Optical Spectrum Analyzers

Quick Comparisona
Item #	OSA20xC	Redstone® OSA30x
Noise Floorb	Absolute Power Power Density
Resolution (pm)c	Click to Enlarge
Spectral Resolution	7.5 GHz (0.25 cm-1)	1.9 GHz (0.063 cm-1)
Spectral Accuracy	±2 ppm	±0.2 ppm
Wavelength Meter Accuracy	±1 ppm	±0.5 ppm
Power Level Accuracy	±1 dB	±0.4 dB
Optical Rejection Ratio	30 dB	40 dB
Polarization Dependence	±1 dB	±0.2 dB (OSA302) ±0.1 dB (OSA305)
Free-Space Input (Collimated Beams)	≤Ø6 mm	≤Ø10 mm
Input Fiber Compatibility	FC/PC Connectors as Standard
Dimensions	320.3 mm x 149.2 mm x 474.7 mm (12.61" x 5.88" x 18.69")	541.0 mm x 224.1 mm x 532.6 mm (21.30" x 8.82" x 20.97")
Weight	20 lbs (10 kg)	58.4 lbs (26.5 kg)
Feature Comparison
Alignment Laser
Optional Purging
GUI with Analysis Tools
Accessible Calibration Laser	-
External Trigger	-
Multi-Detector Configuration	-
Piezoelectric Beam Path Optimization	-

• See the Specs tab for details on all available models.
• Absolute Power mode is recommended for narrowband sources, while Power Density mode is recommended for broadband sources.
• This is the resolution in spectrometer mode, and details for this calculation can be found on the Design tab.

Features

• General-Purpose (OSA20xC) and High-Performance (Redstone^® OSA30x) Instruments Available
• Spectrometer Mode Resolution
  • OSA20xC: 7.5 GHz (0.25 cm^-1)
  • OSA30x: 1.9 GHz (0.063 cm^-1)
• Wavelength Meter Mode Resolution: 0.1 ppm (Only for <10 GHz Linewidth Sources)
• Spectrum Obtained Using Michelson Interferometer and Fourier Transform
• Free-Space (with Cage Compatibility) and FC/PC Fiber-Coupled Inputs
• Operated by Included Windows^® Laptop with Pre-Installed Software
• • Straightforward, Intuitive, and Responsive Interface
  • Real-Time Math Operations and Statistical Analysis

Thorlabs' Optical Spectrum Analyzers (OSAs) perform highly accurate spectral measurements. Compatible with fiber-coupled and free-space light sources, these benchtop instruments suit a wide variety of applications, such as analyzing the spectrum of a telecom signal, resolving the Fabry-Perot modes of a gain chip, and identifying gas absorption lines. We offer two instrument types: the general-purpose OSA20xC instruments, which have a high update rate and moderate resolution, and the high-performance Redstone^® OSA30x instruments, which have a high dynamic range and high resolution.

Our optical spectrum analyzers acquire the spectrum via Fourier transform, using a scanning Michelson interferometer. This approach enables a high-precision Wavelength Meter mode with seven significant figures and ±1 part-per-million (ppm) spectral precision, allows robust statistical analysis of the acquired spectra, and provides broadband spectral measurements with every scan. A frequency-stabilized 632.9918 nm HeNe alignment laser is included in each OSA20xC unit, which is used to ensure a spectral accuracy of ±2 ppm. Each Redstone OSA includes a frequency-locked 1532.8323 nm reference laser, resulting in a spectral accuracy down to ±0.2 ppm.

Thorlabs' OSA20xC spectrum analyzers are optimized to cover five different spectral ranges with a spectral resolution of 7.5 GHz (0.25 cm^-1) and a 30 dB optical rejection ratio. Designed for applications that require higher optical resolutions or sensitivities, the Redstone OSAs feature two detectors, which allow for measurements over a wide wavelength range with a 1.9 GHz (0.063 cm^-1) spectral resolution, as well as a noise floor with a 40 dB optical rejection ratio. For additional details on the interferometer design, please see the Design tab.

These instruments are designed to measure CW light sources. They also work in some applications where a pulsed light source is used; details may be found on the Pulsed Sources tab. Similarly, our OSA instruments are not designed for applications where it is necessary to recover small signals, including fluorescence detection and Raman spectroscopy. If your application would benefit from increased detection sensitivity, please refer to the Custom OSAs tab for some of our capabilities.

Optical Inputs
All of Thorlabs' OSAs accept FC/PC-terminated fiber patch cables and collimated free-space beams up to Ø6 mm (OSA20xC) or Ø10 mm (Redstone OSA30x). Details on compatibility are in the Specs and Free-Space Coupling tabs. For wavelengths from 2 µm to 5.5 µm, we offer fluoride single mode and fluoride multimode fiber patch cables. Optical Spectrum Analyzers with other fiber input receptacles are available by contacting Tech Support.

Software
Each Optical Spectrum Analyzer includes a Windows^® laptop with our OSA software suite pre-installed. This software includes built-in tools for simple and complex analysis, controls for adjusting sensitivity and resolution, a wavelength meter tool for narrowband sources, and a coherence length tool for broadband sources. Also available are apodization functions, which are used to account for the finite path length over which the interferogram is measured. This software also includes built-in support for the HITRAN reference database for spectroscopic analysis. For additional details on software capabilities, please see the Software tab.

• Limited by Bandwidth of Detectors and Optics
• Specified in high-temperature mode. In low-temperature mode, the wavelength range is 1.0 - 2.5 µm.
• Minimum detectable power per nanometer using Zero Fill = 0 and the highest resolution and sensitivity settings.
• See Graphs Below
• In the 350 - 500 nm range, the OSA201C will easily detect lasers and other narrowband sources, but broadband sources may not have sufficient power spectral density to be detected.
• Specified in low-temperature mode over 1.0 - 2.5 µm. In high-temperature mode, the level sensitivity is -65 dBm/nm over 1.0 - 2.6 µm.

• Each specification is valid for a single mode FC/PC-terminated patch cable, as well as for a collimated free-space beam with diameter <3 mm and divergence <3 mrad, assuming the included protective window is installed in the free-space aperture.
• Defined according to the Rayleigh criterion.
• After a 20 minute warm-up (Item #s OSA20xC), for a single mode FC/PC-terminated patch cable at an operating temperature of 20 - 30 °C.
• Specified in parts per million, which corresponds to nearly seven significant figures (depending on the specification). For instance, if the wavelength being measured is 1 µm, the wavelength meter precision will be 200 fm.
• Spectral Precision is the repeatability with which a spectral feature can be measured using the Peak Track tool.
• Measured in Wavelength meter mode (linewidth <10 GHz)
• Can be set from 0 - 9 decimals and has a feature that automatically estimates the relevant number of decimals.
• Using the same input single mode fiber for all measurements.
• Limited by the damage threshold of the internal components.
• Specified using Absolute Power Mode, Zero Fill = 2, and Hann apodization, after a 20 minute warm-up (Item #s OSA20xC), for an operating temperature of 20 - 30 °C. (The different apodization modes available in the OSA software are described in the OSA20xC and Redstone® OSA30x manual.) The specified wavelength range is 450 - 2500 nm for OSA302, 400 - 1000 nm for OSA201C, 600 - 1600 nm for OSA202C, 1.0 - 2.4 µm for OSA203C, 1.3 - 5.0 µm for OSA205C, 2.0 - 11.0 µm for OSA207C, and 1.0 - 5.5 µm for OSA305.
• Specified at ±25 GHz from Main Peak using High Resolution, Low Sensitivity, Hann Apodization, and an Average of 5 Traces
• Connectors for other fiber input receptacles are available upon request. Please contact Tech Support or see the Custom OSAs tab for details.
• The OSA and the Windows^® laptop each come with a region-specific power cord.

