OH Absorption Research Articles

Effects of xanthan gum and HPMC on physicochemical and microstructure properties of sponge cakes during storage.

The effects of xanthan gum (XG) and hydroxypropyl methylcellulose (HPMC) in sponge cakes were studied. Hydrocolloids enhanced the thickening effect in batter that affected the textural attributes of sponge cakes. During storage, the structural changes in XG-cake resulted in higher hardness compared to HPMC-cake. Similar to XG, HPMC also contributed moistness to cake. The moisture loss of cake containing XG was slower than HPMC-cake. FTIR study showed absorption of OH at region of 3600-2900cm-1 that explained the strong interaction of water in cake containing XG compared to other cake formulations.

A survey for OH masers in H2O maser galaxies with the Effelsberg and Green Bank radio telescopes

AbstractWe present a search for OH maser emission in galaxies hosting H2O masers with the 100-m Effelsberg radio telescope and the Green Bank Telescope (GBT). This survey is aimed at investigating the apparent rarity and/or possible mutual exclusion of megamaser emission from OH and H2O in the same galaxy. Our study establishes new and better upper limits on the OH maser luminosity. Our work duplicates the number of H2O masers searched for OH emission. No new maser detections have been found. OH absorption, both in the 1667 and 1665 MHz transitions, is instead detected in two galaxies of the sample, IC342 and NGG5793.

Real-Time and Label-Free Chemical Sensor-on-a-chip using Monolithic Si-on-BaTiO3 Mid-Infrared waveguides

Chip-scale chemical detection is demonstrated by using mid-Infrared (mid-IR) photonic circuits consisting of amorphous silicon (a-Si) waveguides on an epitaxial barium titanate (BaTiO3, BTO) thin film. The highly c-axis oriented BTO film was grown by the pulsed laser deposition (PLD) method and it exhibits a broad transparent window from λ = 2.5 μm up to 7 μm. The waveguide structure was fabricated by the complementary metal–oxide–semiconductor (CMOS) process and a sharp fundamental waveguide mode has been observed. By scanning the spectrum within the characteristic absorption regime, our mid-IR waveguide successfully perform label-free monitoring of various organic solvents. The real-time heptane detection is accomplished by measuring the intensity attenuation at λ = 3.0–3.2 μm, which is associated with -CH absorption. While for methanol detection, we track the -OH absorption at λ = 2.8–2.9 μm. Our monolithic Si-on-BTO waveguides establish a new sensor platform that enables integrated photonic device for label-free chemical detection.

Towards a three-dimensional distribution of the molecular clouds in the Galactic Centre

We present a study of the three-dimensional structure of the molecular clouds in the Galactic Centre (GC) using CO emission and OH absorption lines. Two CO isotopologue lines, $^{12}$CO ($J$=1$\rightarrow$0) and $^{13}$CO ($J$=1$\rightarrow$0), and four OH ground-state transitions, surveyed by the Southern Parkes Large-Area Survey in Hydroxyl (SPLASH), contribute to this study. We develop a novel method to calculate the OH column density, excitation temperature, and optical depth precisely using all four OH lines, and we employ it to derive a three-dimensional model for the distribution of molecular clouds in the GC for six slices in Galactic latitude. The angular resolution of the data is 15.5 arcmin, which at the distance of the GC (8.34 kpc) is equivalent to 38 pc. We find that the total mass of OH in the GC is in the range 2400-5100 Solar mass . The face-on view at a Galactic latitude of b = 0{\deg} displays a bar-like structure with an inclination angle of 67.5 $\pm$ 2.1{\deg} with respect to the line of sight. No ring-like structure in the GC is evident in our data, likely due to the low spatial resolution of the CO and OH maps.

Plasma generated during underwater pulsed laser processing

The plasma induced during underwater pulsed laser ablation of graphite is studied both experimentally and theoretically. The results of the experiment show that the maximum plasma temperature of 25000K is reached 20ns from the beginning of the laser pulse and decreases to 6500K after 1000ns. The observed OH absorption band shows that the plasma plume is surrounded by the thin layer of dissociated water vapour at a temperature around 5500K.The hydrodynamic model applied shows similar maximum plasma temperature at delay times between 14ns and 30ns. The calculations show also that already at 14th ns, the plasma electron density reaches 0.97·1027m−3, which is the critical density for 1064nm radiation. At the same time the plasma pressure is 2GPa, which is consisted with earlier measurements of the peak pressure exerted on a target in similar conditions.

