Flame Optical Bench Options
Hover over the numbers on the image for more info.
Fiber Optic (SMA 905) Connector
Light from a fiber enters the optical bench.
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 in place at the time of spectrometer assembly.
This mirror focuses first-order spectra on the detector plane.
Detector Collection Lens
This cylindrical lens focuses the light from the tall slit onto the shorter detector elements.
We offer a 2048-element FLAME-S (Sony ILX511B) or a 3648 element FLAME-T (Toshiba TCD1304AP) linear CCD array.
OFLV Variable Longpass Order-sorting Filter
Precisely blocks second- and third-order light from reaching specific detector elements.
UV Detector Window Upgrade
Standard window is replaced with a quartz window for applications <360 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, 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 while larger slits have higher light throughput. Slit size is labeled as shown.
|INTSMA-5||5-µm wide x 1-mm high||~3.0 pixels|
|INTSMA-10||10-µm wide x 1-mm high||~3.2 pixels|
|INTSMA-25||25-µm wide x 1-mm high||~4.2 pixels|
|INTSMA-50||50-µm wide x 1-mm high||~6.5 pixels|
|INTSMA-100||100-µm wide x 1-mm high||~12 pixels|
|INTSMA-200||200-µm wide x 1-mm high||~24 pixels|
|INTSMA-000||Interchangeable bulkhead with no slit||NA|
|INTSMA-KIT||Interchangeable SMA Kit connectors; 5µm; 10µm; 25µm; 50µm; 100µm and 200µm||NA|
Ocean Optics also offers a range of FC connector slits in the same wavelengths, with the product code INTFC-XXX. An INTFC-KIT is also available. Note that these items are made to order and have a longer lead time. Contact an Ocean Optics Application Sales Engineer for more details.
If selected, an absorbing filter is installed between the slit and the aperture in the SMA 905 bulkhead. The filter is used to limit bandwidth of light entering the spectrometer or to balance color. Filters are installed permanently.
Each filter is designed for a specific slit. If you anticipate needing the filter with multiple slit sizes, then you must specify this at the time of order. Contact us for details.
The collimating mirror is matched to the 0.22 numerical aperture of our standard optical fibers. Light reflects from this mirror, as a collimated beam, toward the grating. You can opt to install a standard mirror or a NIR-enhancing but UV absorbing SAG+ mirror.
SAG+ mirrors are often specified for fluorescence. These mirrors 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.
Specify standard or SAG+ mirrors when ordering your spectrometer.
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.
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. As with the collimating mirror, the mirror type needs to be specified when ordering.
This cylindrical lens 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 and slit for low light-level applications such as fluorescence. Preconfigured Flame spectrometers with a collector lens are available – look for –ES at the end of the name.
There are two choices of detector available for the Flame. We offer a 2048-element FLAME-S (Sony ILX511B) or a 3648 element FLAME-T (Toshiba TCD1304AP) linear CCD array. These both have an effective range of 190-1100 nm. The optics split the light into its component wavelengths which fall across the different pixels. Each pixel responds to the wavelength of light that strikes it. The detector outputs an analog signal from each pixel that is converted via the ADC into a digital signal. The driver electronics process this signal and send the spectrum via the USB connection to the software. The best choice of detector will depend on the application.
|Specification||S Type (FLAME-S)||T Type (FLAME-T)|
|Detector:||Sony ILX511B linear silicon CCD array||Toshiba TCD1304AP linear silicon CCD array|
|Watch for:||N/A – Offers strong all-around performance||
Our proprietary filters precisely block second- and third-order light from reaching specific detector elements. Light reflected off the grating can propagate 2nd and 3rd order effects at whole multiples of the incident light. While these signals are weak, they may cause stray light that reduces the accuracy of the spectrometer response. Order sorting filters reject this stray light only allowing the desired wavelength through to the detector. Order sorting filters are combined with detector window upgrades. The full range available is listed below. These must be specified at the time of ordering.
The standard BK7 glass window on the detector begins to absorb light around 340nm. For applications in the UV, below 360nm, we recommend the detector window upgrade. This replaces the BK-7 glass with Quartz. Typically these are used in conjunction with an order sorting filter to block the impact of 2nd and 3rd order effects at higher wavelengths.
|DET2B-200-535||Sony ILX511B detector, installed, with Custom OFLV Coated Window Assembly for Grating#5 and Grating#5U, S-bench||FLAME-S|
|DET2B-200-850||Sony ILX511 detector, installed, with 200 – 850 nm variable longpass filter and UV2 quartz window;
Best for UV-VIS systems configured with Grating #1 or #2
|DET2B-200-1100||Sony ILX511 detector, installed, with 200 – 850 nm variable longpass filter and UV2 quartz window;
Best for UV-VIS systems configured with XR-1 grating
|DET2B-350-1000||Sony ILX511 detector, installed, with 350 – 1000 nm variable longpass filter;
Best for VIS systems configured with Grating #2 or #3
|DET2B-UV||Sony ILX511 detector, installed, with UV2 quartz window;
Best for systems configured for <360nm
|DET2B-VIS||Sony ILX511 detector, installed, with VIS BK7 window;
Best for systems configured for >400nm
|DET4-200-535||Toshiba TCD1304AP detector, installed, with Custom OFLV Coated Window Assembly for Grating#5 and Grating#5U, S-bench||FLAME-T|
|DET4-200-850||Toshiba TCD1304AP detector, installed, with 200 – 850 nm variable longpass filter and UV2 quartz window;
Best for systems configured with Grating #1 or #2
|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
|DET4-350-1000||Toshiba TCD1304AP detector, installed, with 350 – 1000 nm variable longpass filter;
Best for VIS systems configured with Grating #2 or #3
|DET4-UV||Toshiba TCD1304AP detector, installed, with UV4 quartz window;
Best for systems configured for <360 nm
|DET4-VIS||Toshiba TCD1304AP detector, installed, with VIS BK7 quartz window;
Best for systems configured for >400 nm