USB4000 Optical Bench Options
Hover over the numbers on the image for more info.
SMA 905 Connector
Light from a fiber enters the optical bench.
Fixed Entrance Slit
Use our Range and Resolution Calculator to find out how your slit choice affects optical resolution.
Longpass Absorbing Filter
A filter has a transmission band and a blocking band to restrict radiation to a certain wavelength region for eliminating second- and third-order effects.
Light reflects from this mirror, as a collimated beam, toward the grating.
Grating & Wavelength Range
Gratings are fixed place at the time of spectrometer assembly. Dispersion will depend on your choice of starting wavelength.
This mirror focuses first-order spectra on the detector plane.
L4 Detector Collection Lens
This cylindrical lens focuses the light from the tall slit onto the shorter detector elements.
We offer a 3648-element linear CCD array Toshiba detector.
OFLV Variable Longpass Order-sorting Filter
Precisely blocks second- and third-order light from reaching specific detector elements.
UV4 Detector Window Upgrade
Standard window is replaced with a quartz window for applications <340 nm.
Light from a fiber enters the optical bench through the SMA 905 Connector. The SMA 905 bulkhead provides a precise location for the end of the optical fiber, fixed slit, absorbing filter and fiber clad mode aperture.
Light passes through the installed slit, which acts as the entrance aperture. Slits come in various widths from 5 µm to 200 µm. The slit is fixed in the SMA 905 bulkhead to sit against the end of a fiber. Smaller slit sizes achieve the best optical resolution.
|SLIT-5||5-µm wide x 1-mm high||~5.3 pixels|
|SLIT-10||10-µm wide x 1-mm high||~5.7 pixels|
|SLIT-25||25-µm wide x 1-mm high||~7.5 pixels|
|SLIT-50||50-µm wide x 1-mm high||~11.6 pixels|
|SLIT-100||100-µm wide x 1-mm high||~21 pixels|
|SLIT-200||200-µm wide x 1-mm high||~42 pixels|
When selected, an absorbing filter is installed between the slit and the clad mode aperture in the SMA 905 bulkhead. The filter is used to limit bandwidth of light entering spectrometer or to balance color. Filters are installed permanently.
|OF1-WG305||Longpass filter; transmits light >305 nm|
|OF1-GG375||Longpass filter; transmits light >375 nm|
|OF1-GG395||Longpass filter; transmits light >395 nm|
|OF1-GG475||Longpass filter; transmits light >475 nm|
|OF1-OG515||Longpass filter; transmits light >515 nm|
|OF1-OG550||Longpass filter; transmits light >550 nm|
|OF1-OG590||Longpass filter: transmits light >590 nm|
The collimating mirror is matched to the 0.22 numerical aperture of our optical fiber. Light reflects from this mirror, as a collimated beam, toward the grating. You can opt to install a standard mirror or a UV absorbing SAG+ mirror.
SAG+ mirrors are often specified for fluorescence. These mirrors also absorb nearly all UV light, which reduces the effects of excitation scattering in fluorescence measurements. Unlike typical silver-coated mirrors, the SAG+ mirrors won’t oxidize. They have excellent reflectivity — more than 95% across the Vis -NIR.
We install the grating on a platform that we then rotate to select the starting wavelength you have specified. Then we permanently fix the grating in place to eliminate mechanical shifts or drift.
Predicted Ranges & Resolutions
See a series of graphs to demonstrate the predicted Range and Resolution of your USB4000 Spectrometer.
This mirror focuses first-order spectra on the detector plane. Both the collimating and focusing mirrors are made in-house to guarantee the highest reflectance and the lowest stray light possible. You can opt to install a standard or SAG+ mirror.
This cylindrical lens, made in-house to ensure aberration-free performance, is fixed to the detector to focus the light from the tall slit onto the shorter detector elements. It increases light-collection efficiency and reduces stray light. It also is useful in a configuration with a large-diameter fiber for low light-level applications.
We offer a 3648-element (Toshiba TCD1304AP) linear CCD array detector with an effective range of 200-1100 nm. Each pixel responds to the wavelength of light that strikes it. Electronics bring the complete spectrum to the software.
Our proprietary filters precisely block second- and third-order light from reaching specific detector elements.
When selected, the detector’s standard BK7 window is replaced with a quartz window to enhance the performance of the spectrometer for applications <340 nm.
|DET4-200-850||Toshiba TCD1304AP detector, installed, with 200-850 nm variable longpass filter and UV4 quartz window; best for UV-VIS systems configured with grating #1 or #2||USB4000|
|DET4-200-1100||Toshiba TCD1304AP detector; installed, with 200-850 nm variable longpass filter and UV4 quartz window; best for systems configured with XR-1 grating||USB4000|
|DET4-350-1000||Toshiba TCD1304AP detector; installed, with 350-1000 nm variable longpass filter; best for VIS systems configured with grating #2 or #3||USB4000|
|DET4-UV||Toshiba TCD1304AP detector, installed, with UV4 quartz window; best for systems <360nm||USB4000|
|DET4-VIS||Toshiba TCD1304AP detector, installed, with VIS BK7 window; best for systems configured for >400nm||USB4000|
|Detector:||Toshiba TCD1304AP Linear CCD array|
|Detector range:||200-1100 nm|
|Pixel size:||8 μm x 200 μm|
|Pixel well depth:||100,000 electrons|
|Signal-to-noise ratio:||300:1 (at full signal)|
|Dark noise:||50 RMS counts|
|Sensitivity:||130 photons/count at 400 nm; 60 photons/count at 600 nm|