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If we interpret the broad width of the emission line as being due to velocity motion of individual gas clouds, we infer line of sight velocities of ~ 500 km s −1 , suggesting a dark halo mass of 1.3 × 10 13 M , as expected for a small cluster. We compare the emission halo to the emission filaments surrounding NGC 1275, the central galaxy of the Perseus cluster. The chaotic velocity structure and the extent of the emission are similar, although the Ly α luminosity of LAB1 is two orders of magnitude larger. Combined with the lack of coherent velocity shear and the high ratio of the Ly α and X-ray flux, the comparison leads us to speculate that the emission halo of SMM J221726+0013 is powered by the interaction between cooling gas and a relatively weak out-flow from the central source. Our data do not distinguish whether this flow is driven by vigorous star formation or by a heavily obscured AGN. Title: Science preparation and key personnel Reference: MUSE-MEM-SCI-053 Issue: 1.0 Date: 02/02/04 Page: 7/25 Figure 4 SAURON cube summed in the wavelength direction to produce a continuum image, showing the QSO in the centre and some foreground stars. It is clear, however, that this interpretation needs to be confirmed by combining radiative transfer models with realistic simulations of massive galaxy formation in the early universe. The structure of emission halo suggests a cavity around SMM J221726+0013. While one possible explanation is that this region has been filled with hot, completely ionised material, the dip in the emission may equally be explained because of dust obscuration in the material ejected from the sub-millimeter source. The “mini-haloes” around the two Lyman-break galaxies in the field (C11 and C15) show clear velocity shear across their emission haloes. The structure appears to be consistent with a bipolar outflow of material, similar to Figure 5. Red dots indicate ‘detections’ of line emitting objects. For reference, continuum objects visible in figure 4 above are marked with dotted lines along the wavelength direction. Some of the detections are hence the residuals from the continuum subtraction process. Nevertheless, there are a number of other strong detections.
Title: Science preparation and key personnel Reference: MUSE-MEM-SCI-053 Issue: 1.0 Date: 02/02/04 Page: 8/25 that seen in the star-bursting dwarf galaxy M82. If the material is an out-flow, the deprojected velocity of the flow is ~200 km s −1 : less than the velocity inferred for the outflow from M82, and less than the outflow velocities inferred by Pettini et al. (1998, see also Teplitz et al., 2000) from comparison of the redshifts of Ly α and nebular emission lines in the rest-frame optical. Further Observations We have also observed a field centred on a bright QSO (HB89-1738+350). This is a V=20.5, z=3.239 QSO chosen so that its rest frame Ly α would be inside the SAURON range, but also so that the cube would include a significant range where intervening absorption systems seen along the line of sight to the QSO could be correlated with any emission line objects found in the SAURON cube. The analysis of this data set (figure 4) is still in progress, but preliminary results from work by Joris Gersson are shown in figure 5. The detection algorithm is currently under development, but follows the traditional approach of searching for single pixels with significant flux in them, and then requiring that a certain number of nearby pixels are also above some (lower) threshold. This process is run twice – once searching for positive detections, and once for negative detections to allow an estimate to be made of the number of spurious detections. References Bacon et al., 2001, MNRAS, 326, 23 Chapman, Lewis, Scott, et al., 2001, ApJ, 548, 17 Eales et al., 1999, APJ, 515, 518 Pettini M., Kellog M., Steidel C. S., Dickinson M., Adelberger K., Giavalisco M., 1998, 508, 539 Smail I., Ivison R., Blain W.A., Kneib J.-P., 2002, MNRAS, 331, 495 Steidel, Adelberger, Shapley, Pettini, Dickinson, Giavalisco, 2000, ApJ ,532, 170 Teplitz H.I., McLean I.S., Becklin E.E., 2000, ApJ, 533, L63 4.2.2. Searches for line emitting galaxies at z~6. Using existing multi-object spectrographs (e.g. FORS-2) in a multi-slit+filter mode (Crampton and Lilly 1999) enables us to carry out "blank-field" searches for line emission that are directly comparable to the integral field approach of MUSE. In these surveys, the integral field is effectively built up out of multiple long-slit exposures displaced in position. The much smaller number of pixels in FORS-2 relative to MUSE means that such a survey must necessarily be more limited in spatial coverage, spectral range, and/or spatial and spectral resolution. The FORS-2 survey being undertaken as MUSE-precursor science is only targeted at the 9000-9250 Å atmospheric window between the OH forest, which corresponds to 6.42 < z < 6.58 for Ly α . This is a particularly interesting range, since it represents the highest redshifts known. Furthermore, the evidence that the reionization of the Universe may
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The median descendant mass of galax
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with the slicer development for NIR
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Science Case Coordinator : R. Bacon
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Title: Science Case Reference: MUSE
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Keck Telescope (Rhoads et al. 2000)
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5. Solar system Title: Science Case
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Exposure Time Calculator and Perfor
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Title: ETC and performance analysis
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to achieve. To show the importance
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ANNEX - ETC mathcad sheet Roland Ba
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