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Background C-itra is the drug of choice for treatment of most non-CNS, non-life-threatening forms of endemic mycoses (EM), including histoplasmosis, blastomycosis, coccidioidomycosis, sporotrichosis and talaromycosis. SUBA represents a new formulation of itraconazole that utilizes nanotechnology to improve bioavailability when administered orally. SUBA is formulated as nanoparticles allowing for absorption in the small bowel while not relying on gastric acidity for optimal absorption. MSG-15 is an open-label, comparative clinical trial comparing SUBA to c-itra for the treatment of EM. Herein we report the final PK and AE profiles of these two compounds. Methods Subjects with proven and probable EM were eligible this open-label comparative study. The protocol allowed up to 14 d of prior therapy with any antifungal for this episode of EM. Subjects were randomized to receive either SUBA 130 mg po bid or c-itra 200 mg po bid for up to 6 months. Follow up occurred at 7, 14, 28, 42, 84 and 180 d post-enrollment. PK samples were obtained at 7, 14, and 42 d. Clinical assessment, including symptom assessment, AEs, overall drug tolerance, and quality of life were assessed at each visit. We used descriptive statistics for this analysis. Results 89 subjects with EM entered the trial, including 43 on SUBA and 46 on c-itra. We measured PK serum levels of itra and hydroxyl-itra at days 7, 14, and 42 and these data are depicted in Figures 1-3. There were no significant differences in these levels, including combined itra/hydroxyl-itra levels, among the two study arms. AUC for itra and hydroxyl-itra were similar for both arms. AEs as assessed at each study evaluation were also quite similar among the two study arms. Overall, any AE occurred in 74% vs 85% of SUBA and c-itra recipients, respectively (NS). Drug-related AEs occurred in 35% vs 41% of SUBA and itra recipients, respectively (NS). Most common drug-related AEs included cardiovascular (edema and hypertension), nausea and loss of appetite. Combined Itraconazole and Hydroxy-itraconazole Concentration Over Time Conclusion Compared to c-itra, SUBA demonstrates almost identical serum levels despite being dosed at roughly 60% standard dosing for c-itra (130 mg po bid vs 200 mg po bid). SUBA is slightly better tolerated than c-itra, although the specific AEs are similar. Disclosures Peter G. Pappas, MD, Astellas (Research Grant or Support)Cidara (Research Grant or Support)F2G (Consultant)Matinas (Consultant, Scientific Research Study Investigator)Mayne Pharma (Research Grant or Support)Scynexis (Research Grant or Support) Andrej Spec, MD, MSCI, Mayne Pharma (Grant/Research Support) Marisa Miceli, MD, SCYNEXIS, Inc. (Advisor or Review Panel member) George R. R. Thompson III, III, MD, Amplyx (Consultant, Grant/Research Support)Appili (Consultant)Astellas (Consultant, Grant/Research Support)Avir (Grant/Research Support)Cidara (Consultant, Grant/Research Support)F2G (Consultant, Grant/Research Support)Mayne (Consultant, Grant/Research Support)Merck (Scientific Research Study Investigator)Pfizer (Advisor or Review Panel member)

Using the CHARA Array and the Palomar Testbed Interferometer, the chemically peculiar star $\lambda$ Bo\"{o}tis has been spatially resolved. We have measured the limb darkened angular diameter to be $\theta_{LD} = 0.533\pm0.029$ mas, corresponding to a linear radius of $R_{\star} = 1.70 \pm 0.10 R_\odot$. The measured angular diameter yields an effective temperature for $\lambda$ Boo of $T_{eff} = 8887 \pm 242$ K. Based upon literature surface gravity estimates spanning $\log{(g)} = 4.0-4.2$ $[\rm{cm s}^{-\rm{2}}]$, we have derived a stellar mass range of $M_{\star} = 1.1 - 1.7$ $M_\odot$. For a given surface gravity, the linear radius uncertainty contributes approximately $\sigma(M_\star) = 0.1-0.2 M_\odot$ to the total mass uncertainty. The uncertainty in the mass (i.e., the range of derived masses) is primarily a result of the uncertainty in the surface gravity. The upper bound of our derived mass range ($\log(g)=4.2, M_\star = 1.7\pm0.2 M_\odot$) is consistent with 100-300 MYr solar-metallicity evolutionary models. The mid-range of our derived masses ($\log(g)=4.1, M_\star = 1.3\pm0.2 M_\odot$) is consistent with 2-3 GYr metal-poor evolutionary models. A more definitive surface gravity determination is required to determine a more precise mass for $\lambda$ Boo.

