-------------------------------------------------------------- Structure and Evolution of Clusters of Galaxies (Laerte Sodre) Brief program summary and its significance: Current cosmological models suggest that galaxy clusters have been formed only recently. We plan to obtain multicolor images and redshifts for galaxies in a well defined sample of clusters with z > 0.3, looking for evidences for dynamical and morphological evolution of these structures. The superb image quality and angular resolution provided by SOAR will also allow to detect arcs produced by gravitational lensing, as well as to study the spectral and morphological evolution of galaxies in clusters. Required minimum field of view (arcmin): 10 arcmin ? The bigger, the better, of course, but for clusters with z > 0.5 a fov of 5 arcmin is ok. Required psf (FWHM, profile details): 0.2-0.5 arcsec Typical target separation if multiple targets per exposure: 5-10 arcsec Signal/noise required per resolution element: 30 Typical exposure time for this S/N & lunar phase: hours Anticipated photometric dynamic range required: low What additional photometric calibrations are required? I would like to survey as many clusters as possible If IR, is tip/tilt feasible (consider isoplanatic patch)? ??? Anticipated number of separate pointings to complete program: Can this program execute in a queue? yes Anticipated post-focus instrumentation requirements (filters, gratings, etc.): Required instruments (spectral R, filters, wavelength range): optical and IR imagers; low-resolution multiobject spectrograph How soon might you need to revisit this target with another instrument? Why can't this program execute on the Blanco 4m? part of the project can be done on the Blanco, but for clusters at z > 0.5 we will need better image quality References (for non-mainstream applications): -------------------------------------------------------------- Structure and Stellar Populations of Low Surface Brightness Galaxies in the Field (Laerte Sodre) Brief program summary and its significance: Low surface brightness galaxies (LSB) are the dominant galactic population in the universe. Its study has impact in many areas, like the barion content of the universe, the nature of the faint blue galaxies that causes the excess in galaxy counts detected at moderate redshifts, and the epoch of galaxy formation. We plan to obtain high resolution optical and IR images for well defined samples of LSB galaxies. This will allow us to study in detail the structure of these elusive objects, and to put constraints in the history of their stellar populations. Measuring the central velocity dispersion of these objects is needed to estimate the depth of the potential well and to investigate the relation between surface brightness, luminosity and mass in these galaxies Required minimum field of view (arcmin): 5 arcmin is ok Required psf (FWHM, profile details): 0.2-0.5 arcsec Typical target separation if multiple targets per exposure: Signal/noise required per resolution element: >10 Typical exposure time for this S/N & lunar phase: minutes-hours for photometry, hours for spectroscopy, dark Anticipated photometric dynamic range required: very high (photometry) What additional photometric calibrations are required? usual If IR, is tip/tilt feasible (consider isoplanatic patch)? Anticipated number of separate pointings to complete program: several Can this program execute in a queue? yes Anticipated post-focus instrumentation requirements (filters, gratings, etc.): Required instruments (spectral R, filters, wavelength range): optical and IR imagers, low resolution spectrograph (R=2000, 4000-8000A) How soon might you need to revisit this target with another instrument? Why can't this program execute on the Blanco 4m? part of the project can be done on the Blanco, but to fully explore morphological details we will need better image quality References (for non-mainstream applications): -------------------------------------------------------------- Satellite Galaxies (Laerte Sodre) Brief program summary and its significance: Satellite galaxies are often found around bright galaxies as exemplified by our own Local Group. The study of companions of galaxies may allow us to understand the origin and evolution of galaxies, the extension of dark halos, and even to test cosmological models, because different cosmologies lead to distinct predictions about the nature of the environment around bright galaxies. We plan in this project to investigate the system of satellite galaxies of galaxies of different morphological types in a variety of environments, from quasi-isolated galaxies to strongly interacting galaxy pairs. In the first part of the program we will make high resolution images to prepare lists of satellite candidates. In the second part we will measure radial velocities for this sample (at least for the high surface brightness candidates). These data will allow us to probe dynamically the environment around bright galaxies. Required minimum field of view (arcmin): as large as possible Required psf (FWHM, profile details): 0.2-0.4 arcsec Typical target separation if multiple targets per exposure: arcsec to minutes Signal/noise required per resolution element: 100 for photometry, 5-10 for spectroscopy Typical exposure time for this S/N & lunar phase: minutes to hours Anticipated photometric dynamic range required: very high What additional photometric calibrations are required? usual If IR, is tip/tilt feasible (consider isoplanatic patch)? Anticipated number of separate pointings to complete program: Can this program execute in a queue? yes Anticipated post-focus instrumentation requirements (filters, gratings, etc.): Required instruments (spectral R, filters, wavelength range): optical and IR imagers, low resolution spectrograph (R=2000, 4000-8000A) How soon might you need to revisit this target with another instrument? Why can't this program execute on the Blanco 4m? part of the project can be done on the Blanco References (for non-mainstream applications):