Click to Enlarge
The resolution shown here was calculated using the formula explained in the Design tab. Although the formula is valid for all OSA models, the usable wavelength range of each model is limited by the bandwidth of the detectors and optical coatings. Note that the resolution is valid only for the specified wavelength range of the instrument.

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Absolute Power mode is recommended for narrowband sources. The OSA203C noise floor was measured in low-temperature mode.

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Power Density mode is recommended for broadband sources. The OSA203C noise floor was measured in low-temperature mode.

Data Acquisition Specifications

The scan sensitivity and resolution are two independent settings controlled from the software. The sensitivity setting modifies the range of detector gain levels, while the resolution setting changes the optical path difference (OPD). For more details, see the Design tab.

Design

This tab describes the key concepts and implementation of the design used in Thorlabs' Fourier Transform Optical Spectrum Analyzers.

• Interferometer Design
• Resolution and Sensitivity
• Absolute Power and Power Density
• Interferogram Data Acquisition
• Interferogram Data Processing
• Wavelength Meter Mode
• Wavelength Calibration and Accuracy
• Optical Rejection Ratio

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Figure 2: Schematic of the optical path in Thorlabs' Redstone OSA30x. Note that the OSA302 does not include the dispersion compensation plate in the interferometer. 

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Figure 1: Schematic of the optical path in Thorlabs' OSA20xC OSAs, detailing the dual retroreflector design. 

Interferometer Design

Thorlabs' OSA20xC Fourier Transform Optical Spectrum Analyzers (FT-OSA) utilize two retroreflectors, as shown in Figure 1. These retroreflectors are mounted on a voice-coil-driven platform, which dynamically changes the optical path length of the two arms of the interferometer simultaneously and in opposite directions. The advantage of this layout is that it changes the optical path difference (OPD) of the interferometer by four times the mechanical movement of the platform. The longer the change in OPD, the finer the spectral detail the FT-OSA can resolve.

The Redstone^® OSA302 and OSA305 FT-OSAs use a standard arrangement of one fixed and one movable retroreflector as shown in Figure 2. The mobile retroreflector is mounted on Thorlabs' patented voice-coil-driven platform*, which changes the optical path length of the branch. The fixed retroreflector is mounted on a piezo actuator that translates the retroreflector in the two dimensions orthogonal to the beam path in a self-alignment algorithm. This configuration changes the OPD between the two branches by twice the mechanical movement of the platform.

*The Redstone OSA30x is constructed using Thorlabs' patented voice-coil-driven platform design. 

After collimating the unknown input, a beamsplitter divides the optical signal into two separate paths. The path length difference between the two paths is varied up to 40 mm for the OSA20xC and 160 mm for the Redstone OSA30x. The collimated light fields then optically interfere as they recombine at the beamsplitter.

The detector assemblies shown in Figures 1 and 2 record the interference pattern, commonly referred to as an interferogram. This interferogram is the autocorrelation waveform of the input optical spectrum. By applying a Fourier transform to the waveform, the optical spectrum is recovered. Note that the Redstone OSA models collect asymmetrical interferograms in terms of the location of the point of zero path difference (ZPD), and these interferograms are usually called single-sided; the OSA20xC instruments collect double-sided interferograms. The resulting spectrum offers both high resolution and very broad wavelength coverage with a spectral resolution that is related to the optical path difference. The wavelength range is limited by the bandwidth of the detectors and optical coatings. The accuracy of our systems is ensured by including a frequency-stabilized 632.9918 nm HeNe reference laser in the OSA20xC models and a frequency-locked 1532.8323 nm infrared reference laser in the Redstone OSA30x models. The reference laser is inserted into the interferometer and closely follows the same path traversed by the unknown input light field. This reference laser provides highly accurate, interferometric measurements of beam path length changes, allowing the systems to continuously self-calibrate and ensure accurate optical analysis well beyond what is possible with a grating based OSA.

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Figure 3: OSA Resolution vs. Wavelength of the Unknown Input
The resolution shown here was calculated using the formula to the left. Although the formula is valid for all OSA models, the usable wavelength range of each model is limited by the bandwidth of the detectors and optical coatings. Note that for the OSA20xC instruments, Δk = 1 cm^-1 for Low Resolution Mode and Δk = 0.25 cm^-1 for High Resolution Mode. For the Redstone OSA30x models, Low, Medium Low, Medium High, and High Resolutions correspond to Δk's of 4.0, 1.0, 0.25, and 0.063 cm^-1, respectively. Note that the resolution is valid only for the specified wavelength range of the instrument.

The OSA20xC and Redstone OSAs have spectral resolutions of 7.5 GHz (0.25 cm^-1) and 1.9 GHz (0.063 cm^-1), respectively. The resolution in units of wavelength is dependent on the wavelength of light being measured. For more details, see the Resolution and Sensitivity section below. In this context, the spectral resolution is defined according to the Rayleigh criterion and is the minimum separation required between two spectral features in order to resolve them as two separate lines. These spectral resolution numbers should not be confused with the resolution when operating in the Wavelength Meter mode, which is considerably better.

To reduce the presence of water absorption lines in the MIR region of the spectrum, our OSAs feature two 1/4" ID quick-connect hose connections on the back panel, through which the interferometer can be purged with dry air or nitrogen. Our Pure Air Circulator Unit, which uses hosing that can be directly inserted into these connectors, is ideal for this task.

Resolution and Sensitivity

The resolution of this type of instrument depends on the optical path difference (OPD) between the two paths in the interferometer. It is usually easier to understand the resolution in terms of wavenumbers (inverse centimeters), as opposed to wavelength (nanometers) or frequency (terahertz).

Assume we have two narrowband sources, such as lasers, with a 1 cm^-1 energy difference, 6500 cm^-1 and 6501 cm^-1. To distinguish between these signals in the interferogram, we would need to move away 1 cm from the point of zero path difference (ZPD). The OSA20xC can move ±4 cm in OPD and thus spectral features 0.25 cm^-1 apart can be resolved, while the Redstone OSA30x can move 16 cm in OPD and resolve spectral features that are 0.063 cm^-1 apart. The resolution of the instrument can be calculated as:

where Δλ is the resolution in pm, Δk is the resolution in cm^-1, and λ is the wavelength in µm. The resolution in pm as a function of wavelength, converted using this formula, is shown in Figure 3.

