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The 100 m OWL ESO Concept Study has undergone a full review early November 2005. The development of the concept, the conclusions of the review panel and the planned post-review actions for the European Extremely Large Telescope (ELT) to be built by ESO in the next 10 years are presented and discussed.
The 8-instrument suite studied by the ESO community in the frame of the conceptual study of the 100 m OWL telescope is briefly presented. Potential capability for unique science and the main technical challenges are identified.
The dimensional curse of having to pack 3D spectrophotometry data on solely 2D detectors is briefly discussed, and the main astronomical domains covered by 3D spectroscopy introduced. Finally, the scientific case for high spatial resolution 3D techniques coupled to Adaptive Optics capabilities is presented, with special emphasis on the observation of the nuclei of galaxies.
Preliminary results on the radial velocity field of the ring-shaped nebula N206 in the LMC are given. Several early type stars are located inside this nebula one of them being a WC5-6 star. A discussion about the kinematics of the gas around the WR star is also given.
1) Photometry from de Vaucouleurs 1958 shows a bulge obeying the r1/4 law up to less than 5 pc from the center with an effective radius re = 17′5. In the region from 0.01 to 0.2 re, equal luminosity curves are well approximated by similar ellipses of axial ratio 0.68. The reduced spatial density υ* and the reduced gravitationnal potential φ* (i.e. for a mass to luminosity ratio f equal to 1) can then be easily computed (Monnet and Simien 1977).
This paper reviews recent optical results on the large scale distribution of ionized gas in spiral galaxies, including our own. There is a diffuse, inhomogeneous emission in the arm region in spirals, including our Galaxy, and in gas-rich galaxies a fainter diffuse emission between the arms.
From 6000 optical radial velocities of H II regions a new spiral structure (4 arms of pitch angle 20°) is found. The radial velocities of the observed H II regions are the same with the velocities of the H I regions. The kinematics of H II regions is similar to that of Cepheids and B stars.
First interferometric results on M 33 in the Hα line at a dispersion of 20 Å/mm, involving 1048 radial velocities, have already been published (Carranza et al., 1968). A new analysis with 3000 measures more will be published soon.
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