------------------------------------------------------------- "INFRARED SPECTROSCOPIC STUDY OF YSOs IN DISTANT STAR FORMATION REGIONS" (J. Gregorio-Hetem) Brief program summary and its significance: We have detected with ROSAT, hundreds of X-rays sources that are possible intermediate and low mass young stellar objects (Herbig Ae/Be and T Tauri stars) associated to star formation regions in giant molecular clouds (Monoceros-Canis Majoris Complex). By doing spectroscopy in the 1-4 mum it is possible to observe the H2 and H3+ infrared lines, in order to study the interaction of X-rays (~1Kev) with molecular gas. The physical conditions of these distant molecular clouds, for which the low mass star formation is not well known, could be studied by comparing the intensities of the IR lines with the X-ray heating. Required minimum field of view (arcmin): 1' point sources, 5' clusters Required psf (FWHM, profile details): 0.2" Typical target separation if multiple targets per exposure: 30" for clusters Signal/noise required per resolution element: ~30 Typical exposure time for this S/N & lunar phase: 1 h; grey nights 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: tens of different fields to be observed in three clouds. Can this program execute in a queue? may be Anticipated post-focus instrumentation requirements (filters, gratings, etc.): --- Required instruments (spectral R, filters, wavelength range): high resolution IR spectrographs (R>20000) Why can't this program execute on the Blanco 4m? the faintest objects will require the better imaging and flat fielding of SOAR References (for non-mainstream applications): Draine & Woods 1993, ApJ 363, 464 ------------------------------------------------------------------------------ " HIGH RESOLUTION ANALYSIS OF T TAURI STARS" (J. Gregorio-Hetem) Brief program summary and its significance: High resolution spectroscopy in the 300-1000 nm range will be applied to Spectral Synthesis Models in order to determine temperature, gravity and metallicity of a sample of T Tauri stars, for different elements: C2 molecular lines and Li atomic lines are synthesized to derive C and Li abundances. MaH bands can give gravity accurate values. The iron lines are tracers of the chromospheric activity. Required minimum field of view (arcmin): <1' Required psf (FWHM, profile details): 0.2" Typical target separation if multiple targets per exposure: --- Signal/noise required per resolution element: >100 Typical exposure time for this S/N & lunar phase: hours, any lunar phase 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: want to survey stars in different spectral ranges. Can this program execute in a queue? may be Anticipated post-focus instrumentation requirements (filters, gratings, etc.): --- Required instruments (spectral R, filters, wavelength range): high resolution optical spectrograph (R>50,000) How soon might you need to revisit this target with another instrument? --- Why can't this program execute on the Blanco 4m? the brighter stars could be done with Blanco. References (for non-mainstream applications): Castilho et al. 1995 A&A 297, 503 ------------------------------------------------------------------------------ " DEEP INFRARED IMAGING OF YOUNG STELLAR CLUSTERS ASSOCIATED TO GIANT MOLECULAR CLOUDS" (J. Gregorio-Hetem) Brief program summary and its significance: The intermediate and low mass young population, still embedded in molecular clouds, are better detected in near-infrared wavelengths, not affected by the visual extinction. Deep imaging observations in these spectral range are useful to identify embedded populations and to study the circumstellar emission. We have detected in distant molecular clouds (~1Kpc) X-ray emission typical from young stellar objects of intermediate and low mass, but there is a lack of information about the possible near-IR population, possible associated to these clouds. Only a small part of one of them has been observed in the 0.9-2.2 mum: a 15' x 15' arcmin of the central core of Mon R2. This photometric study revealed a cluster of hundreds of IR sources. We intend to obtain images of the X-rays sources detected by ROSAT in the Mon-Can Complex in order to complete our understanding of the young population associated to distant star formation regions. Coronographics images would be useful to detect circumstellar structures like disk or envelopes. Required minimum field of view (arcmin): 5-10' Required psf (FWHM, profile details): 0.2" Typical target separation if multiple targets per exposure: --- Signal/noise required per resolution element: >100 Typical exposure time for this S/N & lunar phase: long Anticipated photometric dynamic range required: >10^4 What additional photometric calibrations are required? excellent flat fielding (better than 1%) If IR, is tip/tilt feasible (consider isoplanatic patch)? yes Anticipated number of separate pointings to complete program: tens of different fields to be observed in three clouds. Can this program execute in a queue? may be Anticipated post-focus instrumentation requirements (filters, gratings, etc.): --- Required instruments (spectral R, filters, wavelength range): coronograph, IR imager with small pixel scales How soon might you need to revisit this target with another instrument? --- Why can't this program execute on the Blanco 4m? inadequate imaging performance References (for non-mainstream applications): Hodapp 1994, ApJS 94, 615 -----------------------------------------------------------------------------