The resolution of the OSA20xC instruments can be set to High or Low in the main window of the software. In high resolution mode, the retroreflectors translate by the maximum of ±1 cm (±4 cm in OPD), while in low resolution mode, the retroreflectors translate by ±0.25 cm (±1 cm in OPD). The Redstone OSA30x instruments can be set to one of four resolution modes: High, Medium High, Medium Low, or Low. These settings correspond to OPDs of 16 cm, 4 cm, 1 cm, and 2.5 mm, respectively. The OSA software can cut the length of the interferogram that is used in the calculation of the spectrum in order to remove spectral contributions from high-frequency components.

The sensitivity of the instrument depends on the electronic gain used in the sensor electronics. Since an increased gain setting reduces the bandwidth of the detectors, the instrument will run slower when higher gain settings are used. The figures below show the dependency of the noise floor on the wavelength and OSA model.

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Figure 4: Noise Floor in Absolute Power Mode
Absolute Power mode is recommended for narrowband sources. The OSA203C noise floor was measured in low-temperature mode.

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Figure 5: Noise Floor in Power Density Mode
Power Density mode is recommended for broadband sources. The OSA203C noise floor was measured in low-temperature mode.

Absolute Power and Power Density

The vertical axis of the spectrum can be displayed as Absolute Power (Figure 4) or Power Density (Figure 5), both of which can be displayed in either a linear or logarithmic scale. In Absolute Power mode, the total power displayed is based on the actual instrument resolution for that specific wavelength; this setting is recommended to be used only with narrow spectrum input light. For broadband devices, it is recommended that the Power Density mode is used. Here the vertical axis is displayed in units of power per unit wavelength, where the unit wavelength is based upon a fixed wavelength band and is independent of the resolution setting of the instrument.

Interferogram Data Acquisition

For the OSA20xC models, the interference pattern of the reference laser is used to clock a 16-bit analog-to-digital converter (ADC) such that samples are taken at a fixed, equidistant optical path length interval. The HeNe reference fringe period is digitized and its frequency multiplied by a phase-locked loop (PLL), leading to an extremely fine sampling resolution. Multiple PLL filters enable frequency multiplication settings of 16X, 32X, 64X, or 128X. At the 128X multiplier setting, data points are acquired approximately every 1 nm of carriage travel. The multiple PLL filters enable the user to balance the system parameters of resolution and sensitivity against the acquisition time and refresh rate.
 
The Redstone OSA30x instruments instead sample the interferogram at a fixed frequency of up to 1 MHz with an 18-bit ADC while the retroreflector platform moves at a constant speed controlled by a PID loop. At the highest sensitivity setting, there is one data point collected about every 1 nm of travel. The collected data is resampled to fit up to 128 data points per reference laser period.

The fine sampling can be very useful when the measured light is weak and broadband, causing only a very short interval in the interferogram at the ZPD to contain all the spectral information. This portion of the interferogram is normally referred to as the center burst.

A high-speed USB link transfers the interferograms to the OSA software, which is highly optimized to take full advantage of modern multi-core processors, as well as top-performing graphics processing units (GPUs). The software performs a number of calculations to analyze and condition the input waveform in order to obtain the highest possible resolution and signal-to-noise ratio (SNR) at the output of the Fast Fourier transform (FFT).

The OSA20xC devices make use of a very low noise and low distortion detector amplifier with automatic gain control provides a large dynamic range, allows optimal use of the ADC, and ensures excellent signal-to-noise (SNR) for up to 10 mW of input power. For low-power signals, the system can typically detect less than 100 pW from narrowband sources. The balanced detection architecture enhances the SNR of the system by enabling the OSA20xC to use all of the light that enters the interferometer, while also rejecting common mode noise.

The Redstone OSA detector modules contain high gain-bandwidth product (GBP) amplifiers, which fully exploit the detectors’ dynamic range, combined with high-current low-noise buffers driving a high-bandwidth 18-bit ADC. Automatic amplifier adjustments optimize the number of used ADC bits (filling ratio). Switchable optical attenuators provide for a wide input power range even with early saturating IR-detectors. Differential amplifiers, as well as balanced transmission architectures with effective screening and filtering techniques, assure a good signal integrity for a high spurious-free dynamic range. 

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Figure 6: A Typical Interferogram

Interferogram Data Processing

The interferograms (see Figure 6) generated by the instrument vary from 50 thousand to 16 million data points depending on the resolution and sensitivity mode settings employed. The FT-OSA software analyzes the input data and intelligently selects the optimal FFT algorithm from our internal library.

Additional software performance is realized by utilizing an asynchronous, multi-threaded approach to collecting and handling interferogram data through the multitude of processing stages required to yield spectrum information. The software's multi-threaded architecture manages several operational tasks in parallel by actively adapting to the PC's capabilities, thus ensuring maximum processor bandwidth utilization. Each of our FT-OSA instruments ships complete with a laptop computer that has been carefully selected to ensure that both the data processing and user interface operate optimally.

Wavelength Meter Mode

When narrowband optical signals are analyzed, the FT-OSA automatically calculates the center wavelength of the input, which can be displayed in a window just below the main display that presents the overall spectrum. The central wavelength, λ, is calculated by counting interference fringes (periods in the interferogram) from both the input and reference lasers according to the following formula:

Here, m_ref is the number of fringes for the reference laser, m_meas is the number of fringes from the input laser, n_ref is the index of refraction of air at the reference laser wavelength (632.9918 nm or 1532.8323 nm), and λ_ref,vac is the vacuum wavelength of the reference laser. n_meas is the index of refraction of air at the wavelength λ_meas,vac and is determined iteratively from λ_meas,air (that is, the measured wavelength in air) using a modified version of the Edlén formula (OSA software version 2.90 or lower) or Ciddor's formula (OSA software version 3.00 or higher).

The resolution of the FT-OSA operating as a wavelength meter is substantially higher than the system when it operates as a broadband spectrometer because the system can resolve a fraction of a fringe (see the Interferogram Data Acquisition section above). In practice, the resolution of the system is limited by the bandwidth and structure of the unknown input, noise in the detectors, drift in the reference laser, interferometer alignment, and other systematic errors. In Wavelength Meter mode, the system has been found to offer reliable results as low as ±0.1 pm in the visible spectrum and ±0.2 pm in the NIR/IR (see the Specs tab for details).

The software evaluates the spectrum of the unknown input in order to determine an appropriate display resolution. If the data is unreliable, as would be the case for a multiple peak spectrum, the software disables the Wavelength Meter mode so it does not provide misleading results.

