Augusto Damineli-IAG/USP

Brief program summary and its significance:
INNER STRUCTURE OF OUR GALAXY.

The inner structure of the Milk Way can be traced by the very young massive
stellar population found in GHII regions and UCHII.  The high transparency
of the IM in the NIR window, the optimal performance of SOAR at these wavelengths 
and the localization of the telescope under the Galactic Center, make it 
a unique facility to explore the inner Galactic regions. Some of these
regions are thought to harbor massive OB stars in the very early evolutionary
stages, very important to know the evolutionary phase of matter accretion and to diagnose 
young galaxies.  We plan to carry a survey in these regions through JHKL/narrow filter 
imaging and H K-band spectroscopy.


Required minimum field of view (arcmin): <5 arcmin

Required psf (FWHM, profile details):0.2-0.4"

Typical target separation if multiple targets per exposure:variable

Signal/noise required per resolution element:~50 at H=15(spectroscopy)
    around 30 for J=20 H=19, K=18

Typical exposure time for this S/N & lunar phase:~1/2hour/gray
                                                  
Anticipated photometric dynamic range required:~8mag

What additional photometric calibrations are required?excellent bckgd  and telluric 
                                                      lines correction

If IR, is tip/tilt feasible (consider isoplanatic patch)? yes

Anticipated number of separate pointings to complete program:~100(photometry) 
       about 300 (spectroscopy)

Can this program execute in a queue? yes

Anticipated post-focus instrumentation requirements (filters, gratings,
etc.): a)JHK spectroscopy R>3000 b)IR narrow band filters, or Fabry-Perrot 
       or tunable filters - c)JHKL broad-band filters.

Required instruments (spectral R, filters, wavelength range): (previous item)

How soon might you need to revisit this target with another instrument?the program 
 is self contained. One visit for photometry and another for followp spectroscopy.

Why can't this program execute on the Blanco 4m? Highest angular posible angular 
        resolution, to avoid stellar blens and background nebular contamination.

References (for non-mainstream applications): Hanson 7 Conti 1994, ApJ 423, 
L139, Hanson & Conti 1995 ApJ 448 L45,
Hanson, Wowarth & Conti 1996 (ApJ-subm), Wood & Churchwell 1989 ApJS 69, 831.