Operational RSS-1024 Frequently Asked Questions
1. I want to set up a UVB-1, MFR, UVMFR, or SPUV site and only download data every few days on my YESDAS-2. Is unattended operation doable? What about the TSI and RSS?
Yes, absolutely. For radiometers such as the UVB-1, MFR-7, UVMFR-7 and SPUV-10, the YESDAS supports automated remote unattended operation. However, depending on the number of instruments, you will likely want to order the PCMCIA-2 memory card option.
For our TSI and RSS instruments, you can expect to collect anywhere from 1 to 32mb of data per day, depending on data rates. Thus a local PC or a 24-hour, 7 day a week Internet connection is good to have. In cases where it is infeasible to have a network connection, the TSI-880's optional DSM-420 data storage module supports 420Mb of removable storage.
2. For many months the shadowband shaded the diffuser correctly, but getting closer to the summer solstice, we notice it does not appear to have enough length to shadow the diffuser completely. Each day the gap of shadow becomes slightly larger.
This is happening near summer solstice … it is not adjusted correctly. This will crete significant, non-correctable measurement errors to direct-and-diffuse around solar noon. Here are some things to try to get it aligned:
1. Using a protractor, cut a small (roughly 3") triangle of thin cardboard with the angle of your site latitude. Now slip the triangle under the motor case between the stand and the motor housing, to verify your motor's shaft angle is equal to your site latitude. Has to be within about a degree, once set you can forget it. I realize you said you did this, but verify it.
2. Check that your motor assembly is pressed all the way back against the machined slide (a both points top and bottom), If there is a small gap loosen the screw and press the motor hard against the slide and re-tighten the clamp.
3. Use a bubble level to verify the diffuser is level in both planes. Do not let the bubble level come in contact with the white diffuser, which is soft. Do not worry about the level of the base itself you want to check the level right at the black diffuse ring.
4. Assuming the above three items are set correctly, the band may have been bent slightly out of round. Gently bend it down (not too much). Do this around solar noon.
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3. Owners of UV-B networks would like to know what instrumentation is required for making routine calibrations of the Model UVB-1.
rather complicated area of radiation physics. First of all, you don't calibrate broadband UVB-1 instruments using irradiance standard or arc lamps. The spectral output of FEL lamps is wildy different than the solar spectrum. What you do is calibrate a spectroradiometer using a FEL lamp, then you co-locate the spectroradiometer with a pool of about five closely matched broadband instruments and using the sun, transfer the calibration (a UVRSS or U-1000 will work for this, in the past we've also used Richard McKenzie's own spectroradiometer as a check). Please direct them to chapter 4 of the attached UVB-1 manual which outlines the procedure. You should read this before meeting with them.
This will be far more expensive path if they do not own a UVRSS-1024. In some real sense this is a very good reason to buy a UVRSS, it permit you to derive calibration constants directly, (usign the same transfer source, the sun). We sell the PFC-5001 lamp calibrator as an accessory to the UVRSS (does not work standalone).
Most users pay us the cost calibrate them at the factory. NIST/PTB/NPL are highly competent labs, but it will be expensive. In the US the specific NIST lab to talk to is the CUCF - have them look at:
CUCF calibrates all of the USDA's broadband UVB-1s for Colorado State (who runs the US Dept of Agriculture's UV-B monitoring program.)
The UVRSS can produce ozone data, (see page 3-23 of the manual for information.) We have compared the UVRSS favorably with Dobson measurements taken near Boulder, Colorado.
4. What is the ambient temperature operating range of the radiometers (UVB-1, MFR/UVMFR and SPUV? Will they work in the arctic?
YES has successfully deployed MFR and SPUV systems running from the tropics to Point Barrow, Alaska. However, above 75° north or south latitude you won't be able to make direct-normal or diffuse measurements (a SPUV works just fine above this range but requires a tracker). The SPUV working temperature range is -50° to +50° ; the MFRs working temperature range is -35° C to +40° C. But extreme wind loads can decrease the range slightly. If you can protect the instrument from wind and add additional infrared heaters for cold operations it can work at much lower temperature ranges, as the MFR Point Barrow installation indicates.
Each MFR is characterized yearly in our optical calibration facility, in five ways:
1. A North/South angular scan (via a cosine bench),
2. An East/West angular scan ( " ),
3. Relative spectral filter function response (via a monochromator),
Channel dark levels, and
4. Absolute voltage response (via a NIST traceable irradiance standard lamp).
The actual MFR head characterization takes four steps:
1 & 2. North/south and east/west angular measurements of an MFR head are done at 1 degree increments from -90 to +90 degrees off axis. The measurements are taken at a special cosine test facility, using a 500 watt lamp mounted 5 meters form the turntable. This generates your solarinfo (.sol file) that permits angular correction, In this step we characterize the angular effects of the diffuser that are so critical to doing the direct-normal calculation and for Optical Depth accuracy.
3. Next, a spectral scan of the head is done. The head is put in front of a 150 watt lamp fed monochromator which sweeps over the bandwidth of each filter passband at 1 nm increments. This is a "relative spectral response test"
4. Finally, we put the MFR head in front of a 1000 watt quartz halogen tungsten filament lamps lamp (50 cm distant) and get the absolute voltage sensitivity of the channel. Using the bandpass determined in Step 3, along with the lamp's table of irradiance outputs, we calculate the actual engineering constants to get you from volts out to w/m^2/nm.
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