Cooled spectrometer

Introduction

A cooled spectrometer is a spectrometer with the cooled detector, used to measure the spectra of the light with the reduced noise and the improved sensitivity, and it is used in the astronomy, the physics, the chemistry, the research, and the many other applications. The cooled spectrometer measures the spectrum of the light by the dispersion with the grating or the prism, and the detector is cooled to reduce the thermal noise, providing the improved signal-to-noise ratio and the sensitivity; the cooled spectrometer consists of an entrance slit, a dispersing element, a cooled detector, such as the cooled charge-coupled device (CCD) camera, the electronics, and the software, and it provides the spectrum, with features such as the high sensitivity; the cooled spectrometer is used for the measurement of the spectra in the astronomy, for the spectroscopic analysis, for the measurement of the weak signals, for the research, and for many other applications, and it is an essential instrument for the sensitive spectroscopy. Cooled spectrometers are used in the astronomy, in the physics, in the chemistry, in the research, and for many other applications. With their cooled detectors, cooled spectrometers are essential for the sensitive spectral measurement.

Cooled Spectrometer LCSP-T2010

Cooled Spectrometer is designed for high-precision spectral analysis that offers a wavelength range of 180 to 1100 nm. It has a built-in thermoelectric cooling system that cools the dete...

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Standards

European Pharmacopoeia 2.2.25-Spectrophotometry, ultraviolet and visible

ASTM E275-08(2022)-Standard Practice for Describing and Measuring Performance of Ultraviolet, Visible, and Near-Infrared Spectrophotometers

Complies with the above standards, but is not limited to them.

Features

1. Cooled spectrometer with thermoelectrically cooled detector for low-light and high-sensitivity spectral measurement.

2. Peltier-cooled CCD/CMOS detector reduces dark noise for improved signal-to-noise in low-light applications.

3. Suitable for fluorescence, Raman, luminescence, low-light spectroscopy, research and quality control.

4. Includes spectrometer optical bench, cooled detector, cooling system, controller, software and operation manual.

5. Supports high-sensitivity spectral acquisition for weak light signals and long-integration measurements.

FAQ

Q1: What testing scenarios is this spectrometer mainly applied to?

A: The cooled spectrometer is used in fluorescence spectroscopy, Raman spectroscopy, photoluminescence, chemiluminescence, low-light spectral measurement, materials research, life sciences, environmental monitoring, and quality control to measure spectra of weak light signals with high sensitivity and low noise, using a thermoelectrically (Peltier) cooled detector (typically CCD or CMOS) that reduces dark current noise by cooling the detector to -20 to -70 degrees C, enabling long integration times (seconds to minutes) for detecting weak signals that would be lost in the noise of an uncooled detector. It supports fluorescence spectroscopy (emission and excitation spectra of fluorescent dyes, proteins, quantum dots, GFP, fluorophores - weak fluorescence signals require high sensitivity; cooled detector reduces noise for low-concentration samples), Raman spectroscopy (Raman scattering is inherently weak (1 in 10^6-10^8 photons scattered) - cooled detector is essential for acquiring quality Raman spectra with reasonable integration times; used for material identification, pharmaceutical analysis, forensic science, art conservation), photoluminescence (PL) spectroscopy (semiconductors, nanomaterials, perovskites, LEDs - PL intensity can be weak for low-quantum-yield materials; cooled detector enables measurement of weak PL signals and temperature-dependent PL), chemiluminescence and bioluminescence (light emitted from chemical reactions or biological processes - very weak signals; cooled detector with long integration can detect these without external light source), low-light absorption/transmission spectroscopy (samples with very low light transmission (high absorbance, opaque samples, thin films) - cooled detector can measure the weak transmitted light with long integration), UV-Vis-NIR spectroscopy of dilute samples (very dilute solutions with weak absorption - cooled detector improves SNR for accurate measurement of small absorbance values), spectral radiometry and light source characterization (weak light sources, LED characterization, lamp spectral output - cooled detector for accurate measurement of low-intensity sources), and research applications requiring high spectral sensitivity and low noise. The cooled detector provides 10-100x improvement in signal-to-noise ratio compared to uncooled detectors for long integration times, making it essential for weak-light spectroscopy.

Q2: What standards does the spectrometer comply with?