Determination of the Rate Coefficients of the CH4 + O2 → HO2 + CH3 and HCO + O2 → HO2 + CO Reactions at High Temperatures

Rate coefficients of the title reactions, R1 (CH4 + O2 → HO2 + CH3) and R2 (HCO + O2 → HO2 + CO) were obtained over T = 1610 ~ 1810 K and T = 200 ~ 1760 K, respectively, and at ρ = 7.1 µmol/cm3. A lean CH4/O2/Ar mixture (0.1% CH4, ϕ = 0.02) was heated behind reflected shock waves and the temporal OH absorption profiles were measured using a laser absorption spectroscopy. Reaction rate coefficients were elucidated by matching the experimental profiles via optimization of k1 and k2 values in the reaction simulation. The rate coefficient expressions derived are k1 = 1.46 × 1014 exp (−26 210 K/T) cm3/mol/s, T = 1610 ~ 1810 K and k2 = 1.9 × 1012 T0.176 exp (−245 K/T) cm3/mol/s, T = 200 ~ 1760 K.

Effects of salts on phosphorus adsorption in alkalize Tunisian soil

Many previous studies have been conducted in an attempt to determine phosphorus (P) adsorption in soil. Often, these studies cannot be compared, because the reports did not give a satisfactory characterization of the dynamics of soil P in saline conditions. In our experiment, three salts extracts (CaCl2, NaCl and KCl) with the same concentration (0.01 M) were used to determine the amount of P adsorption in Solonetz soil samples of the semi-arid areas of Kondar region (Tunisia). Also, we focused on the influence of contact time on P-Salts adsorption in the alkalize soil. The analytic data were approached from the following kinetics’ models: pseudo first order, pseudo second order and Elovich model. Results obtained showed that salts addition increased significantly the amount of P adsorption with the following order of salts extracts (P–CaCl2 > P–NaCl > P–KCl > P). The mechanism of phosphate ions adsorption by soil was studied using IR spectroscopy. Infrared spectral characteristics of the amorphous material indicated that the adsorption is due to exchange phenomena of phosphate ions with surface groups. It was also demonstrated that the addition of CaCl2 salt caused a shift and an increase of OH, Si–O (Si–O–Si, Si–O–Al) and Al–OH absorption bands which favored the adsorption of P ions. Moreover, the second-order model was shown to be the best fit for describing phosphorus adsorption associated with different salts, as seen from the correlation coefficient R2 which ranged from 0.98 to 0.99.

Inflowing gas onto a compact obscured nucleus in Arp 299A

Aims. We probe the physical conditions in the core of Arp 299A and try to put constraints on the nature of its nuclear power source. Methods. We used Herschel Space Observatory far-infrared and submillimeter observations of H2O and OH rotational lines in Arp 299A to create a multi-component model of the galaxy. In doing this, we employed a spherically symmetric radiative transfer code. Results. Nine H2O lines in absorption and eight in emission, as well as four OH doublets in absorption and one in emission, are detected in Arp 299A. No lines of the 18O isotopologues, which have been seen in compact obscured nuclei of other galaxies, are detected. The absorption in the ground state OH 2?3/2-2?3/2(5/2)+-(3/2)-?3/22-2?3/2 52+-32-doublet at 119 ?m is found redshifted by ? 175 km s-1 compared with other OH and H2O lines, suggesting a low excitation inflow. We find that at least two components are required in order to account for the excited molecular line spectrum. The inner component has a radius of 20-25 pc, a very high infrared surface brightness (3 × 1013L·kpc-2), warm dust (Td > 90 K), and a large H2 column density (NH2 > 1024 cm-2). The modeling also indicates high nuclear H2O (1-5 × 10-6) and OH (0.5-5 × 10-5) abundances relative to H nuclei. The outer component is larger (50-100 pc) with slightly cooler dust (70-90 K) and molecular abundances that are approximately one order of magnitude lower. In addition to the two components that account for the excited OH and H2O lines, we require a much more extended inflowing component to account for the OH 2?3/2-2?3/2(5/2)+-(3/2)- ?3/22-2?3/2 52+-32-doublet at 119 ?m. Conclusions. The Compton-thick nature of the core makes it difficult to determine the nature of the buried power source, but the high surface brightness indicates that it is an active galactic nucleus and/or a dense nuclear starburst. Our results are consistent with a composite source. The high OH/H2O ratio in the nucleus indicates that ion-neutral chemistry induced by X-rays or cosmic-rays is important. Finally we find a lower limit to the 16O/18O ratio of 400 in the nuclear region, possibly indicating that the nuclear starburst is in an early evolutionary stage, or that it is fed through a molecular inflow of, at most, solar metallicity.