Wavelength Calibration and Accuracy

The OSA20xC instruments use a built-in stabilized HeNe reference laser with a vacuum wavelength of 632.9918 nm. The use of a stabilized HeNe ensures long-term wavelength accuracy as the dynamics of the stabilized HeNe are well-known and controlled. The Redstone OSA30x incorporates a frequency-locked reference laser with a vacuum wavelength of 1532.8323 nm. Because of the frequency-lock, long-term wavelength accuracy is ensured, and the reference laser is connected to an FC/APC output and can be fed into the instrument fiber input for additional calibration if so desired.

The instrument is factory-aligned so that the reference and unknown input beams experience the same optical path length change as the interferometer is scanned. The effect of any residual alignment error on wavelength measurements is less than 0.5 ppm; the input beam pointing accuracy is ensured by a high-precision ceramic receptacle and a robust interferometer cavity design. No optical fibers are used within the scanning interferometer. The wavelength of the reference laser in air is actively calculated for each measurement using the Edlén formula (OSA software version 2.90 or lower) or Ciddor's formula (OSA software version 3.00 or higher) with temperature and pressure data collected by sensors internal to the instrument.

Optical Rejection Ratio

The ability to measure low-level signals close to a peak is determined by the optical rejection ratio (ORR) of the instrument. It can be seen as the filter response of the OSA and can be defined as the ratio of the power at a peak of interest to the power at a given distance from said peak. For Thorlabs' OSAs, the ORR is defined with a stricter condition: instead of just considering the power at a single data point, e.g., 25 GHz from the peak, the power of the highest noise in the wavelength range from 25 GHz to 2 THz is related to the power of the peak. This way, any additional limiting peaks that are not located at the test distances will still be included in the ORR value:

If the ORR is not higher than the optical signal-to-noise ratio of the source to be tested, the measurement will be limited by the OSA's response, rather than reflecting a true property of the tested source. The table to the right provides an example.

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The underside of the OSA has M4-tapped holes that accept the three mounting feet included with the unit (see the Shipping List tab).

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Item #	Qty	Description
OSA205C	1	Fourier Transform Optical Spectrum Analyzer, 1.0 - 5.6 µm
CRM1	2	Cage Rotation Mount for Ø1" Optics, SM1 Threaded, 8-32 Tap
LPMIR050-MP2	2	Ø12.5 mm SM05-Mounted Linear Polarizer, 1500 - 5000 nm
SM1A6	2	Adapter with External SM1 Threads and Internal SM05 Threads, 0.15" Long
ER4-P4	1	Cage Assembly Rod, 4" Long, Ø6 mm, 4 Pack
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Item #	Qty	Description
OSA205C	1	Fourier Transform Optical Spectrum Analyzer, 1.0 - 5.6 µm
CRM1/M	2	Cage Rotation Mount for Ø1" Optics, SM1 Threaded, M4 Tap
LPMIR050-MP2	2	Ø12.5 mm SM05-Mounted Linear Polarizer, 1500 - 5000 nm
SM1A6	2	Adapter with External SM1 Threads and Internal SM05 Threads, 0.15" Long
ER4-P4	1	Cage Assembly Rod, 4" Long, Ø6 mm, 4 Pack
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Cage-Mounted Polarizers in Front of Free-Space Input (OSA205C Shown)

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The free-Space optical input on the Redstone OSA30x accepts collimated beams with ≤Ø10 mm beam diameter.

Directly Compatible with Free-Space Beams

Thorlabs' OSAs each include a free-space optical input aperture, allowing them to directly accept collimated beams up to a maximum beam size of Ø6 mm (OSA20xC) or Ø10 mm (Redstone^® OSA30x). To align the input light source with respect to the OSA's internal interferometer, a red, Class 1 alignment beam is emitted from the aperture; the alignment beam is activated by rotating a switch on the OSA20xC front panel or by a button in the OSA software for the Redstone*. The input source should be made collinear to the alignment beam for the OSA to provide optimal measurement accuracy. Four 4-40 taps around the input aperture enable compatibility with our 30 mm cage system (OSA20xC) or 60 mm cage system (Redstone OSA30x); use cage rods no shorter than 1.5" to prevent attached cage components from clashing with the door.

The OSA20xC interferometer assembly normally "floats" on gel bushings inside the case. When using the free-space input, it may be desirable to lock the interferometer to the optical table surface. This can be accomplished by using the provided mounting feet (see the Shipping List tab) to secure the OSA using two of Thorlabs' CF175C(/M) clamping forks, as illustrated in the image to the right. Likewise, even though the Redstone OSA30x is rigid and does not float, it is recommended to use two or more clamping forks when using the free-space input.

When the OSA20xC interferometers are locked to an optical table, the beam height is 61 mm (2.4") from the table surface. The Redstone OSA30x free-space input accepts a beam height of 117 mm (4.6") above the table surface. To adjust the input beam height to that of the OSA's input, we recommend using Thorlabs' RS99(/M) Periscope Assembly or a periscope constructed with our DP14A(/M) Damped Post.

We recommend only using the posts supplied with the OSA to secure it to the optical table. Other posts, such as our Ø1/2" optical posts, should not be used to secure the OSA; they will not provide adequate support because the OSA20xC and Redstone OSA30x weigh 20 lbs (10 kg) and 58.4 lbs (26.5 kg), respectively. We also do not recommend using long optical posts to raise the OSA off of the optical table surface.

*Additional details for free-space alignment with the Redstone can be found in the application note here.

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A Redstone OSA305 secured to an optical table and used to measure the free-space beam of a laser diode. The laser diode is mounted in a laser diode mount, and the beam is reflected by mirrors mounted in KM100 and KCB1 Kinematic Mounts. The 30 mm cage assembly is coupled to the 60 mm cage rod holes on the Redstone using the previous generation LCP02 which has been replaced by the LCP33 cage plate adapter.

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Item #	Qty	Description
Optical Spectrum Analyzer
OSA205C	1	Fourier Transform Optical Spectrum Analyzer, 1.0 - 5.6 µm
Items Attached to Optical Spectrum Analyzer
KCB1	1	Right-Angle Kinematic Mirror Mount with Tapped Cage Rod Holes, 30 mm Cage System and SM1 Compatible, 8-32 and 1/4"-20 Mounting Holes
PF10-03-P01	1	Ø1" Protected Silver Mirror
ER3-P4	1	Cage Assembly Rod, 3" Long, Ø6 mm, 4 Pack
ERSCB-P4	1	Rod Adapter for Ø6 mm ER Rods, L = 0.27", 4 Pack
CF175C	1	Clamping Fork for Ø1.25" Pedestal Bases, 1.75" Counterbored Slot, 1/4"-20 Captive Screw
Other Items
LDM9T	1	Laser Diode Mount with Integrated Temperature Controller
C171TMD-C	1	f = 6.2 mm, NA = 0.30, WD = 2.8 mm, Mounted Aspheric Lens, ARC: 1050 - 1700 nm
S1TM08	1	SM1 to M8 x 0.5 Lens Cell Adapter
POLARIS-K1E	2	Polaris® Ø1" Mirror Mount, 3 Adjusters, Monolithic Optic Retention
PF10-03-P01	1	Ø1" Protected Silver Mirror
RS1P8E	2	Ø1" Pedestal Pillar Post, 8-32 Taps, L = 1"
RS4M	1	Ø25.0 mm Post Spacer, Thickness = 4 mm
RS10M	1	Ø25.0 mm Post Spacer, Thickness = 10 mm
CF175C	2	Clamping Fork for Ø1.25" Pedestal Bases, 1.75" Counterbored Slot, 1/4"-20 Captive Screw
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View Metric Product List

