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Brief program summary and its significance: 
MAGNETIC FIELD STRUCTURE OF THE INTERSTELLAR MEDIUM 
(A.M. Magalhaes)
 
The observed stellar formation rate in molecular dark clouds is not 
as high as it would be if the clouds were simply under gravitational 
collapse. Other mechanisms, such as magnetic fields and turbulent 
motion, must influence the evolution of a given cloud. The determination 
of the magnetic field is hence crucial to understand the clouds' structure 
and evolution. This program aims at determining this structure at 
small angular scales, which is very important for small condensations such 
as globules or the (shocked) interface of stellar winds and the ISM, 
such as parts of the Gum Nebulae or 30 Dor. The program will 
use imaging polarimetry in the optical and IR (for denser 
regions) in combination with the antecipated unique imaging capabilities 
of SOAR. 
 
Required minimum field of view (arcmin): 6'. 
 
Required psf (FWHM, profile details): <0.5" optical, 
<0.4" IR  
 
Signal/noise required per resolution element: > 1000 
 
Typical exposure time for this S/N & lunar phase: typically 
several minutes per waveplate position; 1/2h - 1 h total. 
 
What additional photometric calibrations are required? 
Observations of polarized and unpolarized standards ( the latter
not necessarily on the same night). 
 
If IR, is tip/tilt feasible (consider isoplanatic patch)? 
Tip-tilt required. 
  
Can this program execute in a queue? Probably yes.
 
Anticipated post-focus instrumentation requirements (filters, gratings, 
etc.): polarimetric capabilities in the optical and IR (ie., 
polarizing optics in optical path); straight-through port. 
 
Required instruments (spectral R, filters, wavelength range): 
optical imager, IR imager 
 
Why can't this program execute on the Blanco 4m? High angular resolution 
imaging capabilities required. 
  
 
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Brief program summary and its significance: 
 
GEOMETRY AND PHYSICS OF YOUNG STELLAR 
OBJECTS 
(A.M. Magalhaes)
 
The environments of YSO are regions where dust scattering 
dominates. This is evidenced by high values of linear 
polarization (several tens of percent) observed toward these objects. 
Circular polarization from multiple scattering 
has just begun to be used as a complementary tool. It is clear 
that optical but specially IR polarization must be considered 
if any meaningful interpretation of such environment is to be 
made. In addition, the highest possible angular resolution, 
revealing details closer to the star, are crucial if use of scattering 
models is to be appropriately made. High angular resolution 
imaging polarimetry capability will further make SOAR unique in  
in the hemisphere and possibly in the world. 
 
Required minimum field of view (arcmin): 2' 
 
Required psf (FWHM, profile details): <0.5" in the optical; 
<0.2" in the IR. 
 
Signal/noise required per resolution element: >100 for linear 
polarimetry; > 2000 for circular polarimetry 
 
Typical exposure time for this S/N & lunar phase: typically 
from a few minutes to several min or so per waveplate position; 
from 15min to 1 h total 
 
What additional photometric calibrations are required? 
Observations of polarized and unpolarized standards (the latter
not necessarily on the same night). 
 
If IR, is tip/tilt feasible (consider isoplanatic patch)? 
Tip-tilt required.

Can this program execute in a queue?
Probably yes.
 
Anticipated post-focus instrumentation requirements (filters, gratings, 
etc.): polarimetric capabilities in the optical and IR (ie., 
polarizing optics in optical path); straight-through port.
 
Required instruments (spectral R, filters, wavelength range): 
optical imager, IR imager 
 
Why can't this program execute on the Blanco 4m? 
 High angular resolution imaging capabilities required. 
 
 
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Brief program summary and its significance: 
 
STRUCTURE OF ACTIVE GALACTIC NUCLEI 
(A.M. Magalhaes)

Study of the geometry and physics of the central regions of
Active Galactic Nuclei (AGN) is important if we want to understand
their central engines. Spectropolarimetry, coupled with the antecipated
imaging capability of SOAR, will be an important tool in
that regard. Some Type 2 AGN (with narrow permitted
and forbidden lines) have obscured broad line regions visible only
in reflected, and hence polarized, light. Thus the polarized flux
(= %polarization * flux) of such objects look like the total flux
of a Type 1 AGN (with broad permitted and narrow forbiden lines).
In the cases of the recently discovered AGN with double-peaked
emission lines, spectropolarimetric observations should test the
merits of the accretion disk and other interpretations. A third
case is that of the Broad Absorption Line QSOs, where spectropolarimetry
and its ability to study aspects of the geometry of polarized
objects even without spatially resolving them will be very important.
 
Required minimum field of view (arcmin): 1' 
 
Required psf (FWHM, profile details): <0.4" optical, <0.2" IR.
 
Typical target separation if multiple targets per exposure: 
 
Signal/noise required per resolution element: >2000 
 
Typical exposure time for this S/N & lunar phase: typically 
2-4 h total per object 
 
What additional photometric calibrations are required? 
Observation of a polarized standard star or through calibration optics.
 
If IR, is tip/tilt feasible (consider isoplanatic patch)? 
Tip-tilt required.

Can this program execute in a queue? Yes 
 
Anticipated post-focus instrumentation requirements (filters, gratings, 
etc.): polarimetric capabilities in the optical and IR (ie., 
polarizing optics in optical path); straight-through port. 
 
Required instruments (spectral R, filters, wavelength range): Optical 
and Near IR spectrographs; R~2000-5000; an IFU (integral field unit) 
and/or a Fabry-Perot for resolved targets. 
 
Why can't this program execute on the Blanco 4m? Image quality 
required 
  
 
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