Temperature regime and water/hydroxyl behavior in the crater Boguslawsky on the Moon

In this work we examine the lunar crater Boguslawsky as a typical region of the illuminated southern lunar highlands with regard to its temperature regime and the behavior of the depth of the water/hydroxyl-related spectral absorption band near 3µm wavelength. For estimating the surface temperature, we compare two different methods, the first of which is based on raytracing and the simulation of heat diffusion in the upper regolith layer, while the second relies on the thermal equilibrium assumption and uses Moon Mineralogy Mapper (M³) spectral reflectance data for estimating the wavelength-dependent thermal emissivity. A method for taking into account the surface roughness in the estimation of the surface temperature is proposed. Both methods yield consistent results that coincide within a few K. By constructing a map of the maximal surface temperatures and comparing with the volatility temperatures of Hg, S, Na, Mg, and Ca, we determine regions in which these volatile species might form stable deposits. Based on M³ data of the crater Boguslawsky acquired at different times of the lunar day, it is found that the average OH absorption depth is higher in the morning than at midday. In the morning a dependence of the OH absorption depth on the local surface temperature is observed, which is no more apparent at midday. This suggests that water/OH accumulates on the surface during the lunar night and largely disappears during the first half of the lunar day. We furthermore model the time dependence of the OH fraction remaining on the surface after having been exposed to the temporally integrated solar flux. In the morning, the OH absorption depth is not correlated with the remaining fraction of OH-containing species, indicating that the removal of water and/or OH-bearing species is mainly due to thermal evaporation after sunrise. In contrast, at midday the OH absorption depth increases with increasing remaining fraction of OH-containing species, suggesting photolysis by solar photons as the main mechanism for removal of the remaining OH-containing species later in the lunar day.

Characterization of Solid Bitumen from Panandhro Lignite (Western India) Based on FTIR and Pyrolysis GC-MS Study

In this study, FTIR and pyrolysis GC-MS analysis methods are used to characterize the handpicked solid bitumen (viscous residue of hydrocarbon) found as fillings in the lignite of Panandhro field, Gujarat. The FTIR data shows that solid bitumen is marked by intense aliphatic CHx stretching peaks between 3000 and 2800 cm -1 , medium absorption of OH stretching, aromatic C=C, and aliphatic deformation peaks. A factor versus C factor plot indicates that it is mainly composed of type-II kerogen (organic matter). The pyrolysis GC-MS data shows the highly aliphatic nature of the solid bitumen. The overall characteristics indicate that the studied solid bitumen is of pre-oil generation type and formed from increase in thermal maturity of lignites.

Illuminating the past 8 billion years of cold gas towards two gravitationally lensed quasars

Using the Boolardy Engineering Test Array of the Australian Square Kilometre Array Pathfinder (ASKAP BETA), we have carried out the first $z = 0 - 1$ survey for HI and OH absorption towards the gravitationally lensed quasars PKSB1830$-$211 and MGJ0414$+$0534. Although we detected all previously reported intervening systems towards PKSB1830$-$211, in the case of MGJ0414+0534 three systems were not found, indicating that the original identifications may have been confused with radio frequency interference. Given the sensitivity of our data, we find that our detection yield is consistent with the expected frequency of intervening HI systems estimated from previous surveys for 21-cm emission in nearby galaxies and $z \sim 3$ damped Lyman $\alpha$ absorbers. We find spectral variability in the $z = 0.886$ face-on spiral galaxy towards PKSB1830$-$211, from observations undertaken with the Westerbork Synthesis Radio Telescope in 1997/1998 and ASKAP BETA in 2014/2015. The HI equivalent width varies by a few per cent over approximately yearly time-scales. This long-term spectral variability is correlated between the north-east and south-west images of the core, and with the total flux density of the source, implying that it is observationally coupled to intrinsic changes in the quasar. The absence of any detectable variability in the ratio of HI associated with the two core images is in stark contrast to the behaviour previously seen in the molecular lines. We therefore infer that coherent opaque HI structures in this galaxy are larger than the parsec-scale molecular clouds found at mm-wavelengths.