Item #	Qty	Description
Optical Spectrum Analyzer
OSA205C	1	Fourier Transform Optical Spectrum Analyzer, 1.0 - 5.6 µm
Items Attached to Optical Spectrum Analyzer
KCB1/M	1	Right-Angle Kinematic Mirror Mount with Tapped Cage Rod Holes, 30 mm Cage System and SM1 Compatible, M4 and M6 Mounting Holes
PF10-03-P01	1	Ø1" Protected Silver Mirror
ER3-P4	1	Cage Assembly Rod, 3" Long, Ø6 mm, 4 Pack
ERSCB-P4	1	Rod Adapter for Ø6 mm ER Rods, L = 0.27", 4 Pack
CF175C/M	1	Clamping Fork for Ø1.25" Pedestal Bases, 44.4 mm Counterbored Slot, M6 x 1.0 Captive Screw
Other Items
LDM9T/M	1	Laser Diode Mount with Integrated Temperature Controller, Metric
C171TMD-C	1	f = 6.2 mm, NA = 0.30, WD = 2.8 mm, Mounted Aspheric Lens, ARC: 1050 - 1700 nm
S1TM08	1	SM1 to M8 x 0.5 Lens Cell Adapter
POLARIS-K1E	2	Polaris® Ø1" Mirror Mount, 3 Adjusters, Monolithic Optic Retention
PF10-03-P01	1	Ø1" Protected Silver Mirror
RS1P4M	2	Ø25.0 mm Pedestal Pillar Post, M4 Taps, L = 25 mm
RS4M	1	Ø25.0 mm Post Spacer, Thickness = 4 mm
RS10M	1	Ø25.0 mm Post Spacer, Thickness = 10 mm
CF175C/M	2	Clamping Fork for Ø1.25" Pedestal Bases, 44.4 mm Counterbored Slot, M6 x 1.0 Captive Screw
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An OSA205C secured to an optical table and used to measure the free-space beam of a laser diode. The laser diode is mounted in an LDM9T Laser Diode Mount, and the beam is redirected by mirrors mounted in POLARIS-K1E and KCB1 Kinematic Mounts.

Software

Version 3.31

This version includes a GUI for controlling the OSA20xC and Redstone^® OSA30x, as well as a "virtual device" mode ideal for evaluating the software prior to purchase.

ThorSpectra Software for the Optical Spectrum Analyzers

Each Optical Spectrum Analyzer includes a Windows^® laptop with our OSA software suite pre-installed. This software features a straightforward, intuitive, responsive interface that exposes all functions in one or two clicks. We regularly update this software to add significant new features and make improvements suggested by our users. Several key functions are explained in the Tutorial Videos tab.

The software download page also offers programming reference notes for interfacing with our instruments using LabVIEW^®, Visual C++, and Visual C#.

Version 3.20 and higher can be used to control all OSA20xC, Redstone OSA30x, and CCS series devices. The software can export data into various file formats, including Matlab, Galactic SPC, JCAMP-DX, CSV, and text formats.

Software Highlights

The text below summarizes several key features of the OSA software suite. Complete details on the software are available in the ThorSpectra User Guide.

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Peak Track Mode Used with a 2.8 µm Fabry-Perot Laser

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Coherence Length and Power of 1550 nm Superluminescent Diode (SLD)

Built-In Tools for Simple and Complex Analysis
The OSA software displays either the fast-Fourier-transformed spectrum or the raw interferogram obtained by the instrument. In the main window, it is possible to average multiple spectra or interferograms; display the X-axis in units of nm (in air or vacuum), cm^-1, cm^-1 (Raman Shift Wavenumber), THz, or eV; compare the live spectrum to previously saved traces; perform algebraic manipulations on data; and calculate common quantities such as transmittance and absorbance.

Robust graph manipulation tools include automatic and manual scaling of the displayed portion of the trace and markers for determining exact data values and visualizing data boundaries. Automated peak and valley tracking tools (see the screenshot to the right) identify up to 2048 peaks or valleys within a user-defined wavelength range and follow them over a long period of time. Statistical parameters of traces such as standard deviations, RMS values, and weighted averages are available, and a curve fit tool fits polynomials, Gaussians, and Lorentzians to the spectrum or interferogram.

Acquired data can be saved as a spectrum file that can be loaded quickly into the main window. Data can also be exported into Matlab, Galactic SPC, JCAMP-DX, CSV, and text formats.

Adjustable Sensitivity and Resolution Settings
The scan sensitivity and resolution can be adjusted by the user to balance the needs of the experiment against the data acquisition rate. These settings vary the number of data points per interferogram from 50 thousand to 16 million. The sensitivity setting modifies the range of detector gain levels, while the resolution setting controls the optical path difference (OPD). The table in the Specs tab shows how the data acquisition rate depends upon the chosen settings.

Wavelength Meter Tool for Narrowband Sources
For sources with <10 GHz linewidth, the Wavelength Meter tool enables extremely accurate determinations of the center wavelength (±1 ppm accuracy, 0.2 ppm precision, and 0.1 ppm resolution). This mode allows the system to resolve a fraction of a fringe in the interferogram, using the internal stabilized reference laser (see Interferogram Data Acquisition in the Design tab for details). The uncertainty in the measurement is continuously determined and displayed as gray numbers.

As shown in the image to the right, a built-in tool plots the output of the wavelength meter measurement as a function of time. If the software determines that the wavelength meter will give inaccurate results (as it would for broadband sources), it is automatically disabled.

Coherence Length Module for Broadband Sources
Because Thorlabs' OSAs obtain the raw interferogram of the unknown source (as opposed to grating-based spectrum analyzers, which cannot offer this capability), the software is able to calculate the coherence length of the input signal, as shown by the screenshot to the right. The Coherence Length tool considers the envelope of the interferogram and reports the optical path length over which the envelope's amplitude decays to 1/e of its maximum value on both sides.

The ability to view the interferogram in real time allows the user to confirm the coherence length reported by the software and adjust the signal amplitude to avoid saturation. The maximum coherence length measurable by the OSA is limited by the maximum optical path difference in the highest-resolution setting, making this tool best suited for broadband sources.

Apodization and Interferogram Truncation
Since the resolution of any Fourier-transformed spectrum is intrinsically constrained by the finite path length over which the interferogram is measured, the software implements several functions to account for the effect of the finite path length on the spectrum that is obtained. The user may select from a number of apodization methods (dampening functions), including cosine, triangular, Blackman-Harris, Gaussian, Hamming, Hann, and Norton-Beer functions. Furthermore, the effective optical path length can also be shortened to eliminate contributions from high-frequency spectral components.