We report on the development of two new mechanically rugged, high light yield transparent ceramic scintillators: (1) Ce-doped Gd-garnet for gamma spectroscopy, and (2) Eu-doped Gd-Lu-bixbyite for radiography. GYGAG(Ce) garnet transparent ceramics offer ρ = 5.8g/cm3, Zeff = 48, principal decay of 8 lp/mm.

We present infrared interferometric angular size measurements for rapidly rotating stars which indicate non-circular projected disk brightness distributions. For the A7IV-V star Altair, assuming that the apparent oblateness of the photosphere is due to the star's rapid rotation, a rigorous evaluation of the observation data in the context of a rigidly rotating Roche model shows that an estimate of v sin i = 210 ± 13 km s–1 can be derived that is independent of spectroscopic techniques. Altair is the first main sequence star for which direct observations of an oblate photosphere have been reported, and the first star for which v sin i has been established from observations of the star's photospheric geometry. Future prospects for this technique are considered, and a prospective catalog of 67 rotationally oblate targets is presented.

Milliarcsecond resolution observations of cool stars are becoming increasingly common and sophisticated as recent advances in telescope technology mature. To varying degrees, these observations rely up on stellar models for interpretation of their data, while at the same time present particular challenges to those models. Indications of departures from spherical symmetry are beginning to be observed as increasingly rich image information is obtained by a new generation of interferometers. Examination the subtle variations of wavelength-specific sizes exhibits rich structure, connected to the atmospheric chemistry. For the pulsating stars, such as Mira variables, that structure varies with time, with the phase lags between the various sizes being connected to the atmospheric dynamics. Complex morphologies associated with atmospheric winds have been revealed with these high resolution experiments. A review of these recent results will be presented, concentrated on their implications upon stellar modelling, and the prospects for future observational data.

As part of the long-term monitoring of Mira variables at the Palomar Testbed Interferometer, we report high-resolution narrowband angular sizes of the oxygen-rich Mira S Lac and the carbon-rich Mira RZ Peg in the near-infrared. The data set spans three pulsation cycles for S Lac and two pulsation cycles for RZ Peg (a total of 1070 25 s observations) and represents the first study to correlate multiepoch narrowband interferometric data of Mira variables. When the calibrated visibility data are fitted using a uniform disk brightness model, differences are seen in their angular diameters as a function of wavelength within the K band (2.0-2.4 μm), the source of which is believed to be molecular absorptions in or above the photospheres of the two chemically different Miras. Using visible photometric data provided by the Association Francaise des Observateurs d'Etoiles Variables (AFOEV), the continuum minimum size of RZ Peg lags this by 0.28 ± 0.02 in pulsation, similar to the phase lag found in Correlation Radial Velocities (CORAVEL) data. However, for S Lac, the continuum minimum size tracks the visual maximum brightness. Based on the mean of the continuum angular diameter cycloids, basic stellar parameters are computed for both RZ Peg and S Lac, with both showing maximum atmospheric extension with respect to the 2.0 and 2.4 μm diameters near phase 0.9. Using the mean value of the fitted cycloids, RZ Peg has a radius Rmean = 377 ± 111 R☉ and a mean Teff = 2706 ± 36 K; S Lac has a radius Rmean = 292 ± 73 R☉ and a mean Teff = 2605 ± 47 K. The dominant source of error in the radii is the large uncertainty in the distances to these two stars.

We report high-resolution (

We present infrared interferometric angular size measurements for the A7IV-V star Altair that indicate a noncircular projected disk brightness distribution. Given the known rapid rotation of this star, we model the data as arising from an elongated rigid atmosphere. To first order, an ellipse may be fitted to our interferometric diameter measurements, with major and minor axes of 2a = 3.461 ± 0.038 mas and 2b = 3.037 ± 0.069 mas, respectively, for a difference of 424 ± 79 μas between 2a and 2b, and with an axial ratio of a/b = 1.140 ± 0.029. Assuming that the apparent oblateness of the photosphere is due to the star's rapid rotation, a more rigorous evaluation of the observation data in the context of a rigidly rotating Roche model shows that an estimate of v sin i = 210 ± 13 km s-1 can be derived that is independent of spectroscopic techniques. Also derived are values for the mean effective temperature and the mean linear radius, and an observational constraint upon the relationship between rotation velocity and stellar inclination is established. Altair is the first main-sequence star for which direct observations of an oblate photosphere have been reported and the first star for which v sin i has been established from observations of the star's photospheric geometry.

