(This is a partial "reprint" of a poster paper presented at the January 1996 meeting of the American Astronomical Society.)
ChAOS sodium laser beacon. In December 1995, our sodium laser was launched from the Apache Point telescope through a 12 inch lens mounted on the corner of the
secondary mirror support structure. This lens is visible in the lower right-hand
corner of the photo. Three flat mirrors and a field lens guide the beam from the laser to the lens. Boresighting and aligning the laser with the 3.5m telescope are done by tilting these three mirrors. Note that the sodium spot is not visible in this photo; the bright spot at the end of the beam is caused by reflection off of a thin layer of clouds.
Diode-laser mounted on the telescope. This photo shows the laser mounted
on the Nasmyth port of the 3.5m telescope. A thermally insulated "house" was constructed to prevent heat leakage into the dome. Additionally, the entire optical
bench of the laser was placed into a thermally controlled box to prevent temperature
fluctuations. This photo was taken right after the laser was first lowered onto the Nasmyth port (by removing the roof of the house).
Diode-pumped sum frequency laser. Left: Two mode locked Nd:YAG lasers, one tuned to 1.064µm and the other to 1.319µm, are mixed in non-linear crystals to generate light at the sodium D2 line (0.589µm). The laser outputs 7-9 Watts of high-quality sodium light with a FWHM line width of about 1GHz. Right: In this photo,
the 1.064µm laser is on the left (seen as green because of frequency doubling), the 1.319µm
laser is in the middle (fairly invisible), and the summed-frequency sodium laser is visible on
the right side of the bench.
Laser Pulses. Left: Transform-limited spectral profile of the 0.589µm sodium laser. Free spectral range of the spectrum analyzer is 8 GHz. FWHM of the spectrum is about 1 GHz. The laser line width can be changed from about 1 to 3 GHz using mode lock "chirping". Center: The laser operates at a pulse rate of 400 Hz. This plot shows the laser's micropulse temporal profile. Right: This plot shows the laser's macropulse temporal profile (which lasts about 150µs).
Laser Profiles Theoretical instantaneous laser beam profile at the sodium layer
for an optimized 0.5 meter launch telescope. The three curves correspond to seeing
of 1, 2/3, and 1/2 arcsecons.
Lincoln Labs laser group. Pictured here are some of the people at Lincoln Labs who created our sum frequency laser.
Radiative saturation becomes significant (i.e. effective cross-section reduced by a factor of two) at:
| Usable line width | delta nu ~ 3 GHz |
| Sodium natural line width | delta nu ~ 10 MHz |
| Saturation effects at | I ~ 2W/cm^2 |
| Spot size expected at good site | 20 cm FWHM |
| Laser peak power | P < 1000W |
| Laser mean power | P ~ 1000W x duty cycle |
| Laser power required for high order AO | P ~ 10W |
MMT Experiment. Left: In 1993, in a joint experiment with the University of Arizona
adaptive optics group, we took our CW laser to the MMT. The laser was projected out of a 75cm guide telescope in the center of the MMT. The U of A group was able to
"close" their adaptive optics system with this beacon. Right: This is a contour plot of the sodium beacon produced in the MMT experiment. The beacon was imaged through a single mirror of the MMT.
In this 2.6 sec exposure with a 1.2 Watt CW laser, the artificial star is equivalent to
a star of V magnitude 12.5 and has a FWHM of 1.0 arcsec x 1.3 arcsec. The slight
elongation is due to the 2.5m offset between the beam projector and the receiving
telescope.
Yerkes Experiments. Left: In 1991, we projected our dye laser through a five inch
telescope at Yerkes Observatory and viewed the sodium beacon with the famous 40 inch refractor. Right: In this false-color and highly foreshortened view of the return, the streak at lower right is produced by low-altitude Rayleigh backscatter and becomes most intense (red spot) at 23km where the beam encounters volcanic dust from an eruption of Mt. Pinatubo. Farther up, the backscatter fades as the air thins. At upper left is the 12th magnitude artificial sodium star at an altitude of 90km.
Our CW dye laser. Nestor Farmiga adjusts our continuous wave dye laser in the basement of Yerkes Observatory.