Libraries for LabVIEW, C, C++, and C#
Device interface libraries containing a multitude of routines for data acquisition, instrument control, and spectral processing and manipulation are also provided with the instrument. These libraries can be used to develop customized software using LabVIEW, C, C++, C#, or other programming languages. We also provide a set of LabVIEW routines to assist with writing your own applications.

Spectroscopic Analysis from HITRAN Reference Database
In environmental sensing and telecom applications, it is often useful to identify atmospheric compounds (such as water vapor, carbon dioxide, and acetylene) whose absorption lines overlap with that of the source being measured. Some example measurements are shown below. The OSA software includes built-in support for HITRAN line-by-line references, which can be used to calculate absorption cross sections as a function of vapor pressure and temperature. The predictions can be fit to the measured trace for comparison, and fits using mixtures of gases are supported. See the Gas Spectroscopy tab for an example setup.

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Experimentally Measured Carbon Dioxide (CO₂) Absorbance in Near-Infrared

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Carbon Dioxide Absorption Before and After Baseline Correction

Software Tutorial Videos

To help customers learn about, use, and understand the Optical Spectrum Analyzer software, we have prepared several short narrated videos that describe the basic aspects of the software and the optimal settings for common types of measurements. Although the OSA model shown in the videos has been discontinued, the principles of operation have not changed.

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OSA202C Contents (North American Power Cords Shown)

Shipping List

Every OSA20xC order includes the following:

• Optical Spectrum Analyzer
• Windows^® Laptop
  
  • Includes Pre-Installed OSA Software (Version 3.30) and a Mouse
  • U.S. English Configuration
• Factory Calibration Report
• OSA and Laptop Power Supplies with Region-Specific Power Cords
• High-Speed USB 2.0 Cable (Replacement Item # USB-A-79)
  • Connects the OSA to the Laptop
• Three Mounting Feet
  • Used to Secure the Interferometer to an Optical Table (See Free-Space Coupling Tab)
• SPW603 Spanner Wrench and VP10C Vacuum Pickup Tool
  • Used to Remove Protective Window in Front of Free-Space Input in Cases When
    Etalons are Visible in the Spectrum

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Redstone OSA305 Contents (North American Power Cords Shown)

Every Redstone^® OSA30x order includes the following:

•  Optical Spectrum Analyzer
•  Windows^® Laptop
  • Includes Pre-Installed OSA Software (Version 3.30) and a Mouse
  • U.S. English Configuration
• Factory Calibration Report
• OSA and Laptop Power Supplies with Region-Specific Power Cords
• USB 3.0 Cable (Replacement Item # CABU31)
  • Connects the OSA to the Laptop
• SPW801 Spanner Wrench and VP10C Vacuum Pickup Tool
  • Used to Remove Protective Window in Front of Free-Space Input in Cases When
    Etalons are Visible in the Spectrum
• Lens Tube Adapter for Free-Space Port
• Calibration Patch Cable (Replacement Item # P5-SMF28E-FC-2)

Analyzing Pulsed Sources Using the OSA20xC and Redstone^® Instruments

Impact of a Pulsed Source on the Interferogram and Spectrum
As the Optical Path Difference (OPD) continuously changes during an interferogram measurement, a pulsed light source effectively modulates the interferogram. In the case of 100% modulation (i.e. on-off pulsation), the resulting interferogram will contain repetitive regions (slots) with no information. These slots correspond to OPDs when no light can be measured by the detector assembly. The resulting interferogram in this case is the true interferogram masked with the pulsed signal. Figure 1 shows measured interferograms and the corresponding spectra for a light source in CW and pulsed operation. Although the spectrum of the light source is expected to be the same for CW and pulsed operation (ignoring small changes in the peak shape and position due to, for example, a decreased LD chip temperature resulting from the pulsed drive), additional frequency artifacts appear symmetrically about the expected peak due to the modulation in the pulsed interferogram. These "spectral ghosts" are a result of the temporal, rather than the spectral, behavior of the source. To measure the true spectrum of the light source, it is crucial to make the spectral ghosts sufficiently small or force the spectral ghosts to fall outside the frequency / wavelength range of interest.

Figure 1: Interferograms and spectra for a narrowband light source in CW (Top) and pulsed at 20 kHz (Bottom)
operation measured with an OSA20xC device. The square wave modulation of the interferogram induces the spectral ghosts shown in the bottom right plot.

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Figure 2: Stacked spectra for 55 pulse repetition rates between 100 Hz and 100 kHz for a 1550 nm DFB laser diode measured with an OSA20xC device. The intensity is mapped in a logarithmic scale. OSA settings: High Resolution, High Sensitivity, No Apodization, 5 averages.

Mathematically, the resultant spectrum of a pulsed source can be described by a convolution between the spectrum of the light source and the spectrum corresponding to the pulses. As a result, the impact of these artifacts will vary with the pulse repetition rate and the modulation depth of the light source as well as the OPD sample rate (cm/s) of the OSA. The modulation depth of the light source determines the amplitude of the spectral ghosts; a weak modulation yields weak spectral ghosts while a modulation of 100% (on-off pulsation) yields the strongest spectral ghosts.

Figure 2 shows how the behavior of the spectral ghosts as a function of the pulse repetition rate for a narrowband source. In the figure, the spectra were measured for 55 pulse repetition rates between 100 Hz and 100 kHz for a 1550 nm DFB laser diode connected to an OSA20xC device. We have offset the y-axis such that the true peak (the light gray horizontal line) has been centered at a relative frequency of 0 THz. The figure can be divided into three regions: f_p ≤ 3 kHz, 3 kHz < f_p ≤ 30 kHz and f_p >30 kHz. For f_p ≤ 3 kHz, the spectral ghosts are clearly observed symmetrically about the true peak within the resultant spectrum, and move farther and farther away from the true peak as the repetition rate increases. The second region starts above 3 kHz, when the first spectral ghosts have moved beyond the spectral range of the OSA. However, aliasing / folding create higher order spectral ghosts that appear within the spectral range of the OSA. In the third region, f_p > 30 kHz, the resulting spectrum agrees very well with the CW spectrum because the repetition rate of the source has extended beyond the bandwidth limit of the detectors. As a result, the pulsed source appears like a CW source to the OSA electronics.

