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We are about to start posting some very exciting results, so I thought we should provide some information about our filter system.  We are using Sloan Digital Sky Survey (SDSS) standard r’, i’, and z’ filters as our main bandpasses.  These filters were provided by Asahi Spectra.  Our CCD47 has a near-IR coating to maximize its long wavelength quantum efficiency (QE).   The below plot shows the combined QE of our system (taking into account only the CCD and filters), as well as the mean wavelengths of the filters.

Update 22 July 2011: added the transmission of our 950 Long Pass (950 LP) filter. This should be treated with a little caution, as it is from a catalog page, and not a measurement of our actual filter. Also note that these calculations were done assuming our CCD47 QE goes to 0 at 1.1 microns, since the manufacturer’s curve stops at 1.05.

On July 18 we succesfully mounted the NAS on the tower. Then recabled the system. Illuminated the the ASM at the top of the tower with the white light fiber source. Checked the optical alignment (which was unchanged from before). Then we moved the the PWFS on the 3axis stage (while tilting the dummy 50/50 beamsplitter) till the image of the ASM was round and centered on the PI stage (with its 12mm mirror it is the smallest optic). Then we took a 10 mode interaction matrix. Closed the loop! Then we took 50 and 200 mode IMATs with loop closed at 0.05 gain to clean up errors in the tower vibrations on the windy day we were working with (the tower was not floating since this was just an engineering test). Then closed the loop with the 200 modes to yield great images on the CCD47. A great day!Mounting the NAS

The lowest 50 KL modes from our interaction matrixClosed loop Pupils and ASM Mirror positionsThe Arizona team after the first closed loop (Jared, Laird, Derek)Alfio after closing the loop

This week we finished the optical alignment in the optical lab. We also mounted the NAS on the tower as a test. Then we pulled the NAS off the tower and mounted all the optics into the the NAS for the first time. Then we aligned the flowerpot (calibration point source) to the NAS and the board to the the flowerpot. See photos below

Laird bolting board on NASThe optical board on the NAS (flowerpot at top with calibration source)

A well aligned PWFS

The PWFS is now aligned on the bench. In the image you can see to the right a single frame of the CCD39 showing a flat wavefront with a slight tilt from our lamp source. On the left you an see the diffraction-limited image of the source on our VisAO camera in r’ band (resolution of 18 milliarcsec on the sky).An r’ band image of the lamp and its “flat” wavefront on the PWFS

Here is the current view of the, almost complete, integration of the wavefront sensor, VisAO camera, and their electronics and control computers. Derek Kopon (right) is working on the alignment of the optics and Jared Males (left) is working on the software. 

Wavefront Sensor (below Jared), CCD electronics box (on top of bench), VisAO camera electronics box (below bench)alignment fiber (flower pot), with VisAO camera and wavefront sensor behind