Polymorphism of α_S1-casein in goat milk: identification of A, B, E and F variants by biochemical and genetic analysis

Many researches, related to genetic polymorphism of αS1-casein in goat milk, showed a marked variability and implications in milk and dairy product traits. The genetic variants (from A to G) were associated with four levels of expression: 3,6 g/L per A, B and C (“strong” alleles); 1,6 g/L per E (“medium” allele); 0,6 g/L per F (“weak” allele) and 0 g/L per O (“null” allele). Differences existing among the A, B, C, D, E, F, G and O have been described (Grosclaude et al., 1994). To analyze genetic polymorphism of caseins from goat milk, distinct electrophoretic (Russo et al., 1986; Addeo et al., 1988) and chromatographic techniques (Jaubert and Martin, 1992; Iametti et al., 1999) were applied. In last years, the advancement in technological field is allowing the research of primary structure of protein variants (Ferranti et al., 1997; Trujillo et al., 2000) and basic sequence of new alleles (Martin et al., 1999; Bevilacqua et al., 2002; Ramunno et al., 2002). In this work, we employed electrophoretic protein separation (IEF and SDS-PAGE), chromatographic analysis (RP-HPLC) and molecular biology techniques based on polymerase chain reaction (real-time PCR) to detect αS1-CN genetic variants from goat milk. The utility of protein and DNA analysis combination was discussed

Jet triggered Type Ia supernovae in radio-galaxies?

We report the serendipitous discovery of a supernova (SN) in the nearby radio-galaxy 3C 78. Observations obtained with the STIS spectrograph on board the Hubble Space Telescope show, at a distance of 0.54 arcsec (300 pc) from the galaxy nucleus, a second bright source, not present in previous images. As this source was fortuitously covered by the spectrograph slit its spectrum was obtained and it is characteristic of a Type Ia SN. This SN is closely aligned with the radio-jet of 3C 78. Analysis of historical records shows that such a close association between jet and supernova occurred in 6 of the 14 reported SNe in radio-galaxies. The probability that this results from a random distribution of SN in the host galaxy is less than 0.05%. We then argue that jets might trigger supernova explosions.Comment: 9 pages, 3 figures, 1 table, to appear in ApJL, 20 Jul 200

Large Merger Recoils and Spin Flips From Generic Black-Hole Binaries

We report the first results from evolutions of a generic black-hole binary, i.e. a binary containing unequal mass black holes with misaligned spins. Our configuration, which has a mass ratio of 2:1, consists of an initially non-spinning hole orbiting a larger, rapidly spinning hole (specific spin a/m = 0.885), with the spin direction oriented -45 degrees with respect to the orbital plane. We track the inspiral and merger for ~2 orbits and find that the remnant receives a substantial kick of 454 km/s, more than twice as large as the maximum kick from non-spinning binaries. The remnant spin direction is flipped by 103 degrees with respect to the initial spin direction of the larger hole. We performed a second run with anti-aligned spins, a/m = +-0.5 lying in the orbital plane that produces a kick of 1830 km/s off the orbital plane. This value scales to nearly 4000 km/s for maximally spinning holes. Such a large recoil velocity opens the possibility that a merged binary can be ejected even from the nucleus of a massive host galaxy.Comment: 4 pages. Accepted for publication in ApJ

Kinerja Protokol Routing Pada Lingkungan Wireless Mesh Network Dengan Combined Scalable Video Coding

Teknologi wireless mesh network (WMN) yang beroperasi pada standar IEEE 802.11 merupakan teknologi jaringan nirkabel terdiri dari mesh router dan mesh client dipadukan dengan internet, teknologi seluler dan jaringan sensor. Seiring perkembangan teknologi dan meningkatnya kebutuhan manusia, transmisi video melalui jaringan nirkabel semakin penting dan dibutuhkan. Umumnya, pembahasan transmisi video melalui teknologi jaringan nirkabel masih secara umum, sehingga memberikan tantangan dalam penggunaan throughput, end to end delay, packet loss dan PSNR. Combined Scalable Video Coding (CSCV) merupakan skema baru perkembangan dari H.264/MPEG-4. Pada penelitian ini CSCV digunakan untuk pengiriman video dengan standar IEEE 802.11 pada lingkungan WMN dan diaplikasikan pada protokol AODV, DSDV dan DSR. Untuk mengetahui kinerja protokol routing mana yang lebih baik dalam transmisi video CSVC digunakan metrik pengujian end to end delay, throughput, packet loss dan PSNR. Untuk analisis dan pengukuran data digunakan simulator NS-2, dan hasil percobaan simulasi yang dilakukan menunjukkan AODV memiliki nilai end to end delay yang rendah yaitu 0,57 detik, DSR memiliki nilai yang baik didalam throughput yaitu 31 kbps dan PSNR yaitu 22,7 dB, sedangkan DSDV memiliki packet loss yang rendah yaitu 56,4%

Radio morphology and spectral analysis of cD galaxies in rich and poor galaxy clusters