"Pulsed Mode" Operation
To help remove some of these frequency artifacts, the OSA software contains a "Pulsed Mode" measurement (Figure 3). The "slot period" of the interferogram, determined by the pulse repetition rate of the light source and the OPD rate of the OSA, affects the positions of the spectral ghosts. A shorter slot period yields a larger spectral distance between the true peak and the first order ghost peaks. In Thorlabs' OSAs, the OPD sample rate is given by the speed of the moving carriage which can be controlled by the user indirectly through the sensitivity setting. The higher the sensitivity setting is, the slower the speed of the moving carriage will be. Thus, the use of the "High" sensitivity mode of the OSA will provide the shortest slot period (i.e. the largest spacing between the feature of interest and the frequency artifacts). In Pulsed Mode, the software acquires several spectra with different sensitivity settings (or OPD sample rates) and filters out the changing spectral features. The sensitivity is set to increasingly high levels, starting with Low. After reaching the highest sensitivity, it is again set to Low, yielding a periodically changing sensitivity. The captured spectra are then combined using the minimum hold function. The spectral ghosts (Figure 4), whose positions depend on the sensitivity setting (the OPD rate), can then be reduced in the measurement as shown in Figure 4. It is important to note that the Pulse Mode button is found under the "Sweep" or "Instrument" menu and can be started only after the current sweep has been completely stopped.

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Figure 3: Screenshot of the OSA software in Pulsed
Mode; the icon is indicated with a red circle.

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Figure 4: (Left) Measured spectra for a narrowband light source pulsed at 1 kHz with (from top to bottom) Low, Medium-Low, Medium-High, and High sensitivity settings (i.e. a decreasing OPD sample rate from top to bottom). (Right) Measured spectrum using the Pulsed Mode, i.e., a minimum hold combination of spectra similar to those shown in the bottom left plots.

Narrowband Light Source
A DFB laser diode emitting at 1550 nm (193.7 THz) was used as a narrowband light source and measured with an OSA203C in both CW and pulsed operation. The laser diode was modulated (using Thorlabs' ITC4001 controller) with repetition rates between f_p = 20 Hz and 100 kHz. Five averaged spectra were captured for each light source setting; the CW spectra were acquired in high sensitivity mode, and the pulsed spectra were recorded in both high sensitivity and pulsed mode. It is important to note that the pulsed mode does not allow averaging. Instead the minimum hold function was used for 5 sets of spectra from the four different sensitivity settings.

Figure 5 shows the resultant spectra for the source in CW mode as well as four different pulse repetition rates between 100 Hz and 100 kHz. As the pulse rate increases, the spectral ghosts (as recorded in the high sensitivity mode) move further and further away from the true laser peak until nearly identical spectra are obtained at 100 kHz.

Figure 5: Spectra from measurements of a 1550 nm (193.7 THz) pulsed narrowband source. Pulse repetition rates shown (left to right): 100 Hz, 1 kHz, 13 kHz, and 100 kHz. Black line: CW measurement; blue line: pulsed source measured with high sensitivity; red line: pulsed source measured using the pulsed mode. The lower plots are the same data set as the upper plots only on a shorter frequency scale.

Broadband Light Source
A gain chip was driven in amplified spontaneous emission (ASE) mode to create a broadband light source centered at 850 nm (352.9 THz) with a FWHM of 36.4 nm (15.2 THz). An OSA201C was used to measure the spectrum for CW and pulsed operation with pulse repetition rates from f_p = 100 Hz to 100 kHz. The ASE diode was modulated (using Thorlabs' ITC4001 controller) with a 50% duty cycle square wave. A total of 10 averaged spectra were acquired using high sensitivity (CW and pulsed sources) and the pulsed mode (pulsed source). Because pulsed mode does not allow averaging, the minimum hold function was used to acquire five sets of the four different sensitivity settings.

In general, the spectral ghosts are less visible for the broadband peak compared to a narrowband peak. However, the noise floor is higher and the spectral ghosts are clearly seen for a repetition rate of 1 kHz and 13 kHz in Figure 6. Similar to the narrowband source, the spectral ghosts move farther and farther away from the true peak with increasing repetition rate. For a repetition rate of 100 kHz both the measurement using high sensitivity and pulsed mode agree well with the CW measurement. As seen, the shape of the peak is slightly different for the CW spectrum compared to the pulsed spectrum. This is not related to the behavior of the OSA but due to a true change in the peak during pulsed operation, e.g., a lower chip temperature.

Figure 6: Measured spectra from a pulsed broadband source with a center wavelength (frequency) of 850 nm (352.9 THz). The pulse repetition rates shown are 100 Hz, 1 kHz, 13 kHz, and 100 kHz. Top and bottom rows show the full spectrum and the ±50 THz range surrounding the peak, respectively. Black line: CW; blue line: pulsed source measured using high sensitivity; red line: Pulsed Mode.

It is extremely important to note that in general, one has to be careful when measuring broadband peaks at low repetition rates. Since most of the information in the interferogram is located about the zero burst, the peak can be completely missed if the zero burst coincides with no light falling on the detector as shown in Figure 7.

Figure 7: Measured interferograms (left) and spectra (right) obtained when the zero burst resulting from a broadband
source coincides with a pulse (blue curves) and is missed if no light reaches the detector at OPD ~ 0 (red curves).

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Figure 8: (Top) Central portion of a captured interferogram from a broadband femtosecond laser. (Bottom) Measured spectrum captured using an OSA201 (red line) and a measured reference spectrum captured using a scanning grating-based OSA (blue line).

Femtosecond Pulsed Laser
We measured the spectrum of a broadband femtosecond laser using an OSA201C. This laser has a repetition rate of 85 MHz, a pulse width of 10 fs, and an average power of about 300 µW into the fiber. The OSA was set to Low Resolution, High Sensitivity, 5 spectral averages, and no apodization. Light output from the laser was collected with a fiber patch cable (SM600 fiber; 0.12 NA, 4.6 µm mode field diameter at 680 nm) connected to the OSA.

Figure 8 shows the interferogram collected during acquisition, which does not contain any empty slots. This was expected as the 85 MHz repetition rate of the laser is well beyond the 40 kHz bandwidth of the OSA's detectors. Furthermore, the spectrum measured by the OSA agrees very well with the reference spectrum captured using a grating-based OSA that is scanned slowly enough to provide adequate signal for each wavelength measured.

Item #	Frequency Range	Level Sensitivity (Click for Graph)a
OSA207C	833 - 10 000 cm-1 (12.0 - 1.0 µm)	Absolute Power Power Density
OSA205C	1786 - 10 000 cm-1 (5.6 - 1.0 µm)
OSA305
OSA203C	3846 - 10 000 cm-1 (2.6 - 1.0 µm)
OSA302	4000 - 40 000 cm-1 (2.5 µm - 250 nm)

• Lower values of Level Sensitivity correspond to improved detection sensitivity. We therefore recommend selecting the OSA which provides the lowest level sensitivity for the analytes you intend to study.

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Rear-Mounted Hose Connections for Purging the Redstone^® OSA30x Cavity

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Hose Connections for Purging OSA20xC Cavity

Gas Detection and Identification Using an Optical Spectrum Analyzer

As shown in the table to the right, many of Thorlabs' Optical Spectrum Analyzers (OSAs) offer detection extending into the mid-infrared (MIR) region of the spectrum, where many gaseous species characteristically absorb. Moreover, the software included with all OSA models supports files from the HITRAN database, a spectroscopic reference standard. These files can be fit to measured traces to identify unknown gases. With the ability to fit multiple analytes simultaneously and built-in hose connections (compatible with Thorlabs' Pure Air Circulator Unit) for purging the interferometer's cavity of trace gases, these OSAs are ideal for use in home-built gas detection setups.