Water incorporation in garnets from ultrahigh pressure eclogites at Shuanghe, Dabieshan

AbstractThe hydrogen concentration and composition of garnets in the ultrahigh pressure eclogites at Shuanghe, eastern Dabieshan, were investigated using Fourier transform infrared spectroscopy and electron microprobe analysis. The OH absorption bands can be divided into four groups: (1) 3635–3655 cm–1; (2) 3600–3630 cm–1; (3) 3540–3580 cm–1; and (4) 3400–3450 cm–1 and the water content ranges from 45 to 2529 ppm. Based on the behaviour of the OH absorption band and the relationship between water content and the composition of garnets, the samples can be divided into two classes: samples with >400 ppm H2O and samples with ≤400 ppm H2O. The water content of the former shows an obvious positive correlation with Ca atoms and a negative correlation with the Si, Mg and Fe2+ atoms per 12 anions, whereas the water content of the latter shows no obvious linear correlation with cations. It is concluded that the major mechanism of hydroxyl incorporation in garnets with >400 ppm H2O is by the coupled substitution 4H +Z□ → □+ZSi in the tetrahedral site, and that several mechanisms are responsible for OH incorporation in garnets with ≤400 ppm H2O.

An empirical thermal correction model for Moon Mineralogy Mapper data constrained by laboratory spectra and Diviner temperatures

AbstractRadiance measured by the Moon Mineralogy Mapper (M3) at wavelengths beyond ~2 µm commonly includes both solar reflected and thermally emitted contributions from the lunar surface. Insufficient correction (removal) of the thermal contribution can modify and even mask absorptions at these wavelengths in derived surface reflectance spectra, an effect that precludes accurate identification and analysis of OH and/or H2O absorptions. This study characterized thermal effects in M3 data by evaluating surface temperatures measured independently by the Lunar Reconnaissance Orbiter Diviner radiometer, and results confirm that M3 data (Level 2) currently available in the Planetary Data System often contain significant thermal contributions. It is impractical to use independent Diviner measurements to correct all M3 images for the Moon because not every M3 pixel has a corresponding Diviner measurement acquired at the same local time of lunar day. Therefore, a new empirical model, constrained by Diviner data, has been developed based on the correlation of reflectance at 1.55 µm and at 2.54 µm observed in laboratory reflectance spectra of Apollo and Luna soil and glass‐rich samples. Reflectance values at these wavelengths follow a clear power law, , for a wide range of lunar sample compositions and maturity. A nearly identical power law is observed in M3 reflectance data that have been independently corrected by using Diviner‐based temperatures, confirming that this is a general reflectance property of materials that typify the lunar surface. These results demonstrate that reflectance at a thermally affected wavelength (2.54 µm) can be predicted within 2% (absolute) based on reflectance values at shorter wavelengths where thermal contributions are negligible and reflectance is dominant. Radiance at 2.54 µm that is in excess of the expected amount is assumed to be due to thermal emission and is removed during conversion of at‐sensor radiance to reflectance or I/F. Removal of this thermal contribution by using this empirically based model provides a more accurate view of surface reflectance properties at wavelengths >2 µm, with the benefit that it does not require independent measurements or modeling of surface temperatures at the same local time as M3 data were acquired. It is demonstrated that this model is appropriate for common lunar surface compositions (e.g., mare and highlands soils and pyroclastic deposits), but surface compositions with reflectance properties that deviate strongly from these cases (e.g., pyroxene‐, olivine‐, or spinel‐rich locations with minimal space weathering) may require the use of more sophisticated thermal correction models or overlapping Diviner temperature estimates.

Revisiting the cation mass-valence sum approach to assigning infrared OH-bands in dioctahedral smectites in the light of new data from synthetic Ga-Fe3+ smectites

A series of pure Ga-Fe3+ smectites were synthesized at 180°C in order to complete IR data in the Al-Ga-Fe3+ system. MIR and NIR data from natural and synthetic smectites in the Al-Fe3+, Al-Ga and Fe3+-Ga chemical series exemplified a case where some ν OH, δ OH and (ν+δ) OH band positions did not follow the relation: ν OH (cm−1)=(1/2π c)*(kOH/μOH)1/2. This relation is often used to approximate the position of the OH vibration bands from the reduced masses of octahedral cations linked to hydroxyls in clay minerals. In this study, better relations were established between the wavenumbers of the OH absorption band of smectites and the average ionic radius of neighboring octahedral cations. Similar trends were established previously for M-(OH)2 hydroxides (G.W. Brindley, C. Kao, Phys. Chem. Miner. 10 (1984) 187-191) suggesting a possible generalization of a link between OH frequencies in IR spectra and the average ionic radii of neighboring octahedral cations for hydroxylated minerals.

