Brief program summary and its significance:

I. Colour-magnitude diagrams of globular clusters in the
bulge and in the Magellanic Clouds, in the infrared
and optical (Beatriz Barbuy)

Studies of metal-rich stellar populations in the
Galactic bulge are important for the understanding
of the bulge itself, and it is useful for population 
synthesis work. We have been working on VI images of
the bulge globular clusters, and started to obtain JK images.
The Magellanic Clouds clusters amount to about 2000 for both Clouds
so that many of them will not have been studied until the
operation of soar. The MC globular clusters are tracers
of the Clouds' chemical evolution.

Required minimum field of view (arcmin): minimum is 2'x2'

Required psf (FWHM, profile details): 0.5" 


Typical target separation if multiple targets per exposure:
very crowded fields

Signal/noise required per resolution element: 

Typical exposure time for this S/N & lunar phase: 600 s

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):
optical imager, IR imager

How soon might you need to revisit this target with another instrument?

Why can't this program execute on the Blanco 4m? High angular resolution,
and imaging capabilities required.

References (for non-mainstream applications):

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Brief program summary and its significance:

II. INFRARED SPECTROSCOPY OF BULGE STARS (Beatriz Barbuy)

Most stars and clusters in the Galactic bulge are highly reddened.
In the infrared the reddening is attenuated, which makes
possible to carry out spectroscopy of stars not observable
in the optical. For example, for the cluster NGC 6553, 
 E(B-V) = 0.7, E(J-K) = 0.36, Av = 2.2 and Ak = 0.25.
In V the brightest bulge stars have V = 15, whereas in the
infrared they are K = 8 or so. 
Besides, the infrared J, H and K regions offer the opportunity
to observe lines not present in the optical region, such as
clear Sulphur lines, and also several Magnesium lines
(in the optical almost all Mg lines are too strong).
The derivation of abundances of stars in the bulge is
important to understand the formation of the bulge, and also
to infer conclusions about bulges of external galaxies.

Required minimum field of view (arcmin): 1'

Required psf (FWHM, profile details): 

Typical target separation if multiple targets per exposure:
crowded regions

Signal/noise required per resolution element: > 100

Typical exposure time for this S/N & lunar phase:  1/2h - 1 h

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): IR spectrograph
(high res.)

How soon might you need to revisit this target with another instrument?

Why can't this program execute on the Blanco 4m? no IR spectrograph

References (for non-mainstream applications):

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Brief program summary and its significance:

III. STELLAR POPULATIONS IN THE GALAXY, MAGELLANIC CLOUDS,
     NEARBY GALAXIES  (Beatriz Barbuy)

We have developed a method for identifying stellar parameters
(effective temperature Teff, gravity log g, metallicity [Fe/H]
and [Mg/Fe]) of individual stars from low or medium resolution
spectra (the highest the resolution the best, but low resolution
is also possible, with less precision).
The method consists of dividing the observed spectrum
by the spectrum of an observed reference star of known parameters
and/or synthetic spectra, and comparing this to differences found
for the same parameters in a grid of synthetic spectra, using
a perturbation method.
This allows the study of deep stellar populations in our galaxy
(separation between halo, thick disk and disk stars with height z)
as well as in the Magellanic Clouds and nearby galaxies.

A multi-object moderate resolution optical spectrograph would be 
of interest for this program.

Required minimum field of view (arcmin): 10'x10' if multi-object

Required psf (FWHM, profile details): 

Typical target separation if multiple targets per exposure: 30"

Signal/noise required per resolution element: 30 - 50

Typical exposure time for this S/N & lunar phase: 30 min.

Anticipated photometric dynamic range required:

What additional photometric calibrations are required?
two-colour imaging (VI, BV or JK)

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):
multi-object optical spectrograph  (might also be in infrared regions)

How soon might you need to revisit this target with another instrument?

Why can't this program execute on the Blanco 4m? if mult-object spectrograph
is available, yes

References (for non-mainstream applications):

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Brief program summary and its significance:

IV. HIGH RESOLUTION ECHELLE SPECTROSCOPY  (Beatriz Barbuy)

Detailed abundance analysis of bulge stars, 
Magellanic Clouds stars, halo stars, 
and other interesting stars in the Galaxy:
Li-rich stars, T Tauri stars, OH-IR stars,
yellow supergiants, etc. etc.
Results are important for the chemical evolution of
the Galaxy and MCs, besides for testing stellar evolutionary
theories of mixing etc.

Required minimum field of view (arcmin): 

Required psf (FWHM, profile details): 

Typical target separation if multiple targets per exposure:

Signal/noise required per resolution element: 100

Typical exposure time for this S/N & lunar phase:  1/2h - 1 h

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):
High-resolution echelle spectrograph  - Phoenix is ideal in IR

How soon might you need to revisit this target with another instrument?

Why can't this program execute on the Blanco 4m? Feasible in the optical
with Blanco echelle spectrograph. 

References (for non-mainstream applications):

===================================================

Brief program summary and its significance:

V. SPECTRAL EVOLUTION, STELLAR POPULATIONS OF ELLIPTICAL GALAXIES
 (Beatriz Barbuy)

We have been working in a database of atomic and molecular lines
to reproduce the spectra of cool stars (F-M types) from UV to IR.
This database is presently being implemented in a galaxy evolution
code, and will enable us to study in greater detail than previously
in the literature, the behaviour of spectral lines in absorption lines
of elliptical/lenticular galaxies.
For this we need to have rather well-defined lines, and for a 4m
telescope a redshift of about 0.3 should be a limit.
We intend to study the stellar populations and chemical composition
of these composite systems. Later on, with larger telescopes,
the spectral evolution should be studied.



Required minimum field of view (arcmin): 10'x10' if multi-object to
do galaxies in groups

Required psf (FWHM, profile details): 

Typical target separation if multiple targets per exposure:

Signal/noise required per resolution element: 30 - 50

Typical exposure time for this S/N & lunar phase:  1/2h - 1 h 

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):
multi-object optical or IR spectrograph.  A multi-object like 
MOS (CFHT) or the project of NIR-MOS (Gemini). Resolutions of about
R 5000 are ok.

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):

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