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799 results on '"Piasecki, M"'

2. Photoluminescence features and nonlinear-optical properties of the Ag0.05Ga0.05Ge0.95S2eEr2S3 glasses

Author

Halyan, V. V., Yukhymchuk, V. O., Gule, Ye. G., Ozga, K., Jedryka, K. J., Ivashchenko, I. A., Skoryk, M. A., Kevshyn, A. H., Olekseyuk, I. D., Tishchenko, P. V., Shevchuk, M. V., and Piasecki, M.

Subjects
Physics - Applied Physics, Condensed Matter - Materials Science
Abstract

Preparation technology, the structure determination, multiband luminescence and nonlinear optical properties of the chalcogenide glasses are subject of present work. The glass samples with two different Er content were prepared by classical two-stage melt-quenching method. Glass state and morphology were confirmed by X-ray and EDS techniques. Influence of the Erbium doping on the luminescence and NLO properties was investigated.

Published
2020

23. Design and Performance of the ARIANNA Hexagonal Radio Array Systems

Author

Barwick, S. W., Berg, E. C., Besson, D. Z., Cheim, E., Duffin, T., Hanson, J. C., Klein, S. R., Kleinfelder, S. A., Prakash, T., Piasecki, M., Ratzlaff, K., Reed, C., Roumi, M., Samanta, A., Stezelberger, T., Tatar, J., Walker, J., Young, R., and Zou, L.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract

We report on the development, installation and operation of the first three of seven stations deployed at the ARIANNA site's pilot Hexagonal Radio Array in Antarctica. The primary goal of the ARIANNA project is to observe ultra-high energy (>100 PeV) cosmogenic neutrino signatures using a large array of autonomous stations each dispersed 1 km apart on the surface of the Ross Ice Shelf. Sensing radio emissions of 100 MHz to 1 GHz, each station in the array contains RF antennas, amplifiers, 1.92 G-sample/s, 850 MHz bandwidth signal acquisition circuitry, pattern-matching trigger capabilities, an embedded CPU, 32 GB of solid-state data storage, and long-distance wireless and satellite communications. Power is provided by the sun and LiFePO4 storage batteries, and the stations consume an average of 7W of power. Operation on solar power has resulted in >=58% per calendar-year live-time. The station's pattern-trigger capabilities reduce the trigger rates to a few milli-Hertz with 4-sigma thresholds while retaining good stability and high efficiency for neutrino signals. The timing resolution of the station has been found to be 0.049 ps, RMS, and the angular precision of event reconstructions of signals bounced off of the sea-ice interface of the Ross Ice Shelf ranged from 0.14 to 0.17 degrees. A new fully-synchronous 2+ G-sample/s, 1.5 GHz bandwidth 4-channel signal acquisition chip with deeper memory and flexible >600 MHz, <1 mV RMS sensitivity triggering has been designed and incorporated into a single-board data acquisition and control system that uses an average of only 1.7W of power. Along with updated amplifiers, these new systems are expected to be deployed during the 2014-2015 Austral summer to complete the Hexagonal Radio Array., Comment: 17 Page, 27 Figures, 1 Table

Published
2014

24. Time Domain Response of the ARIANNA Detector

Author

Barwick, S. W., Berg, E. C., Besson, D. Z., Hanson, J. C., Klein, S. R., Kleinfelder, S. A., Piasecki, M., Ratzlaff, K., Reed, C., Roumi, M., Stezelberger, T., Tatar, J., Walker, J., Young, R., and Zou, L.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The Antarctic Ross Ice Shelf Antenna Neutrino Array (ARIANNA) is a high-energy neutrino detector designed to record the Askaryan electric field signature of cosmogenic neutrino interactions in ice. To understand the inherent radio-frequency (RF) neutrino signature, the time-domain response of the ARIANNA RF receiver must be measured. ARIANNA uses Create CLP5130-2N log-periodic dipole arrays (LPDAs). The associated effective height operator converts incident electric fields to voltage waveforms at the LDPA terminals. The effective height versus time and incident angle was measured, along with the associated response of the ARIANNA RF amplifier. The results are verified by correlating to field measurements in air and ice, using oscilloscopes. Finally, theoretical models for the Askaryan electric field are combined with the detector response to predict the neutrino signature., Comment: 13 pages, 19 figures, in press at Astroparticle Physics Journal. Contact: J.C. Hanson (j529h838@ku.edu)

Published
2014
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26. Time-domain response of the ARIANNA detector

Author

Barwick, SW, Berg, EC, Besson, DZ, Duffin, T, Hanson, JC, Klein, SR, Kleinfelder, SA, Piasecki, M, Ratzlaff, K, Reed, C, Roumi, M, Stezelberger, T, Tatar, J, Walker, J, Young, R, and Zou, L

