kennicutt 1988, ApJ, 334, 144 Kudritzki et al. 2000, ApJ, 536, 19 Lanzetta et al. 2002, ApJ, 570, 492 Lequeux et al. 1995, A&A, 301, 18 Ouchi et al. 2003, ApJ, 582, 60 Partridge & Peebles, 1967, ApJ, 147, 868 Rhoads et al. 2000, ApJ, 545, 85 Rhoads & Malhotra 2001, ApJ, 563, 5 Rhoads et al. 2003, AJ, 125, 1006 Shimasaku et al. 2003, ApJ, 586, 111 Silva et al. 1998, ApJ, 509, 103 Steidel et al. 2001, ApJ, 546 Stiavelli et al. 2001, ApJ, 561, 37 Valls-Gabaud 1993, ApJ, 419, 7 Venemans et al. 2002, ApJ, 569, 11 Weymann et al 1998, ApJ, 505, L95
Title: Science Case Reference: MUSE-MEM-SCI-052 Issue: 1.3 Date: 04/02/2004 Page: 20/100 2.3. Fluorescent emission and the cosmic web For the past three decades, analytic work (Zeldovich 1970) and cosmological simulations (e.g. White et al 1987, Evrard et al 1994, Furlanetto 2003) have been predicting that the first structures to form in the Universe are tangled in what has been dubbed the “cosmic web”. The picture of matter collapsing into moderately overdense sheets and filaments, with galaxies and galaxy clusters forming through continued collapse at their intersections has become common knowledge in the astronomical community. Yet, direct mapping of the cosmic web remains a challenging observational venture, especially at z ≥ 3. Several methods have been used to achieve this goal, from poking lines of sight to probe integrated one-dimensional properties (Damped Ly α system or Ly α forest studies as in e.g. Rauch 1998), to tri-dimensional surveys of galaxy populations using broad band filters (Lyman Break Galaxies e.g. Steidel et al 1999). The former method covers by construction a very limited portion of the sky since it relies on absorption behind an existing mesh of background quasars which are not spaced closely enough to yield information on a typical filament scale. As for the latter, since it only allows one to detect the brightest of sources, it also suffers from sparse sampling of the filamentary structures. However, galaxy candidates selected for their Ly α emission using deep narrow band filters are already known to sample the high redshift galaxy population at much fainter levels than studies based on continuum emission such as LBGs (see e.g. Steidel et al 2000). Therefore, one naturally expects a better sampling of the high redshift cosmic structures with such a technique. As a matter of fact, the first detection of a z = 3.04 filament by Moller & Fynbo (2001) has demonstrated the power of using Ly α emission to map the cosmic web. Moreover, mapping out filaments in their own Ly α light by finding enough star forming knots, allows one not only to probe the small fraction of baryons embedded inside galaxies but also the more diffuse emission coming from the nearby densest portions of the Inter Galactic Medium. In fact, existing analytic Figure 2-6 : Cosmological simulations of galaxy formation, with two phases of the baryonic gas taken into account(warm and hot phase with SPH, cold and molecular phase with sticky particles). At top is shown the dark matter particules, then the warm gas, cold gas, and the stars formed out the cold phase at bottom. From left to right are shown 4 successive zooms (from Semelin & Combes 2003).
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Title: Science Case Reference: MUSE
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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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8. Curriculum vitae We give here sh
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