SOAR for Astronomers/Observers

This page is intended to provide scientists with an up to date quick glance on the instrumentation currently available on the SOAR telescope and modes of operation.

Instrument Type Wavelength
Field_of_View  (arcmin)       Scale
Resolution (R) Filters Data Reduction
SOAR Imager (SOI) U-sensitive optical imager 310-1000nm 5.2 x 5.2 0.077 N/A UBVRI, ugriz, ubvy, Ha, [SII],  others (see Filters) IRAF Mosaic Reduction, and also PyRAF script - basic image processing
SOAR Adaptive Optics Module (SAM) Laser-guided optical Adaptive Optics imager 400-1000nm 3.1 x 3.1 0.045 N/A BVRI, griz, ubvy, Ha, [SII],  others (see Filters) PyRAF script - basic image processing
Goodman High Throughput Spectrograph High throughput optical imaging spectrograph 310-850nm 7.2 circular 0.15 ~1400-10000 Imaging: UBVRI, ugriz, ubvy, Ha, [SII],  others (see Filters)
Spectra: GG-385, GG-455, GG-495, OG-570
IRAF. Tutorial for reducing single slit and MOS
SPARTAN Near-IR Camera Near-IR imager 1-2.2 um f/12: 5.04 x 5.04
f/21: 3.05 x 3.05
f/12: 0.066
f/21: 0.040
Ohio State IR Imager/Spectrograph (OSIRIS)
Near-IR imaging spectrograph 0.9-2.2 um f/7: 2.37 x 2.37
f/3: 5.65 x 5.65

f/7: 0.139
f/3: 0.331
1200-3000 Y (1.04um), JHK,Ks, He I (1.083um & 2.06um), Fe II (1.644um), 2.03um, BrGamma (2.17um), H2 (2.122um)  

SOAR offers both classical (on-site) observing, and remote observing (for experienced users). This provides with ample scheduling flexibility, making feasible complicated programs, especially those involving sporadic time sampling, that are otherwise normally not feasible in other facilities.

Once you have decided which instrument is best suited for your science program, the following links will help you in preparing your proposal, and later for your SOAR observing run:

  1. Preparing your proposal for requesting time with the SOAR telescope
  2. Preparing for your SOAR observing run: this section will tell you what you need to do for your upcoming run, depending on whether you will be coming to carry out your observations directly at the telescope, or observing remotely via Internet.
  3. Reducing your data.

Please, do not hesitate to contact us if you note errors, or you consider that important information is missing.