Evolution of protein bound Maillard reaction end-products and free Amadori compounds in low lactose milk in presence of fructosamine oxidase I

Thermal treatments and storage influence milk quality, particularly in low lactose milk as the higher concentration of reducing sugars can lead to the increased formation of the Maillard reaction products (MRPs). The control of the Amadori products (APs) formation is the key step to mitigate the Maillard reaction (MR) in milk. The use of fructosamine oxidases, (Faox) provided promising results. In this paper, the effects of Faox I were evaluated by monitoring the concentration of free and bound MRPs in low lactose milk during shelf life. Results showed that the enzyme reduced the formation of protein-bound MRPs down to 79% after six days at 37 °C. Faox I lowered the glycation of almost all the free amino acids resulting effective on basic and polar amino acids. Data here reported corroborate previous findings on the potentiality of Faox enzymes in controlling the early stage of the MR in foods

A family of filters to search for frequency dependent gravitational wave stochastic backgrounds

We consider a three dimensional family of filters based on broken power law spectra to search for gravitational wave stochastic backgrounds in the data from Earth-based laser interferometers. We show that such templates produce the necessary fitting factor for a wide class of cosmological backgrounds and astrophysical foregrounds and that the total number of filters required to search for those signals in the data from first generation laser interferometers operating at the design sensitivity is fairly smallComment: 4 pages, 4 figures, uses iopart.cls, accepted for publications on Classical and Quantum Gravity (Special Issue, Proceedings of Amaldi 2003

Efficacy and Tolerability of a New Formulation in Rectal Ointment Based on Zn-L-Carnosine (Proctilor®) in the Treatment of Haemorrhoidal Disease

Haemorrhoidal disease (HD) shows high prevalence in western countries, reaching 4.4% per year in the US. Topical preparations are the first-line treatments, which are readily available as "over-the-counter" (OTC) products, often containing a nonstandardised mixture of "natural" remedies, or anaesthetics or cortisol;those latter are not free from undesirable effects. The Zinc-L-Carnosine is a cytoprotective compound, promoting mucosal repair in the gastrointestinal tract and also in mucosal repair, following radiation injuries to the rectum as well as in ulcerative colitis. Our aim was to study the efficacy of Zinc-L-Carnosine in relieving acute symptoms of HD, testing a preparation in the rectal ointment, Proctilor (R), in patients complaining of bleeding or thrombosed piles. In a multicentre open trial, 21 patients older than 18 years of age were enrolled. The symptoms of HD were graded according to the Haemorrhoidal Disease Symptoms Score (HDSS) in association with the Short Health Scale (SHS) to assess the influence of HD on quality of life. The pain was assessed with the VAS score, bowel habit by means of the Bristol scale. The patients were evaluated at enrolment (T0) and 2 (T1) and 4 (T2) weeks of treatment with Proctilor (R) rectal ointment. There were 10 men and 11 women; mean age, 49 years. Pain, bleeding, and thrombosis were all significantly reduced after treatment; the mean VAS score decreased from 4.71 +/- 3.05 at T0 to.52 +/- 0.87 and.05 +/- 0.22 at T1 and T2, respectively; (mean +/- SD; p < 0.001 in both cases). Similarly, the HDSS score showed to be significantly reduced between T0, T1 (8.05 +/- 4.55 vs. 1.14 +/- 1.01), and T2 (8.05 +/- 4.55 vs. 24 +/- 0.44) (mean +/- SD; p < 0.001 in both cases). Quality of life showed to be improved as the SHS score decreased significantly with treatment (7.90 +/- 4.17 at T0 vs. 4.24 +/- 0.44 at T1 vs. 4.05 +/- 0.22 at T2; mean +/- SD; p < 0.001 in both cases). The Bristol score of defecation remained substantially unchanged. No side effects or discontinuation of treatment were reported. Results of our investigation suggest a role of Proctilor (R) rectal ointment in treating symptomatic HD with good results and an excellent safety profile. However, our preliminary results encourage further studies on a larger number of patients to confirm the role of Zinc-L-Carnosine in the rectal ointment for the topical treatment of HD

Helium abundance in globular clusters: the R-method

A new estimate of the helium abundance, Y, in globular cluster stars has been obtained through the application of the R-method of Iben (1968) to a sample of galactic globular clusters. A new calibration for the (R-Y) relation has been derived. The influence on the calibration of some theoretical uncertainties and of phenomena like mass loss have been analyzed. The procedure, applied to a sample of 15 clusters whose data reach a level of completeness and photometric accuracy enough to give statistically significant results, led to a mean value for Y equal to 0.23 + or - 0.02. A constant Y with varying metal content seems consistent with the data. The distribution of the number ratios of asymptotic and giant branch stars suggests the full development of the semiconvective zone for the stars of all the considered clusters

