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Title: Science Case Reference: MUSE-MEM-SCI-052 Issue: 1.3 Date: 04/02/2004 Page: 17/100 6x10 -18 flux level of GRAPES, GalICS predicts about 85 galaxies at z>4 in the 11.3 arcmin 2 field of view of the ACS, <strong>for</strong> about 60h of observing time (at a cost of 0.7 h per galaxy), a projection that is quite sensitive to the flux threshold, but lies on the conservative side of the estimates made by the GRAPES team. Of course, if it turns out that GRAPES gets more objects, the efficiency of MUSE will be correspondingly increased. In any case, this makes MUSE deep fields significantly more efficient than current narrow-band surveys, and even than HST deep surveys, to find bona-fide faint Ly α emitters. Moreover, according to these models, most of the objects detected by MUSE at 4
Title: Science Case Reference: MUSE-MEM-SCI-052 Issue: 1.3 Date: 04/02/2004 Page: 18/100 and the SFR history within these objects. Under the assumption that 1 M sun /yr produces 10 42 erg/s (Kennicutt 1988), and that only 15 % of these photons actually escape from the galaxies, the MUSE Ly α luminosity function will probe objects that emit 10 41 erg/s at z~5.7 (currently it gets down to 5 10 42 erg/s, Ajiki et al. 2003), that translates into SFRs lower than 1 M sun /yr, up to objects which emit 10 43 erg/s and have more than 100 M sun /yr. Figure 2-4: The median descendant mass of galaxies studied in various surveys. We used the GALICS simulations to construct a set of simulated galaxies at cosmological distances, and we applied the selection criteria appropriate to each of the surveys. For each selected galaxy the simulation was used to follow the merging tree and to derive the stellar mass at z=0. This is called the descendant mass. The deepest ongoing spectroscopic survey is the VDSS, which selects galaxies to I AB =26. It samples galaxies to a redshift of about 4.5 which are the precursors of current day-galaxies with typical masses of a few times 10 11 solar masses. MUSE goes a factor 10 deeper and samples the precursors of Milky Way type galaxies all the way to a redshift of 6.7, the end of reionization. Figure 2-5: Predictions <strong>for</strong> the 2D 2-point correlation function with the GalICS model. The line shows the values measured in the SUBARU Deep Field at a flux level of 1.1 10 -17 erg/s/cm 2 by Ouchi et al. (2003) in a thin redshift slice z=4.86±0.03, maybe dominated by a large-scale structure. The green dots show the predictions at this flux level in the redshift bin z=4.67
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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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