A: The cooled spectrometer follows relevant ISO, ASTM, IEC and GB/T standards for spectroscopic instruments, including ISO 11151 (lasers and laser-related equipment - standard optical components, related), ASTM standards for spectroscopic methods (ASTM E131 for wavelength calibration, ASTM E2056 for multivariate calibration, relevant ASTM methods for fluorescence, Raman, UV-Vis), IEC 61010 (safety requirements for electrical laboratory equipment), and relevant GB/T standards for spectroscopic instruments. The hardware complies with applicable EMC standards (IEC 61326). Calibration should use certified wavelength standards (holmium oxide glass, mercury-argon lamp, neon lamp - for wavelength calibration; traceable to national standards) and certified photometric standards (NIST-traceable spectral irradiance standard lamp - for intensity/responsivity calibration). For research use, follow established scientific protocols and cite instrument model and settings in publications. Users should verify the specific spectral range (UV, Vis, NIR), resolution, and detector type for their application and measurement requirements.

Q3: What is the warranty period for the whole spectrometer and key components?

A: The whole cooled spectrometer is covered by a 12-month warranty. The optical bench (slit, grating, mirrors, collimator), cooled detector (CCD/CMOS with Peltier cooler), cooling system (thermoelectric cooler, heat sink, fan), controller, data acquisition, software and housing are covered, while calibration lamps, optical fibers, probes, filters, slit plates, cooling fan, and fuses are consumables or accessories. Damage from improper use, detector damage (saturation/blooming from overexposure, moisture condensation inside detector (if cooled below dew point without proper purging - can cause permanent damage), optical contamination (dust, fingerprints on optics), cooling system failure, or unauthorized repair is excluded. Extended warranty may be available for this research instrument. The detector (CCD/CMOS) may have separate warranty terms (typically 1-2 years; detectors are precision components and can be damaged by overexposure, static discharge, or moisture). Peltier cooler may have separate lifespan (typically 10000+ hours).

Q4: Is this device difficult to operate? Is professional training required?

A: Operation requires trained researchers or technicians familiar with spectroscopy, optical alignment, and detector operation. We provide operation manuals, training and application support. Proper instrument setup (wavelength calibration (with certified standard - verify wavelength accuracy before use; recalibrate if grating is moved or temperature changes significantly), intensity/responsivity calibration (with standard lamp - for quantitative intensity measurements; calibration is valid only for the specific optical configuration (fiber, probe, slit) used), dark current measurement (take dark spectrum with shutter closed at the same integration time and temperature as sample measurement - subtract dark from sample to remove dark noise; dark current is temperature-dependent, so maintain stable detector temperature), cooling system operation (allow detector to reach set temperature before measurement (typically 5-15 minutes); maintain stable cooling temperature throughout measurement; ensure proper heat dissipation (fan operation, ambient temperature < 30 degrees C); for deep cooling (< -40 degrees C), may require nitrogen purging to prevent condensation (dry air or nitrogen purge of detector chamber to prevent moisture condensation on cold detector - condensation causes permanent damage; verify purge flow if required)), measurement parameters (integration time (set to maximize signal without saturation - typically 60-80% of full scale; longer integration improves SNR for weak signals but increases dark noise; for cooled detector, dark noise is low so long integration is beneficial), number of scans to average (averaging multiple scans improves SNR by sqrt(N) - typically 3-10 scans; boxcar averaging/smoothing can further improve SNR but reduces resolution), slit width (narrower slit = higher resolution but lower light throughput; wider slit = more light but lower resolution; select based on resolution requirements and signal strength), grating (select grating for spectral range and resolution - higher groove density = higher resolution but narrower range; lower groove density = wider range but lower resolution), sample handling (for fluorescence: use right-angle geometry for clear solutions, front-face for opaque/turbid samples, proper cuvette (quartz for UV, glass for Vis only); for Raman: use proper laser wavelength and power, sample holder (cuvette, capillary, slide), avoid fluorescence interference (use longer wavelength laser (785 nm, 1064 nm) for fluorescent samples, or fluorescence quenching); for absorption: use matched cuvettes, proper blank, avoid stray light), data processing (dark subtraction, reference/background correction, baseline correction, peak identification, spectral library matching, quantitative analysis (calibration curves, multivariate methods)), quality control (wavelength verification (use standard lamp or holmium glass), intensity verification (use standard lamp or reference material), dark noise check (verify dark current is stable and within specification), detector linearity check (verify response is linear over used range)), and maintenance (clean optics (only if necessary - use proper lens tissue and solvent; avoid touching grating (never clean grating - damaged coating); clean external optics only), check cooling fan, verify detector temperature, store in dry environment when not in use (use desiccant if stored for extended period)) are important for accurate, reliable spectroscopic measurements.

Q5: What is the typical lead-time for order delivery?

A: Standard models require 7-30 working days. In-stock units can ship within 3-7 working days. Custom configurations or large built-to-order systems may require additional time, and we confirm the exact schedule before order confirmation.