Experimental Setup
A sample detection setup is shown below. Broadband MIR light generated by a Stabilized Light Source is emitted from a zirconium fluoride fiber (), collimated, then sent into a multipass cell () containing the gas analyte in a sample chamber. Each end of the chamber is sealed by an airtight, transparent window. Gold mirrors on each side of the chamber provide multiple reflections that increase the sensitivity of the measurement; the mirror closer to the light source has a center hole to allow the optical path to enter and exit the chamber. Light exiting the detection setup is collimated by a long-focal-length lens and reflected by a D-shaped mirror into the free-space port of the OSA203C (). The temperature inside the chamber is elevated and held constant in order to prevent the gas's absorption lines from shifting during the measurement.

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A gas detection setup using the OSA203C. A multipass cell is constructed around the sample chamber () in order to provide high detection sensitivity for the gaseous species sealed inside.

Parts Used in Sample Setup (Click Here for a Metric Item List)
Item #	Qty.	Description
Light Source
SLS202La	1	Stabilized Fiber-Coupled Light Source, 450 nm - 5.5 µm (Not Shown)
FB2000-500	1	Ø1" Bandpass Filter, 2.0 µm CWL, 0.5 µm FWHM (Not Shown)
MZ21L1	1	ZrF4 Multimode Fiber Patch Cable, SMA905 Connectors
F028SMA-2000	1	SMA905 Fiber Collimator, AR Coated: 1.8 - 3.0 µm
POLARIS-K1b	1	Polaris® Ø1" Kinematic Mirror Mount
AD11NT	1	Unthreaded Adapter for Ø11 mm Cylindrical Components
Detection
OSA203C	1	Optical Spectrum Analyzer, 1.0 - 2.6 µm
TC200c	2	Temperature Controller
MB1218	1	12" x 18" Aluminum Breadboard
CF125C	3	Clamping Fork with Captive Screw
Other Optomechanics
RS2	6	Ø1" Pillar Post, Length = 2"
RS3	1	Ø1" Pillar Post, Length = 3"
RS4	2	Ø1" Pillar Post, Length = 4"
BA2F	9	Flexure Clamping Base

• This item is no longer available for purchase. Stabilized light sources with similar performance are available here. Please contact Technical Support for assistance with your specific application.
• This previous-generation item is not available for individual purchase. The POLARIS-K1E Ø1" Kinematic Mirror Mount is available as an alternative.
• This previous-generation item is not available for individual purchase. The TC300B Heater and TEC Temperature Controller is available as an alternative.

Parts Used in Sample Setup (Continued) (Click Here for a Metric Item List)
Item #	Qty.	Description
Beam Path Into and Out of Multipass Cell
LB4374	1	Uncoated, Ø1", f = 1000 mm Bi-Convex UV Fused Silica Lens
CP33	1	Post-Mountable, SM1-Threaded Cage Plate for Ø1" Optics
CM750-200-M01	2	Ø75 mm, f = 200 mm Protected Gold Concave Mirror (One Mirror Contains a Center Hole, Similar to Our Herriott Cell Mirrors)
KS3	2	Kinematic Mount for Ø3" Mirrors
VPCH512	2	Ø2.75" CF Flange with CaF2 Window, 180 nm - 8.0 µm
N/A	1	Sample Chamber
C1513	1	Kinematic V-Clamp Mount
PM4	2	Clamping Arm (One Clamping Arm is Included with Each C1513 Mount)
P6	1	Ø1.5" Mounting Post, Length = 6"
PB2	1	Base for Ø1.5" Mounting Posts
PFD10-03-M01	1	1" Protected Gold D-Shaped Pickoff Mirror
KM100D	1	Kinematic Mount for 1" D-Shaped Pickoff Mirrors
MB624	1	6" x 24" Aluminum Breadboard

Assigning Peaks in an Unknown Spectrum
Once the experimental spectrum is obtained, the user chooses a gas or gas mixture that is believed to be present inside the sample chamber, as shown in the figure below to the left. There is no limit to how many species can be considered in the fit, but the fit is more likely to converge when fewer species are chosen. The OSA software ships with HITRAN line-by-line references for acetylene (C₂H₂), water vapor (H₂O), and carbon dioxide (CO₂), and can import additional references downloaded from the HITRAN database. Previously saved spectra in the OSA file format can also be used as references. See the References section of the ThorSpectra manual for details.

The user may optionally allow the software to shift the reference spectrum in wavelength in order to account for measurement effects related to the sample environment. In the case of gas mixtures (i.e., fits performed using more than one reference spectrum), the software scales the intensity of each reference as needed to reproduce the measured spectrum. As shown in the figure below to the right, the output of the fit operation is a graph comparing the measured spectrum, each scaled (and possibly also shifted) reference spectrum, and the sum of the scaled reference spectra.

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In the Reference Fit Setup tab, checkboxes are used to indicate which gaseous species to consider in the fit. The absorption lines can be either "fixed" or "free"; the latter allows the software to shift the reference spectrum in wavelength. The measurement conditions for the HITRAN references are also displayed.

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In the Reference Fit Result tab, the fitted spectrum is displayed simultaneously with the measured spectrum. The fitted spectrum is the sum of the scaled reference spectra included in the fit. The scaled spectrum for each individual gaseous species is also shown.

Olle Rosenqvist
OSA R&D Manager

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Custom OSA Options

• Optical Input
  • FC/PC, FC/APC, or SMA905 Fiber Receptacles
  • Permanently Installed Optical Bandpass and Notch Filters Before Interferometer
• Application-Optimized Detectors
  • High Sensitivity for Low-Level Signal Detection, Such as in Fluorescence or Raman Measurements
  • Wavelength Range and Noise Floor Chosen to Match a Specific Light Source
• Custom Software Modules for Data Analysis

Thorlabs' in-stock OSA models offer a number of detection options for various experimental situations. We invite customers whose needs are not addressed by these models to tailor an OSA to a specific application by working with our engineering and manufacturing team.

In the past, we have built OSAs with user-specified optical inputs, such as FC/APC and SMA905 fiber receptacles, and we have incorporated optical bandpass and notch filters directly into the optical path to reduce light source noise. For customers who use these instruments for sample characterization, our software team has implemented user-designed data analysis modules within the standard OSA software suite.

We have also worked with our customers to choose detector elements targeted at specific light sources and analytes. The graphs below were obtained from custom-built OSAs that were designed for especially high detection sensitivity. Our engineers are well-versed in the tradeoffs between detection bandwidth, sensitivity, and linearity, and can make recommendations based upon the needs of the application and prior customers' experiences. By constraining the OSA's design for a particular use case, additional performance enhancements for that application can be realized.

If you would like to discuss a custom OSA, please contact us with your experimental requirements.