Subjects
GZK neutrinos, Askaryan effect, Radio detector, astro-ph.IM, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics
Abstract

The Antarctic Ross Ice Shelf Antenna Neutrino Array (ARIANNA) is a high-energy neutrino detector designed to record the Askaryan electric field signature of cosmogenic neutrino interactions in ice. To understand the inherent radio-frequency (RF) neutrino signature, the time-domain response of the ARIANNA RF receiver must be measured. ARIANNA uses Create CLP5130-2N log-periodic dipole arrays (LPDAs). The associated effective height operator converts incident electric fields to voltage waveforms at the LDPA terminals. The effective height versus time and incident angle was measured, along with the associated response of the ARIANNA RF amplifier. The results are verified by correlating to field measurements in air and ice, using oscilloscopes. Finally, theoretical models for the Askaryan electric field are combined with the detector response to predict the neutrino signature.

Published
2015

38. Design and Performance of the ARIANNA Hexagonal Radio Array Systems

Author

Barwick, SW, Berg, EC, Besson, DZ, Cheim, E, Duffin, T, Hanson, JC, Klein, SR, Kleinfelder, SA, Prakash, T, Piasecki, M, Ratzlaff, K, Reed, C, Roumi, M, Samanta, A, Stezelberger, T, Tatar, J, Walker, J, Young, R, and Zou, L

Subjects
astro-ph.IM, physics.ins-det
Abstract

We report on the development, installation and operation of the first threeof seven stations deployed at the ARIANNA site's pilot Hexagonal Radio Array inAntarctica. The primary goal of the ARIANNA project is to observe ultra-highenergy (>100 PeV) cosmogenic neutrino signatures using a large array ofautonomous stations each dispersed 1 km apart on the surface of the Ross IceShelf. Sensing radio emissions of 100 MHz to 1 GHz, each station in the arraycontains RF antennas, amplifiers, 1.92 G-sample/s, 850 MHz bandwidth signalacquisition circuitry, pattern-matching trigger capabilities, an embedded CPU,32 GB of solid-state data storage, and long-distance wireless and satellitecommunications. Power is provided by the sun and LiFePO4 storage batteries, andthe stations consume an average of 7W of power. Operation on solar power hasresulted in >=58% per calendar-year live-time. The station's pattern-triggercapabilities reduce the trigger rates to a few milli-Hertz with 4-sigmathresholds while retaining good stability and high efficiency for neutrinosignals. The timing resolution of the station has been found to be 0.049 ps,RMS, and the angular precision of event reconstructions of signals bounced offof the sea-ice interface of the Ross Ice Shelf ranged from 0.14 to 0.17degrees. A new fully-synchronous 2+ G-sample/s, 1.5 GHz bandwidth 4-channelsignal acquisition chip with deeper memory and flexible >600 MHz,

Published
2014

47. Black hole masses from power density spectra: determinations and consequences

Author

Czerny, B., Nikolajuk, M., Piasecki, M., and Kuraszkiewicz, J.

Subjects
Astrophysics
Abstract

We analyze the scaling of the X-ray power density spectra with the mass of the black hole on the example of Cyg X-1 and Seyfert 1 galaxy NGC 5548. We show that the high frequency tail of the power density spectrum can be successfully used for determination of the black hole mass. We determine the masses of the black holes in 6 Broad Line Seyfert 1 galaxies, 5 Narrow Line Seyfert 1 galaxies and two QSOs using available power density spectra. The proposed scaling is clearly appropriate for other Seyfert galaxies and QSOs. In all but 1 normal Seyferts the resulting luminosity to the Eddington luminosity ratio is smaller than 0.15, with a source MCG -6-15-30 being an exception. The applicability of the same scaling to Narrow Line Seyfert 1 is less clear and there may be a systematic shift between the power spectra of NLS1 and S1 galaxies of the same mass, leading to underestimation of the black hole mass. However, both the method based on variability and the method based on spectral fitting show that those galaxies have relatively low masses and high luminosity to the Eddington luminosity ratio, supporting the view of those objects as analogs of galactic sources in their high/soft or very high state based on the overall spectral shape. Bulge masses of their host galaxies are similar to normal Seyfert galaxies so they do not follow the black hole mass-bulge mass relation for Seyfert galaxies, being evolutionary less advanced, as suggested by Mathur (2000). The bulge mass-black hole mass relation in our sample is consistent with being linear, with black hole to bulge ratio $\sim$ 0.03 %, similar to Wandel (1999) and Laor (1998, 2001) for low mass objects but significantly shifted from the relation of Magorrian et al. (1998) and McLure & Dunlop (2000)., Comment: 11 pages, 7 figures, 1 table, accepted for publication in MNRAS

Published
2000
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