Q6: Is regular calibration required? What is the recommended calibration cycle?

A: Wavelength calibration recommended every 3-6 months (or after grating change, significant temperature change, or if wavelength accuracy is suspect) using certified wavelength standard (holmium oxide glass filter for Vis-NIR, mercury-argon lamp for UV-Vis, neon lamp for Vis; verify at multiple wavelengths across the range; record calibration values). Intensity/responsivity calibration recommended every 6-12 months (for quantitative intensity measurements - using NIST-traceable spectral irradiance standard lamp (tungsten-halogen or deuterium-halogen); calibrate at the same optical configuration (fiber, probe, slit, integration time) used for samples; intensity calibration is configuration-specific and must be redone if any optical component is changed). Routine wavelength verification before each use or per day (for critical measurements - use a known emission line (e.g., mercury line at 253.7 nm, 435.8 nm, 546.1 nm) or holmium oxide absorption peaks to verify wavelength accuracy; quick check without full calibration). Dark current/pixel check every 1-3 months (take dark spectrum at standard integration time and temperature; verify dark current level and bad pixels; monitor for increasing dark noise (indicates detector degradation or cooling problem); bad pixels can be corrected in software but should be monitored). Detector cooling temperature verification every 3-6 months (verify actual detector temperature matches set point (using thermistor reading or external sensor; if temperature is unstable or cannot reach set point, check cooling fan, ambient temperature, Peltier cooler). Full spectrometer performance verification annually (wavelength accuracy, resolution, photometric linearity, dark noise, SNR, cooling temperature - per manufacturer specification or ISO/ASTM standards). For research use, maintain calibration records and instrument performance logs (important for data quality and publication reproducibility). Software updates per manufacturer (may include improved calibration algorithms, bug fixes, new features).

Q7: Are supporting consumables universal?

A: Calibration lamps (mercury-argon, neon, holmium oxide glass filter - wavelength calibration; NIST-traceable spectral irradiance standard lamp - intensity calibration), optical fibers (SMA905, FC/PC connectors - various core diameters (100-1000 micrometer), UV/Vis/NIR grades; fiber type should match spectrometer and application), sampling probes (fluorescence probe, Raman probe (with laser coupling), immersion probe, reflection probe - application-specific), light sources (deuterium-halogen (UV-Vis), tungsten-halogen (Vis-NIR), laser (Raman: 532 nm, 785 nm, 1064 nm), xenon flash (fluorescence) - selected based on application), sample holders (cuvette holder (1 cm, 10 cm pathlength), solid sample holder, integrating sphere (for diffuse reflectance), fiber adapter - application-specific), filters (long-pass, short-pass, band-pass - for fluorescence (block excitation light), Raman (block laser line), stray light reduction), slit plates (interchangeable slits for resolution adjustment - spectrometer-specific), cooling fan (replacement), desiccant (for storage), cleaning supplies (lens tissue, isopropanol, compressed air), and fuses are available from spectrometer and optical suppliers, though some accessories (probes, slits, fiber connectors) may be spectrometer-specific (connector type, mounting). Long-term consumable cost includes calibration lamps (periodic replacement - standard lamps have finite lifespan (deuterium ~1000 hours, tungsten ~2000 hours, mercury-argon ~5000 hours); NIST-traceable standard lamps are expensive and should be used only for calibration, not routine use), optical fibers (can degrade over time (bending damage, connector contamination, solarization in UV) - replace when transmission decreases or damage occurs; UV fibers can solarize (permanently lose UV transmission) with prolonged UV exposure), and light source lamps (routine replacement - laser diodes have ~10000 hour lifespan, deuterium lamps ~1000 hours).

Q8: Can I customize parameters or supporting accessories?