Interferometrically determined angular diameters obtained at the Palomar Testbed Interferometer (PTI) for 80 giant and supergiant stars are presented in this paper.

The Keck Interferometer (KI) combined the two 10 m W. M. Keck Observatory telescopes on Mauna Kea, Hawaii, as a long-baseline near- and mid-infrared interferometer. Funded by NASA, it operated from 2001 until 2012. KI used adaptive optics on the two Keck telescopes to correct the individual wavefronts, as well as active fringe tracking in all modes for path-length control, including the implementation of cophasing to provide long coherent integration times. KI implemented high sensitivity fringe-visibility measurements at H (1.6 μm), K (2.2 μm), and L (3.8 μm) bands, and nulling measurements at N band (10 μm), which were used to address a broad range of science topics. Supporting these capabilities was an extensive interferometer infrastructure and unique instrumentation, including some additional functionality added as part of the NSF-funded ASTRA program. This paper provides an overview of the instrument architecture and some of the key design and implementation decisions, as well as a description of all of the key elements and their configuration at the end of the project. The objective is to provide a view of KI as an integrated system, and to provide adequate technical detail to assess the implementation. Included is a discussion of the operational aspects of the system, as well as of the achieved system performance. Finally, details on V^2 calibration in the presence of detector nonlinearities as applied in the data pipeline are provided.

Optical interferometry is a technique by which the diameters and indeed the direct pulsations of stars are routinely being measured. As a follow‐on to a 7 year interferometric campaign to measure the pulsations of over 100 mira variables, our team has been using the Spitzer Space Telescope to obtain 95 mid‐infrared spectra of 25 miras during their pulsations over one year while simultaneously ascertaining their near‐infrared diameters using the Palomar Testbed Interferometer. These data will then be combined with modeling from NLTE and radiative transfer codes to place hard constraints on our understanding of these stars and their circumstellar environments. We present some initial results from this work and discuss the next steps toward fully characterizing the atmosphere, molecular photosphere and dust production in mira variables.

The Palomar Testbed Interferometer (PTI) archive of observations between 1998 and 2005 is examined for objects appropriate for calibration of optical long-baseline interferometer observations - stars that are predictably point-like and single. Approximately 1,400 nights of data on 1,800 objects were examined for this investigation. We compare those observations to an intensively studied object that is a suitable calibrator, HD217014, and statistically compare each candidate calibrator to that object by computing both a Mahalanobis distance and a Principal Component Analysis. Our hypothesis is that the frequency distribution of visibility data associated with calibrator stars differs from non-calibrator stars such as binary stars. Spectroscopic binaries resolved by PTI, objects known to be unsuitable for calibrator use, are similarly tested to establish detection limits of this approach. From this investigation, we find more than 350 observed stars suitable for use as calibrators (with an additional $\approx 140$ being rejected), corresponding to $\gtrsim 95%$ sky coverage for PTI. This approach is noteworthy in that it rigorously establishes calibration sources through a traceable, empirical methodology, leveraging the predictions of spectral energy distribution modeling but also verifying it with the rich body of PTI's on-sky observations., Comment: 100 pages, 7 figures, 7 tables; to appear in the May 2008ApJS, v176n1

We have resolved the classical nova V1663 Aql using long-baseline near-IR interferometry covering the period from 5--18 days after peak brightness. We directly measure the shape and size of the fireball, which we find to be asymmetric. In addition we measure an apparent expansion rate of 0.21 +/- 0.03 mas/day. Assuming a linear expansion model we infer a time of initial outburst approximately 4 days prior to peak brightness. When combined with published spectroscopic expansion velocities our angular expansion rate implies a distance of 8.9 +/- 3.6 kpc. This distance measurement is independent of, but consistent with, determinations made using widely available photometric relations for novae., 6 Pages, Accepted for publication in ApJ

During the last two years we have used the Palomar Testbed Interferometer to observe several explosive variable stars, including V838 Monocerotis, V1663 Aquilae and recently RS Ophiuchi. We observed V838 Monocerotis approximately 34 months after its eruption, and were able to resolve the ejecta. Observations of V1663 Aql were obtained starting 9 days after peak brightness and continued for 10 days. We were able to resolve the milliarcsecond-scale emission and follow the expansion of the nova photosphere. When combined with radial-velocity information, these observations can be used to infer the distance to the nova. Finally we have resolved the recurrent nova RS Oph and can draw some preliminary conclusions regarding the emission morphology., 8 Pages, SPIE Astronomical Telescopes and Instrumentation 2006, Advances in Stellar Interferometery, 6268-161