Hyperspectral interpretation of selected drill cores from orogenic gold deposits in central Victoria, Australia

ABSTRACTHyLogger hyperspectral data obtained from seven orogenic gold deposits in central Victoria, including Bendigo, Ballarat, Maldon, Fosterville, Costerfield, Castlemaine and Wildwood, are presented. The data demonstrate that fresh diamond drill core displays substantial mineralogical variation that can be attributed to the effects of cryptic hydrothermal alteration that might not otherwise be recognised. The most significant hyperspectral response lies in the white mica compositions, which vary in a systematic manner between high-Al muscovitic zones (Al–OH absorption around 2208 nm) that define a phyllic alteration halo around mineralised structures, and low-Al phengitic–chlorite zones (Al–OH absorption >2014 nm) inferred to represent either more distal alteration or possibly regional metamorphic background. An extensive ferroan dolomite alteration halo overlaps the phyllic and sulfidic alteration zones and extends beyond the sampled core in most instances. This ferroan dolomite halo has previously been defined petrographically, geochemically and using carbonate staining techniques, and is further characterised using thermal infrared hyperspectral data in drill core from the Ballarat goldfield. The mineralogical trends identified by the hyperspectral data are best developed in diamond drill core from the Costerfield, Fosterville and Ballarat goldfields, and are less pronounced at the other deposits. At Bendigo and Castlemaine the reasons for this are not immediately clear, but may be related to the close timing of gold mineralisation relative to peak metamorphism. The Maldon area lies within the contact aureole of the Harcourt Batholith and so has been thermally overprinted leading to the recrystallisation of earlier hydrothermal assemblages. The Wildwood deposit is similar to the Magdala deposit at Stawell and differs from the other goldfields in its geological setting, host rock lithologies and style of hydrothermal alteration, with the development of Fe-rich chlorite closely associated with gold mineralisation. The results demonstrate how hyperspectral data can be used to define large hydrothermal alteration footprints associated with orogenic gold mineralisation in central Victoria that are of direct benefit to mineral explorers, as well as independently characterising lithological variations in drill core.

Temperature-dependent VNIR spectroscopy of hydrated Mg-sulfates

We investigate two poly-hydrated magnesium sulfates, hexahydrite (MgSO4 · 6H2O) and epsomite (MgSO4 · 7H2O), in the visible and infrared (VNIR) spectral range 0.5/4.0µm, as particulate for three different grain size ranges: 20–50µm, 75–100µm and 125–150µm. All samples were measured in the 93–298K temperature range. The spectra of these hydrated salts are characterized by strong OH absorption bands in the 1.0–1.5µm region, and by H2O absorption bands near 2 and 3µm. Other weak features show up at low temperatures near 1.75µm (in both hexahydrite and epsomite) and 2.2µm (only in hexahydrite). The spectral behavior of the absorption bands of these two minerals has been analyzed as a function of both grain size and temperature, deriving trends related to specific spectral parameters such as band center, band depth, band area, and band width. Hydrated minerals, in particular mono- and poly-hydrated sulfates, are present in planetary objects such as Mars and the icy Galilean satellites. Safe detection of these minerals shall rely on detailed laboratory investigation of these materials in different environmental conditions. Hence an accurate spectral analysis of such minerals as a function of temperature is key to better understand and constrain future observations.