A: Customization includes spectral range (UV (190-400 nm), Vis (380-780 nm), NIR (780-2500 nm), UV-Vis (190-1100 nm), Vis-NIR (380-2500 nm), UV-Vis-NIR (190-2500 nm) - select based on application; UV requires deuterium source and quartz optics; NIR requires InGaAs detector (instead of Si CCD/CMOS)), resolution (0.1-20 nm - determined by slit width and grating groove density; higher resolution requires narrower slit and higher groove density grating, but reduces light throughput; select based on application (Raman typically 2-10 cm-1 resolution, fluorescence 1-5 nm, absorption 0.5-2 nm)), detector type (CCD (back-thinned, front-illuminated) for UV-Vis, high sensitivity; CMOS for fast readout, low noise; InGaAs for NIR (900-2500 nm); photodiode array (PDA) for fast, simultaneous measurement; EMCCD for ultra-low light (electron-multiplying CCD, very high sensitivity but higher cost and complexity)), cooling temperature (Peltier cooling to -10, -20, -40, -70 degrees C - deeper cooling = lower dark noise, better for long integration, but higher cost and may require nitrogen purging to prevent condensation; -20 to -40 degrees C is typical for most applications), optical bench (Czerny-Turner (most common, good all-around), crossed Czerny-Turner (compact), Echelle (high resolution, wide range with order sorting), concave grating (no moving parts, rugged)), input (SMA905 fiber connector, FC/PC, free-space, slit width (fixed or interchangeable)), grating (multiple grating turret (2-3 gratings for extended range/resolution), single grating), data acquisition (16-bit, 18-bit ADC; readout speed; USB, Ethernet, WiFi connectivity), software (spectrometer control, data acquisition, processing (baseline, peak picking, library search), quantitative analysis (calibration, multivariate PLS/PCR), fluorescence/Raman-specific analysis modules, SDK for custom programming, 21 CFR Part 11 / data integrity for regulated environments), language and accessories. Additional gratings, slits, fibers, probes, light sources, sample holders, and accessories can be ordered separately. Custom orders extend delivery lead-time significantly, especially for deep-cooled, high-resolution, and NIR models.

Q9: Does the purchase include on-site installation and commissioning service?

A: Standard delivery includes the cooled spectrometer, power supply, USB cable, basic software, and instruction manual. On-site installation, calibration, and training are not included for standard orders but can be arranged at additional cost (recommended for complex systems (Raman, fluorescence with integrated light source) and for users new to spectroscopy). Remote guidance and technical support are provided. Calibration before use is essential (wavelength calibration with standard; intensity calibration if quantitative measurements required; many spectrometers come with factory calibration, but recalibration after shipping and installation is recommended).

Q10: What types of samples are compatible with this equipment?

