LISA SPECTROGRAPH SAMPLES
First light of a commercial
version (Shelyak instruments)
February 25, 2011
The setup (Castanet-Tolosan observatory).
The telescope is a Celestron 11 (D = 0.28 m) with a f/6.3 Alan Gee focal reducer (Baader).
The main CCD camera is a QSI583 model. The guiding camera is a video Watec 120N+.
Beta Leo : A standard A3V star
Fusion of visible and infrared spectra (image acquisition: Audela, processing : ISIS).
Note the Pashen serie near 8500 A. The Pashen Alpha is at l10049 A (1.0049 micron).
Consistency of LISA data (at R
= 1000) compared to eShel observation (at R = 10000) for Beta Leo.
The continuum is normalized to unity. The LISA spectrum is shifted by 0.2 continuum unit for clarity.
Z CMa: a Herbig Ae/Be star (V
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Full spectral range (merging of
a visible spectrum and an infrared spectrum, exposure time 6 x 300 seconds for
Note the large spectral range domain, from ultraviolet to near infrared.
Halpha is at the middle of the plot. P-Cygni profile is easily to detect for many lines.
The emission triplet near 8500 A is from ionised calcium.
Detail of blue region.
Detail of infrared region
(absorption near 7600 A is from telluric CO2 molecule, large aborption near 9350 A is from telluric H2O molecule)
Comparison of a high resolution spectrum (eShel at R = 11000) and a medium resolution spectrum (LISA at R = 1000).
Of course, the spectral resolution is inferior for the LISA spectrum, but the signal to noise ratio is significantly superior for a shorter exposure time.
All the details into the LISA spectrum are real.