THE SEARCH FOR MOLECULAR OUTFLOWS IN LOCAL VOLUME AGNs WITH HERSCHEL-PACS*

ABSTRACT We present the results from a systematic search for galactic-scale, molecular (OH 119 μm) outflows in a sample of 52 Local Volume ( Mpc) Burst Alert Telescope detected active galactic nuclei (BAT AGNs) with Herschel-PACS. We combine the results from our analysis of the BAT AGNs with the published Herschel/PACS data of 43 nearby ( ) galaxy mergers, mostly ultra-luminous infrared galaxies (ULIRGs) and QSOs. The objects in our sample of BAT AGNs have, on average, times lower AGN luminosities, star formation rates, and stellar masses than those of the ULIRG and QSO samples. OH 119 μm is detected in 42 of our BAT AGN targets. Evidence for molecular outflows (i.e., OH absorption profiles with median velocities more blueshifted than −50 km s−1 and/or blueshifted wings with 84% velocities less than −300 km s−1) is seen in only four BAT AGNs (NGC 7479 is the most convincing case). Evidence for molecular inflows (i.e., OH absorption profiles with median velocities more redshifted than 50 km s−1) is seen in seven objects, although an inverted P-Cygni profile is detected unambiguously in only one object (Circinus). Our data show that both the starburst and AGN contribute to driving OH outflows, but the fastest OH winds require AGNs with quasar-like luminosities. We also confirm that the total absorption strength of OH 119 μm is a good proxy for dust optical depth as it correlates strongly with the 9.7 μm silicate absorption feature, a measure of obscuration originating in both the nuclear torus and host galaxy disk.

Experimental long-term survey of mid-infrared supercontinuum source based on As2S3 suspended-core fibers

The evolution of supercontinuum generation in chalcogenide suspended-core microstructured optical fibers is studied with regard to their exposure to the room atmosphere. We report the experimental proof of aging-induced supercontinuum generation drift in chalcogenide microstructured fibers. Mid-infrared supercontinuum covering the 2.5–5.5-µm spectral region is demonstrated in a fresh and 7-month-aged counterpart As2S3 fibers, by means of a home-built multistage oscillator power amplifier delivering 300 fs pulses at a repetition rate of 43 MHz in the 3.0–4.1-µm range. Numerical simulations based on the generalized nonlinear Schrodinger equation confirm the significant alteration of supercontinuum generation due to increasing fundamental OH and SH absorption bands.

BROAD [C II] LINE WINGS AS TRACER OF MOLECULAR AND MULTI-PHASE OUTFLOWS IN INFRARED BRIGHT GALAXIES

ABSTRACT We report a tentative correlation between the outflow characteristics derived from OH absorption at 119 μm and [C ii] emission at 158 μm in a sample of 22 local and bright ultraluminous infrared galaxies (ULIRGs). For this sample, we investigate whether [C ii] broad wings are a good tracer of molecular outflows, and how the two tracers are connected. Fourteen objects in our sample have a broad wing component as traced by [C ii], and all of these also show OH119 absorption indicative of an outflow (in one case an inflow). The other eight cases, where no broad [C ii] component was found, are predominantly objects with no OH outflow or a low-velocity (≤100 km s−1) OH outflow. The FWHM of the broad [C ii] component shows a trend with the OH119 blueshifted velocity, although with significant scatter. Moreover, and despite large uncertainties, the outflow masses derived from OH and broad [C ii] show a 1:1 relation. The main conclusion is therefore that broad [C ii] wings can be used to trace molecular outflows. This may be particularly relevant at high redshift, where the usual tracers of molecular gas (like low-J CO lines) become hard to observe. Additionally, observations of blueshifted Na i D λλ 5890, 5896 absorption are available for 10 of our sources. Outflow velocities of Na i D show a trend with OH velocity and broad [C ii] FWHM. These observations suggest that the atomic and molecular gas phases of the outflow are connected.

Synthesis of Waste Cooking Oil-Based Polyol Using Sugarcane Bagasse Activated Carbon and Transesterification Reaction for Rigid Polyurethane Foam

This study was carried out to determine the potential of waste cooking oil (WCO) in preparation of rigid polyurethane (PU) foam. The raw WCO was first filtered and adsorbed by using sugarcane bagasse activated carbon in order to purify the oil. Next, the adsorbed WCO was used to synthesize polyol via transesterification reaction. The WCO-based polyol was then combined with other chemicals at various ratios to form PU rigid foam. The adsorbed WCO showed the decrease in both free fatty acid percentage and viscosity, from 4.3 % to 0.77 % and from 106 mPa.s to 72.5 mPa.s, respectively. No alteration of functional group observed after adsorption as proven by FTIR spectroscopy. The FTIR spectrum of WCO-based polyol showed the formation of OH absorption peak and supported by the increase in hydroxyl value from 0 to 148.79 mgKOH/g after reaction. The formation of urethane linkages (NHCO) backbone in PU foam was confirmed using FTIR. The properties of PU foam are highly dependent on the chemical composition. The density and compressive strength of 60:54:90:40 of glycerol:water:polyol:amine polyurethane foam are 277.7 kg/m3 and 0.10 MPa, respectively. This study showed that WCO exhibit promising potential as raw material for PU formation.