A: The cooled spectrometer measures spectra of various sample types including liquids (solutions, suspensions, emulsions - in cuvettes (1 cm standard, 0.1-10 cm pathlength); for absorption: clear solutions (Beer-Lambert law applies); for fluorescence: dilute solutions (to avoid inner filter effect and reabsorption; typically absorbance < 0.1 at excitation wavelength); for Raman: any liquid (water has weak Raman, good solvent; organic solvents have Raman peaks that may interfere - use appropriate solvent or subtract background)), solids (powders, pellets, films, coatings, crystals, ceramics, metals, polymers - for reflection/absorption: use integrating sphere (diffuse reflectance) or reflection probe; for fluorescence: front-face geometry (for opaque/turbid solids); for Raman: direct measurement (laser focused on sample surface; solids often give strong Raman signals; use appropriate laser power to avoid sample damage/heating)), gases (gas phase samples in gas cell (pathlength 1-100 cm, with windows (quartz for UV, CaF2/NaCl for IR); gas phase spectra have sharp rotational-vibrational lines (requires high resolution); cooled detector can measure weak gas absorption or emission)), and other samples (biological samples (cells, tissues, biofluids - fluorescence (autofluorescence, labeled samples), Raman (label-free molecular fingerprint); environmental samples (water, soil, air filters - absorption, fluorescence, Raman); forensic samples (drugs, fibers, paints, documents - Raman (non-destructive identification), fluorescence (ink differentiation, counterfeit detection)); art and cultural heritage (pigments, varnishes, binding media - Raman (non-destructive identification), fluorescence (varnish aging, pigment mapping)); pharmaceutical samples (API, excipients, formulations, counterfeit drugs - Raman (fast identification, content uniformity), NIR (quantitative analysis, polymorphism); semiconductors and nanomaterials (PL, Raman, absorption - material characterization, quality control)) within the spectral range, detector sensitivity, resolution, and sample holder specification. Different sample types require specific measurement configurations: Absorption/transmission (measure light transmitted through sample; requires light source (broadband) and sample holder (cuvette, gas cell); calculate absorbance = -log(I/I0) where I0 is reference (blank) intensity; Beer-Lambert law: A = epsilon * c * l; for accurate measurement, absorbance should be 0.1-1.0 (below 0.1 = too much noise, above 1.0 = stray light and detector nonlinearity); use matched cuvettes and proper blank; cooled detector improves measurement of low-transmission (high-absorbance) samples with long integration). Fluorescence (measure light emitted by sample after absorption of excitation light; requires excitation light source (LED, laser, xenon lamp), excitation monochromator/filter, sample holder, emission spectrometer (the cooled spectrometer); right-angle geometry for clear dilute solutions (90 degrees between excitation and emission); front-face for opaque/turbid samples; measure emission spectrum (fixed excitation, scan emission) or excitation spectrum (fixed emission, scan excitation); fluorescence intensity is proportional to concentration (at low concentrations, A < 0.1); quantum yield measurement requires reference standard; cooled detector is essential for weak fluorescence (low concentration, low quantum yield) and long integration; avoid inner filter effect (absorption of excitation or emission light by sample - keep absorbance < 0.1 at excitation wavelength; use front-face for concentrated samples); avoid photobleaching (use lower excitation power or shorter integration; some fluorophores degrade under intense light)). Raman (measure inelastic scattering of monochromatic light (laser); requires laser (532 nm, 633 nm, 785 nm, 1064 nm - wavelength selection depends on sample fluorescence and absorption), laser filter (block laser line), sample holder/probe, and spectrometer (the cooled spectrometer); Raman shift (cm-1) = (1/lambda_laser - 1/lambda_scattered) * 10^7; Raman spectrum provides molecular fingerprint (vibrational modes); Raman scattering is very weak (1 in 10^6-10^8 photons) - cooled detector is essential for reasonable integration times; fluorescence interference is a major problem (fluorescence is much stronger than Raman and can swamp Raman signal - use longer wavelength laser (785 nm, 1064 nm) to reduce fluorescence, or use fluorescence quenching, or use shifted excitation Raman difference spectroscopy (SERDS), or use surface-enhanced Raman (SERS) for sensitivity; 532 nm gives strong Raman but high fluorescence; 785 nm is most common for general use (good balance of Raman intensity and low fluorescence); 1064 nm has lowest fluorescence but requires InGaAs detector (lower sensitivity) and Nd:YAG laser; sample damage from laser heating (use appropriate laser power, especially for dark samples and polymers; monitor for sample degradation (spectral changes, burning); use lower power or defocus beam for sensitive samples); Raman is non-destructive and requires minimal sample preparation (can measure through transparent packaging (glass, plastic) - useful for pharmaceutical and forensic applications). Photoluminescence (PL) (similar to fluorescence but for semiconductors and materials (not dyes); measure light emitted after optical or electrical excitation; requires excitation laser/light source and spectrometer; PL peak wavelength and intensity provide information about bandgap, defects, quantum yield, carrier dynamics; cooled detector for weak PL (low quantum yield materials, low temperature PL); temperature-dependent PL (requires cryostat - PL changes with temperature; cooled spectrometer paired with cryostat for low-temperature PL). IMPORTANT: Detector cooling is the key feature that distinguishes this from uncooled spectrometers. The cooling reduces dark current (thermal noise in the detector) by approximately half for every 7-10 degrees C of cooling (e.g., cooling from 25 to -25 degrees C (50 degrees C cooling) reduces dark current by ~2^5 = 32x; cooling to -70 degrees C reduces by ~2^9.5 = ~700x). This enables long integration times (seconds to minutes) without dark noise overwhelming the signal, which is essential for weak light signals (fluorescence, Raman, PL, chemiluminescence, low-transmission absorption). Without cooling, long integration causes dark noise to accumulate, reducing SNR. The cooled spectrometer should be operated with proper cooling: allow warm-up/cool-down time (5-15 minutes for detector to reach set temperature and stabilize), maintain stable ambient temperature (cooling system has limited heat dissipation capacity - if ambient is too hot (>30 degrees C), detector may not reach set temperature or may be unstable; ensure cooling fan is unobstructed), for deep cooling (< -40 degrees C), use dry air/nitrogen purge (to prevent moisture condensation on cold detector and optics - condensation causes permanent damage (water spots on detector, corrosion); verify purge flow rate per manufacturer; use dry air (dew point < -40 degrees C) or nitrogen), do not turn off cooling abruptly (if detector is cold and power is cut, condensation can form as detector warms - maintain purge until detector returns to room temperature; follow manufacturer shutdown procedure). The spectrometer should be stored properly when not in use (store in dry environment with desiccant; if stored for extended period, run periodically to prevent moisture buildup; keep dust caps on fiber connectors to prevent contamination). Waste (used lamps (may contain mercury - hazardous waste, do not throw in regular trash; dispose per hazardous waste regulations), optical fibers (may contain UV-solarized material - generally non-hazardous), cleaning solvents (isopropanol - flammable, dispose per chemical waste regulations), packaging) should be disposed of per applicable regulations (mercury-containing lamps are universal waste/hazardous waste - follow local regulations for disposal and recycling).