We report observations of the recurrent nova RS Oph using long-baseline near-IR interferometry. We are able to resolve emission from the nova for several weeks after the February 2006 outburst. The near-IR source initially expands to a size of approximately 5 milli-arcseconds. However, beginning around day 10 the IR source appears to begin to shrink, reaching approximately 2 milli-arcseconds by day 100. We combine our measured angular diameters with previously available interferometric and photometric data to derive an emission measure for the source, and hence are able to determine the mass-loss rate of the nova in the days following the outburst., Comment: 17 pages, 4 figures. Accepted for publication in ApJ

We have used long-baseline near-IR interferometry to resolve the peculiar eruptive variable V838 Mon and to provide the first direct measurement of its angular size. Assuming a uniform disk model for the emission we derive an apparent angular diameter at the time of observations (November-December 2004) of $1.83 \pm 0.06$ milli-arcseconds. For a nominal distance of $8\pm2$ kpc, this implies a linear radius of $1570 \pm 400 R_{\odot}$. However, the data are somewhat better fit by elliptical disk or binary component models, and we suggest that the emission may be strongly affected by ejecta from the outburst., 12 pages, 1 two-part encapsulated postscript figure. Accepted by ApJL. Added a table of observations

We report the results of a sensitive K-band survey of Herbig Ae/Be disk sizes using the 85-m baseline Keck Interferometer. Targets were chosen to span the maximum range of stellar properties to probe the disk size dependence on luminosity and effective temperature. For most targets, the measured near-infrared sizes (ranging from 0.2 to 4 AU) support a simple disk model possessing a central optically-thin (dust-free) cavity, ringed by hot dust emitting at the expected sublimation temperatures (T_sub~1000-1500K). Furthermore, we find a tight correlation of disk size with source luminosity R propto L^(1/2) for Ae and late Be systems (valid over more than 2 decades in luminosity), confirming earlier suggestions based on lower-quality data. Interestingly, the inferred dust-free inner cavities of the highest luminosity sources (Herbig B0-B3 stars) are under-sized compared to predictions of the optically-thin cavity model, likely due to optically-thick gas within the inner AU., Accepted by Astrophysical Journal; 24 pages, 4 figures, 4 tables

Fifteen 1.25 inch BSTRA balls were scanned with the high energy computed tomography system at LLNL. This system has a resolution limit of approximately 210 microns. A threshold of 238 microns (two voxels) was used, and no anomalies at or greater than this were observed.

A dedicated program of measuring angular sizes of Mira variables using the Palomar Testbed Interferometer has resulted in more than 13,000 measurements of over 60 stars. With visibility data in five channels across the K band, atmospheric extension and sources of opacity are evident in the dataset. Using multiple-epoch narrow-band data, phase lags between wavelength-dependent angular size cycles indicate spatial extent of molcular atmospheres. A spectral angular diameter classification system is developed, based on the recurring shapes of the spectral traces seen in the dataset, which correlates to spectral type. A period-radius relationship is explored, and a refinement on the estimation of angular sizes is made.

We discuss recent work from the Palomar Testbed Interferometer (PTI), including science results and system improvements. In the past two years PTI has been used to observe a wide range of scientifically interesting sources, including binaries, Cepheids and Miras. In addition PTI has been used to observe departures from spherical symmetry in several stars. Recent system improvements incude a new low read-noise camera based on a HAWAII infrared array, routine opteration in two baselines, and operation in the J band. Future developments include an upgrade to three-aperture combination and closure phase measurements, and double-Fourier interferometry.

Interferometric observations in the atmospheric windows of the near infrared (1 to 4 μm) can be efficiently used to probe the chemical composition of Miras atmosphere and provide direct measurements of extended gas layers around these stars. This is illustrated by recent Miras observations carried out with the FLUOR instrument of the IOTA interferometer (Mennesson et al. 2002, and Perrin et al. proceedings of this conference) and with the PTI test-bed (Thompson 2002, Thompson et al. 2002). These visibility measurements show evidence for continuum emission from very extended (2–3 stellar radii) semi-transparent gaseous atmospheric layers, and large apparent diameter changes with pulsation phase. Interestingly these observations are consistent with the extended molecular gas layers (H 2 O, CO …) already inferred around some of these objects from ISO and high resolution ground-based FTS infrared spectra

To determine if a chemical signal produced by female roughskin newts (Taricha granulosa) stimulates amplectic clasping in males, we recorded behavioral responses by males to scented plastic models of female newts. Female-scented models elicited robust amplectic clasping by male newts, whereas unscented models or models scented with male odors were rarely clasped by males. Models treated with female-scented water elicited clasping responses, but not as effectively as models that were scented by placing them in direct contact with females. Protease or heat treatment did not disrupt the clasp-eliciting activity in female-scented water. These findings provide evidence that a pheromone produced by female roughskin newts acts as a releasing stimulus that elicits a specific, stereotypical courtship response in males, and they suggest that the chemical signal is not proteinaceous.

