Updated on June 29, 2021, 11:58 am
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.
|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||310-905nm||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
|Goodman Spectroscopic Pipeline (Python)
IRAF. Tutorial for reducing single slit and MOS
|SPARTAN Near-IR Camera||Near-IR imager||1-2.4 um||f/12: 5.04 x 5.04
f/21: 3.05 x 3.05
|TripleSpec 4.1 Near-IR Spectrograph||Near-IR spectrograph||<>1-2.4 um||~30 arcsec slit;
~3 arcmin slit viewer
|0.27 arcsec/pixel||~3500||J for slit viewer||Custom IDL-based pipeline|
|Visitor Instrument (Special access):
HRCam. Instr. Scientist: A. Tokovinin
|Optical High-speed Imager||400-1000nm||16 x 16 arcsec||0.01575||N/A||BVRI||Custom IDL-based pipeline by A. Tokovinin|
|Visitor Instrument - (Special Acces):
Fabry-Perot unit on SAM. Instr. Scientist: Claudia Mendez-Oliveira
NOT CURRENTLY AVAILABLE
|Fabry-Perot Etalon||400-1000nm||3.1 x 3.1||0.045||4100, 11200||Filters for SAM-FP||Custom pipeline|
|SOAR Integral-Field Unit Spectrograph (SIFS)
||Integral-Field Unit Spectrograph||400-780nm (during SV)||15 x 7.8 arcsec (during SV)||0.3 arcsec/fiber
|--||Custom PyRAF/MSCRED pipeline|
|Ohio State IR Imager/Spectrograph (OSIRIS)
RETIRED - NO LONGER AVAILABLE
|Near-IR imaging spectrograph||0.9-2.2 um||f/7: 2.37 x 2.37
f/3: 5.65 x 5.65
|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:
- Preparing your proposal for requesting time with the SOAR telescope
- 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.
- Reducing your data.
Please, do not hesitate to contact us if you note errors, or you consider that important information is missing.