IUE observations of UB-bright stars in M 3

IUE UV observations of three "UV-bright" stars in M3 are presented. The brightest object - vZ1128 - is confirmed to be a bright Post-AGB star with logL/Lsun=3.09 and Te=30,000 K, which contributes about 25% of the integrated UV light from the cluster at λ=1500Å. The nature of the two other stars, i.e. 524 (logL/Lsun=2.06, Te=33,000 K) and 7561 (iogL/Lsun=2.04, Te=35,000 K), is still controversial. They might be respectively AGB-manque' stars of the sort suggested by Greggio & Renzini (1990), or the result of mergers of binary systems according to Iben (1990), but other possibilities are considered and discussed

High precision photometry of 10000 stars in M 3

A new color-magnitude diagram for M3 is presented. 10000 stars have been measured down to V = 22 with an internal accuracy better than 0.03 mag to get complete and very accurate samples over well defined areas

The stellar population of the globular cluster M 3. I. Photographic photometry of 10 000 stars

A new photographic colour-magnitude diagram (CMD) for the Galactic globular cluster M 3 is presented. This constitutes the preliminary part of a long-term project aiming at using the M 3 stellar population as a powerful test-bench for the predictions of the stellar evolution theory and for cosmological purposes via the population synthesis methods. In this first step, more than 10 000 stars were measured on the Mt. Palomar and Mt. Wilson original plates (Sandage 1953) down to V>21.5 with very high internal accuracy to obtain complete samples over well defined areas. The list of magnitudes, colours and positions for all the measured stars is available from the CDS at Strasbourg upon request. From the analysis of the present CMD the following results are derived: (a) The overall morphology of the main branches and their normal points reproduce in essence the previous results. In particular, the existence of a sizeable population of blue straggler stars (BSS) detected by Sandage (1953) is confirmed. (b) The Red Giant Branch (RGB) and Asymptotic Giant Branch (AGB) are clearly separated, and the RGB metallicity indicators lead to =-1.66+/-0.10 with an upper limit σ[Fe/H]~0.09. The narrow Sub-Giant Branch (SGB) and Turn-Off (TO) region suggest that also the dispersion in the abundance of C,N,O should be very low. (c) The Horizontal Branch (HB) is narrow and the bulk of HB stars covers a wide range in effective temperature (logT_e_=3.70 to 4.55). Six groups of stars have been tentatively identified based on their location on the HB, namely: R (red), V (variables), B (blue), EB (extremely blue) HEB (hot extremely blue) ER (extremely red) - some of these stars may be non-genuine HB stars. The various population ratios computed lead: (i) to confirm the full extension of semiconvection (or, alternatively, to calibrate the overshooting parameter) and to exclude the existence of a "long" breathing pulses phase; and (ii) to determine the primordial helium abundance Y_p_ via the R-method, Y_p_=0.23+/- 0.02. (d) The distance modulus is estimated as (m-M)_0_=14.94 and the age is t=18.7+/-3.5Gyr. The effects of different assumptions and the results previously obtained by various authors using the present data are also discussed. It is interesting to note the wide range of values estimated for the age (from ~13 to ~20Gyr). (e) 65 BSS candidates have been identified. Within the considered areas, BSS seem to be less centrally concentrated than the subgiants in the same magnitude interval, but further checks are needed. Speculations on the possible detection of a BSS progeny located in the red HB are also presented. Future papers of this series will deal with the analysis of CCD data for the inner regions of the cluster

Testing gravitational-wave searches with numerical relativity waveforms: Results from the first Numerical INJection Analysis (NINJA) project

The Numerical INJection Analysis (NINJA) project is a collaborative effort between members of the numerical relativity and gravitational-wave data analysis communities. The purpose of NINJA is to study the sensitivity of existing gravitational-wave search algorithms using numerically generated waveforms and to foster closer collaboration between the numerical relativity and data analysis communities. We describe the results of the first NINJA analysis which focused on gravitational waveforms from binary black hole coalescence. Ten numerical relativity groups contributed numerical data which were used to generate a set of gravitational-wave signals. These signals were injected into a simulated data set, designed to mimic the response of the Initial LIGO and Virgo gravitational-wave detectors. Nine groups analysed this data using search and parameter-estimation pipelines. Matched filter algorithms, un-modelled-burst searches and Bayesian parameter-estimation and model-selection algorithms were applied to the data. We report the efficiency of these search methods in detecting the numerical waveforms and measuring their parameters. We describe preliminary comparisons between the different search methods and suggest improvements for future NINJA analyses.Comment: 56 pages, 25 figures; various clarifications; accepted to CQ

Upper limits on the strength of periodic gravitational waves from PSR J1939+2134

The first science run of the LIGO and GEO gravitational wave detectors presented the opportunity to test methods of searching for gravitational waves from known pulsars. Here we present new direct upper limits on the strength of waves from the pulsar PSR J1939+2134 using two independent analysis methods, one in the frequency domain using frequentist statistics and one in the time domain using Bayesian inference. Both methods show that the strain amplitude at Earth from this pulsar is less than a few times $10^{-22}$.Comment: 7 pages, 1 figure, to appear in the Proceedings of the 5th Edoardo Amaldi Conference on Gravitational Waves, Tirrenia, Pisa, Italy, 6-11 July 200