International audience; Because of an error at the Press, the received date for this paper was incorrectly given as 2004 January 5. The correct received date is 2004 December 5. The Press sincerely regrets this error.

Test runs with a new data processing software system on archival spectra obtained by the International Ultraviolet Explorer (IUE) reveal high-excitation emission lines in the gravitationally lensed binary quasar 0957+561. The lines of O VI λλ1031,1037 and S VI λλ933,945 are readily seen in a single 390 minute, low-dispersion IUE exposure, when calibrated with the New Spectral Image Processing System (NEWSIPS). Coaddition of 10 exposures, as processed by NEWSIPS, followed by the application of a five-point smoothing filter, allows clear detection of the additional emission of C III λ978, N III λ992, S IV λλ1063-1073, N II λ1084, Fe III (UV1; λ1125), and N V λ1238

Feline calicivirus was isolated from eight often cats with chronic stomatitis but not from 10 healthy cats kept under similar conditions. Tests for feline leukaemia viral antigen failed to detect evidence of this infection. The age of affected cats ranged from 1.5 to 11 years with a mean of 5.7 years. Treatment with corticosteroids, megestrol acetate and tooth extraction resulted in clinical improvement but in some cases the condition recurred when treatment was finished.

The clinical findings in a dog with sinoatrial arrest, atrioventricular block and multifocal idioventricular escape beats are described. The clinical findings were associated with a primary myocarditis involving the sinoatrial node, the left and right atrium and atrioventricular node. The differentiation between sinoatrial arrest, sinoatrial block and sinoventricular conduction is discussed.

An experiment is described which apparently eliminates electrode surface effects as a cause of the seismic‐electric effect. Evidently a volume variation of some electrical property or properties of the earth is necessary to explain the experimental results.

The seismic electric effect is the name which has been given to the variation of earth resistivity with elastic deformation. An account is given of the use of this effect in recording seismic waves. The recording circuit employs a direct current sent through the ground by means of a storage battery and spaced electrodes, and the changes in current due to seismic disturbances are recorded. An analysis of the noise appearing in the recording circuit is given and methods of reducing the noise level are described. The results of measurements on the magnitude of the effect are given, and the sensitivity obtainable with the seismic electric method is compared with that given by an electromagnetic pickup.

An investigation of elastic‐wave propagation in near‐surface materials using single‐frequency continuous waves and pulses, over a range of 20 to 1400 cycles, is described. While only touching upon the diverse problems involved in a study of this kind the results indicate a complexity requiring considerable research if a proper understanding, commensurate with the importance of the problem, is to be attained.

Coal as viewed microscopically is seen to be composed largely of discrete organic components referred to as macerals. Each maceral responds differently in carbonization, and each develops into a particular form of carbon in the coke product and has its own characteristic effects on coke microstructure. A classification of macerals has been developed and a number of correlations of this classification with coking behavior and coke properties have been established. Examples of how this classification serves in coal‐blend formulation and for predictive purposes are given. Basic knowledge about the chemical and physical constitution of coal and of the mechanisms involved in the response of coal to process conditions is stressed as a requirement in the development of new coke‐making technology.

In a group of properly prepared poor risk patients with advanced atherosclerosis of both the aortoiliac and femoropopliteal segments, a combined procedure, extra-anatomic bypass with an extended profundoplasty, was used for successful salvage of their ischemic--mean calf pressure=27 millimeters of mercury--limbs. Prediction of success versus failure could be determined on neither clinical nor angiographic-anatomic grounds but was possible using two simple measurements: a large aortoiliac differential pressure--deltaP--between inflow pressure obtained from a standard arm cuff and outflow pressure measured directly from the femoral artery, 89.3 millimeters of mercury versus 33.2 millimeters of mercury, p less than 0.001, and a potentially adequate outflow bed as determined by the percentage drop in outflow [(deltaPo/Po) per cent] upon papaverine injection, 36.3 versus 11.3 per cent, p less than 0.001. These values became an important part of the selection scheme developed in the approach to 24 ischemic limbs.