Brief program summary and its significance: Spectroscopy and Imaging of AGN (Viegas, Gruenwald, de Souza) Hubble images of AGN have shown shock fronts in the NLR and ISO results show star formation close to the center. On the other hand, the analysis of the NLR spectra indicates that shocks may be the additional energy source necessary to explain the observations. Shocks would be responsible for the high ionization lines, for far IR continuum and soft X-ray emission. Spectroscopic imaging (requires Fabry-Perrot or IFU) of close SY 2 would provide information with a spatial resolution of about 10 pc, allowing to test the shock+photoionization model. In particular, high ionization IR lines (Si VII and SI VI) provide important information about the location of the the emitting gas and its main energy source. High resolution spectroscopy with bright lines would provide the velocity field and set limits to the shock velocity. Imaging in the optical and IR bands will permit to detect star-forming regions in the NLR and the presence of dust (torus or not). Required minimum field of view (arcmin): >~ 6' Required psf (FWHM, profile details): 0.2" Typical target separation if multiple targets per exposure: --- Signal/noise required per resolution element: > 10 (spectra), > 50 (line profile) Typical exposure time for this S/N & lunar phase: dark time Anticipated photometric dynamic range required: What additional photometric calibrations are required? If IR, is tip/tilt feasible (consider isoplanatic patch)? yes Anticipated number of separate pointings to complete program: Can this program execute in a queue? yes Anticipated post-focus instrumentation requirements (filters, gratings, etc.): B V I J K filters Required instruments (spectral R, filters, wavelength range): R~ 10000, R~ 30000(profile) 3000 - 20000A How soon might you need to revisit this target with another instrument? Why can't this program execute on the Blanco 4m? spatial resolution References (for non-mainstream applications): ---------------------------------------------------------------------------- Brief program summary and its significance: Temperature and Abundances in HII Galaxies (Viegas, Gruenwald, de Souza, Telles) The chemical composition of HII Galaxies has been used to determine the primordial He abundance. The method is based on a good determination of He/H, O/H and N/H abundances. The empirical methods used to obtain the abundances require the knowledge of the gas density and temperature. Usually the temperature is obtained from the [O III] line ratio. However, observations of planetary nebulae have shown that T([OIII]) may be an overestimation of the gas temperature being higher than the gas temperature indicated by the Balmer jump. If so, the O abundances have been understimated. Observations of a giant HII region have shown the discrepancy between the Paschen temperature and the [O III] temperature. Spectrophotometry of a large number of HII Galaxies is required to analyse this temperature problem, to recalculate the abundances and to rediscuss the primordial He abundance. Required minimum field of view (arcmin): ~ 3-4' Required psf (FWHM, profile details): < 1" Typical target separation if multiple targets per exposure: -- Signal/noise required per resolution element: 30 Typical exposure time for this S/N & lunar phase: 30-60min & dark time Anticipated photometric dynamic range required: -- What additional photometric calibrations are required? If IR, is tip/tilt feasible (consider isoplanatic patch)? yes 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): R = 10000 , 3000 - 12000A How soon might you need to revisit this target with another instrument? Why can't this program execute on the Blanco 4m? yes References (for non-mainstream applications): Gonz\'alez-Delgado R.M. et al., ApJ, 437, 239 Pagel B.E.J. 1995, in The Light Element Abundances, ed. P. Crane (Springer), p 155 Viegas S.M. & Clegg R.E.S. 199 ----------------------------------------------------------------------- Brief program summary and its significance: Dimension of the QSO absorbers (Viegas, Gruenwald, de Souza) The location of the QSO aborption line systems is closely related to the ionizing radiation source. If they are in the halo of intervening galaxies, the integrated radiation from QSOs ionizes the gas and photonionization models predict large absorbers. If the systems are associated with star-forming regions, they are probably denser and smaller. The size can be obtained from the absorption lines if the volumetric density is known. The density can be obtained from the line ratios CII 1334.5/CII* 1335.7, and SiII 1260.4/SiII* 1264.7. Thus spectrophotometric observations with high resolution are required. This project has a follow-up for larger telescopes, which is deep imaging to look for the galaxies in the line of sight of the QSO. Required minimum field of view (arcmin): 4' Required psf (FWHM, profile details): Typical target separation if multiple targets per exposure: Signal/noise required per resolution element: >~50 Typical exposure time for this S/N & lunar phase: > 2 hrs, dark time Anticipated photometric dynamic range required: What additional photometric calibrations are required? 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): R~30000, 3000 - 8000A How soon might you need to revisit this target with another instrument? Why can't this program execute on the Blanco 4m? References (for non-mainstream applications):