|Name||Telescope Class||Pixel scale "/pix||Field of view||Overhead per frame||Filter wheel options|
|Spectral||2-meter||0.300 (bin 2x2)||10'x10'||22s||18|
|Sinistro||1-meter||0.389 (bin 1x1)||26'x26'||42 s||21|
|SBIG 6303||0.4-meter||0.571 (bin 1x1)||29'x19'||14 s||9|
|Merope||2-meter||0.278 (bin 2x2)||5'x5'||29 s||18|
|SBIG||1-meter||0.464 (bin 2x2)||15.8'x15.8'||15 s||21|
For an indication of exposure times to use with the science imagers, use our exposure time calculator.
Data from the science imagers are automatically processed through the BANZAI pipeline.
FLOYDS is a cross-dispersed, low resolution spectrograph, installed at both 2-m telescopes. The wavelength coverage is extremely broad -- with 540-1000nm in first order and 320-570nm in second order, recorded in a single exposure. Resolution varies from R=400 to R=700, and is roughly 0.35 nm/pixel in 1st order and 0.17 nm/pixel in second order. Each FLOYDS has a set of four (30" long) slits with widths of 1.2", 1.6", 2.0", and 6.0". These project to 3.5, 4.4, 4.9, and 14.4 pixels respectively on the detector. Acquisition and guiding is done robotically via a separate camera which images the slit and produces a 6.4’x4.3’ field of view.
For more information, see
LCO's Network of Robotic Echelle Spectrographs (NRES) will be six identical high-resolution (R~53,000), precise (≤ 3 m/s), optical (380-860 nm) echelle spectrographs, each fiber-fed (2.58" per fiber width) simultaneously by two 1 meter telescopes and a ThAr calibration source. The expected long-term accuracy for NRES is better than 3 m/s in less than an hour for stars brighter than V = 12. Like all instruments at LCO, scheduling, observing, and data reduction will be autonomous, and all data will be publicly available after a proprietary period. The first NRES element was installed (in Chile) in March 2017. Commissioning is ongoing.
For more information, see the descriptions of:
The imagers on LCO's 1m and 2m telescopes use 75mm square filters in 18 or 21 capacity filterwheels. Standard loadout is a complete Johnson-Cousins/Bessell set (UBVRI) and a SDSS/PanSTARRS set (u’g’r’i’z’sYw). Two 1m telescopes, one in South Africa and one in Chile, are equipped with Hα and Hβ filters. The Spectral imagers on the 2-m telescopes also contain some narrowband filters: Hα , Hβ, OIII, D51, Astrodon-UV, and Skymapper v.
For full details, see