Evaluation of acoustic rhinometry in a nasal provocation test with allergen

BACKGROUND: The objective was to validate acoustic rhinometry (AR) in a nasal challenge with allergen. METHODS: Nasal response to allergen provocation was based on clinical and symptom scores, cross-sectional changes of the nasal mucosa as measured by AR with the Rhinoklack system, and peak nasal inspiratory flow (PNIF), in atopic and nonatopic volunteers. RESULTS: After allergen challenge, mean variation in minimal cross-sectional area (deltaMCA), as measured by AR, or in peak nasal inspiratory flow (deltaPNIF) in nonatopic volunteers, was -0.4+/-14.3% and 5.2+/-15.7%, respectively, compared to baseline. This allowed the determination of a reaction threshold of -29% for deltaMCA and of -26% for deltaPNIF. All but one of the 30 atopic patients reached the AR reaction threshold, whereas all patients reached the PNIF reaction threshold. AR and PNIF closely correlated with clinical and symptom scores for nasal congestion, since there was no significant difference at reaction threshold between both methods. CONCLUSIONS: In an allergen provocation test, AR appears to be as specific and sensitive as peak nasal inspiratory flow, with the advantage of being independent of the patient's active cooperation. Discrepancies between both methods emphasize the role of nasal cavity anatomy in measuring nasal congestion by AR

Acoustic rhinometry in nasal allergen challenge study: Which dimensional measures are meaningful?

10.1111/j.1365-2222.2004.01988.xClinical and Experimental Allergy3471093-1098CLEA

Guided Wave Testing

Guided waves can propagate long distances in thin-walled structures, such as pipelines or plates. This allows for the efficient monitoring and testing of large structures and for the detection of hidden or inaccessible defects. Guided wave propagation is dispersive and multi-modal, requiring a thorough understanding of the wave propagation and scattering phenomena from simulations. Guided wave dispersion diagrams, mode shapes, and typical signals are illustrated for the example of isotropic plates. Both low and high frequency guided waves have been used for the testing of plate structures, with different wave modes and applications including tomography and arrays for the detection and localization of defects. For multilayered and anisotropic structures, guided wave propagation becomes more complex, and often the fundamental guided wave modes are employed for defect detection. For pipelines different commercially available testing systems have been developed and long propagation distances up to 100 m have been achieved. Careful selection of guided wave mode and excitation frequency allows the minimization of attenuation due to viscoelastic coatings and in buried pipelines. Synthetic focusing using non-axisymmetric modes improves defect imaging and localization. Experimental methods differ from standard ultrasonic testing, as good control of the excited guided wave mode shape and signal are required to achieve improved sensitivity for small defects. In addition to contact piezoelectric transducers, electromagnetic and laser techniques allow for noncontact measurements. Finite Element Analysis is one of the numerical simulation techniques used to obtain a better understanding of guided wave testing and to improve defect characterization

The Tenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-III Apache Point Observatory Galactic Evolution Experiment

The Sloan Digital Sky Survey (SDSS) has been in operation since 2000 April. This paper presents the Tenth Public Data Release (DR10) from its current incarnation, SDSS-III. This data release includes the first spectroscopic data from the Apache Point Observatory Galaxy Evolution Experiment (APOGEE), along with spectroscopic data from the Baryon Oscillation Spectroscopic Survey (BOSS) taken through 2012 July. The APOGEE instrument is a near-infrared R similar to 22,500 300 fiber spectrograph covering 1.514-1.696 mu m. The APOGEE survey is studying the chemical abundances and radial velocities of roughly 100,000 red giant star candidates in the bulge, bar, disk, and halo of the Milky Way. DR10 includes 178,397 spectra of 57,454 stars, each typically observed three or more times, from APOGEE. Derived quantities from these spectra (radial velocities, effective temperatures, surface gravities, and metallicities) are also included. DR10 also roughly doubles the number of BOSS spectra over those included in the Ninth Data Release. DR10 includes a total of 1,507,954 BOSS spectra comprising 927,844 galaxy spectra, 182,009 quasar spectra, and 159,327 stellar spectra selected over 6373.2 deg(-2)