We present a radio morphological study and spectral analysis for a sample of 13 cD galaxies in rich and poor clusters of galaxies.} Our study is based on new high sensitivity Giant Metrewave Radio Telescope (GMRT) observations at 1.28 GHz, 610 MHz and 235 MHz, and on archival data. From a statistical sample of cluster cD galaxies we selected those sources with little information available in the literature and promising for the detection of aged radio emission. Beyond the high sensitivity images for all 13 radio galaxies, we present also a detailed spectral analysis for 7 of them. We found a variety of morphologies and linear sizes, as typical for radio galaxies in the radio power range sampled here (low to intermediate power radio galaxies). The spectral analysis shows that 10/13 radio galaxies have steep radio spectrum, with spectral index $\alpha \ge 1$. In general, the radiative ages and growth velocities are consistent with previous findings that the evolution of radio galaxies at the cluster centres is affected by the dense external medium (i.e. low growth velocities and old ages. We suggest that the dominant galaxies in A 2622 and MKW 03s are dying radio sources, which at present are not fed by nuclear activity. On the other hand, the spectacular source at the centre of A 2372 might be a very interesting example of restarted radio galaxy. For this source we estimated a life cycle of the order of 10$^6$ yr.Comment: Accepted by A&A, 25 pages, 28 figures, 6 tables and appendix Full version including high quality images available at http://www.ira.inaf.it/~tventuri/pap/Venturi.pd

Clave para el reconocimiento de los géneros de algas macrofitas del intermareal rocoso bonaerense

Fil: Parma, Ana. Instituto de Biología Marina y Pesquera Almirante Storni. Río Negro; ArgentinaFil: Pascual, Marcela S.. Instituto de Biología Marina y Pesquera Almirante Storni. Río Negro; ArgentinaFil: Sar, Eugenia Alicia. División Ficología. Facultad de Ciencias Naturales y Museo. Universidad Nacional de La Plata; Argentin

BeppoSAX observation of Hercules A and MRC 0625-536

We present BeppoSAX observations of the two FR I type radio galaxies Hercules A (3C 348) and MRC 0625-536 in the energy range $0.2 - 200$ keV. Data analysis shows that the X-ray flux from Hercules A is consistent with a diffuse thermal plasma emitting at $T \approx 4-5$ keV with a possible, but somewhat uncertain, contribution of a softer component at $T \approx 3$ keV. The non thermal emission from the active nucleus must be significantly smaller than the thermal one, and no indication of relevant core obscuration by a surrounding torus was detected. The flux from MRC 0625-536 originates form an extended region and has been fitted to a thermal law with $T \approx 5.7$ keV and with a column density consistent with the galactic absorption. A spatially resolved spectral analysis does not show a relevant variation of the temperature and the metallicity across the diffuse emission zone. A non thermal spectral component, related to the nuclear activity, may be present in the innermost region with some possible amount of local obscuration, contributing \lapp 10% to the total luminosity. Hard X-ray emission from MRC 0625-536 has been detected in the PDS (15 - 200 keV) that may be related either to its galactic core or to the intracluster region

Studi Kecermatan Alat Ukur Kebulatan (Roundness Tester Mechine) Produksi Laboratorium Pengukuran Universitas Riau

Accuracy is the closeness or the accuracy of the measurement results with the actual value. Accuracy can also mean a measure of the closeness results of the analysis of the actual invitation analyte levels. Accuracy is vital that must be fulfilled and owned by any measurement tool, use the measuring instrument that has high accuracy and good will produce accurate measurement data and other wise use measuring devices are not accurate, do not meet the standards of the results obtained will not be accurate. This study aims to determine the value of the mandrel roundness deviation, roundness accuracy Measuring Equipment (Roundness Tester Machine) and large deviations in the roundness measuring instrument (Roundness TesterMachine) (instrument error) and the operator or gauges (human error). From the results, the large stroundness deviation value for minimum circumscribed circle is 0,474 mm, maximum inscribed circle 0,417 mm, minimum zone circle 0,495 mm, least squares circle 0,207 mm, for the value of sphericity (roundness) for the smallest outer for minimum circumscribed circleis 0,003 mm, maximum inscribed circle 0,003 mm, minimum zone circle is 0,003 mm, least squares is 0,001 mm. Value accuracy roundness measuring instrument (Roundness TesterMachine) in position 1 = 0,006 mm, position 2 = 0,006 mm, position 3 = 0,011 mm, position 4 = 0,018 mm, position 5 = 0,003 mm, position 6 = 0,018 mm, position 7 = 0,021 mm, position 8 = 0,031 mm, position 9 = 0,002 mm, position 10 = 0,001 mm and error measuring instrument (instrument error) is the largest 0,02944 mm or 18,871% and the smallest deviation is 0,00029 mm or 0,225%. Operator error or measuring (Human Error) for first test (human) 22%, second test 5,33%, third test 182%, fourth test 187%, fifth test 58%

X-ray-emitting Atmospheres of B2 Radio Galaxies

We report ROSAT PSPC spatial and spectral analysis of the eight B2 radio galaxies NGC 315, NGC 326, 4C 35.03, B2 0326+39, NGC 2484, B2 1040+31, B2 1855+37, and 3C 449, expected to be representative of the class of low-power radio galaxies. Multiple X-ray components are present in each, and the gas components have a wide range of linear sizes and follow an extrapolation of the cluster X-ray luminosity/temperature correlation, implying that there is no relationship between the presence of a radio galaxy and the gas fraction of the environment. No large-scale cooling flows are found. There is no correlation of radio-galaxy size with the scale or density of the X-ray atmosphere. This suggests that it is processes on scales less than those of the overall gaseous environments which are the major influence on radio-source dynamics. The intergalactic medium is usually sufficient to confine the outer parts of the radio structures, in some cases even to within 5 kpc of the core. In the case of NGC 315, an extrapolation suggests that the pressure of the atmosphere may match the minimum pressure in the radio source over a factor of about 40 in linear size (a factor of about 1600 in pressure).Comment: 34 pages, including 10 figures, using aasms4.sty To appear in the Ap