scholarly journals Wide band propagation in train-to-train scenarios — Measurement campaign and first results

2017 ◽  
Author(s):  
Paul Unterhuber ◽  
Stephan Sand ◽  
Mohammad Soliman ◽  
Benjamin Siebler ◽  
Andreas Lehner ◽  
...  
Keyword(s):  
Wide Band ◽  
Measurement Campaign ◽  
First Results

scholarly journals The Thousand-Pulsar-Array programme on MeerKAT – I. Science objectives and first results

2020 ◽  
Vol 493 (3) ◽  
pp. 3608-3615 ◽  
Author(s):  
Simon Johnston ◽  
A Karastergiou ◽  
M J Keith ◽  
X Song ◽  
P Weltevrede ◽  
...  
Keyword(s):  
Radio Emission ◽  
Single Pulse ◽  
Wide Band ◽  
Radio Pulsars ◽  
Pulse Trains ◽  
First Results ◽  
Dispersion Measures ◽  
Large Survey ◽  
First Time

ABSTRACT We report here on initial results from the Thousand-Pulsar-Array (TPA) programme, part of the Large Survey Project ‘MeerTime’ on the MeerKAT telescope. The interferometer is used in the tied-array mode in the band from 856 to 1712 MHz, and the wide band coupled with the large collecting area and low receiver temperature make it an excellent telescope for the study of radio pulsars. The TPA is a 5 year project, which aims at to observing (a) more than 1000 pulsars to obtain high-fidelity pulse profiles, (b) some 500 of these pulsars over multiple epochs, and (c) long sequences of single-pulse trains from several hundred pulsars. The scientific outcomes from the programme will include the determination of pulsar geometries, the location of the radio emission within the pulsar magnetosphere, the connection between the magnetosphere and the crust and core of the star, tighter constraints on the nature of the radio emission itself, as well as interstellar medium studies. First, results presented here include updated dispersion measures, 26 pulsars with Faraday rotation measures derived for the first time, and a description of interesting emission phenomena observed thus far.

First results of a joint measurement campaign with PAMIR-Ka and MIRANDA-94

2020 ◽  
Author(s):  
Ingo Walterscheid ◽  
Patrick Berens ◽  
Michael Caris ◽  
Stefan Sieger ◽  
Olaf Saalmann ◽  
...  
Keyword(s):  
Joint Measurement ◽  
Measurement Campaign ◽  
First Results

scholarly journals First Results for CCD Observations with the 70 cm Meniscus Telescope

1995 ◽  
Vol 148 ◽  
pp. 56-59
Author(s):  
Omar M. Kurtanidze ◽  
Teimuraz M. Kvernadze
Keyword(s):  
Narrow Band ◽  
Spectral Response ◽  
Ccd Camera ◽  
Wide Band ◽  
Interference Filter ◽  
Ccd Observations ◽  
First Results ◽  
Observational Mode ◽  
Imaging Mode ◽  
Objective Prism

AbstractFrom the middle of 1993, a ST-6 CCD Camera (375 × 242 array with 23 × 27 microns pixel size) was mounted at the Newtonian focus (f/3) of the 70 cm meniscus telescope of the Abastumani Observatory. The photometer is now equipped with various sets of narrow-band interference, intermediate and wide band standard niters. Some pilot observations were carried out in direct imaging mode and in combination with an 8° objective prism (166 Å mm−1 at Hγ). Spectrophotometric standard stars with absolute calibrations were observed in the 8° mode to determine the CCD spectral response. Some other observations were performed with a prism-interference filter combination to estimate the observational mode efficiency.

scholarly journals Performance Analysis of Different Indoor Ultra Wide Band Channel Indicators

2018 ◽  
Vol 7 (2) ◽  
pp. 13-18
Author(s):  
A. Sorrentino ◽  
L. Mucchi ◽  
S. Cappa ◽  
M. Migliaccio
Keyword(s):  
Performance Analysis ◽  
Error Estimation ◽  
Standard Error ◽  
Wide Band ◽  
Office Building ◽  
Ultra Wide Band ◽  
Computational Time ◽  
Propagation Channel ◽  
Measurement Campaign

In this paper, performance of different indicators for the profiling of Ultra Wide Band (UWB) wireless propagation channel are analyzed. In particular, the γ-indicator and the kurtosis index k are compared in terms of the standard error. In order to improve the accuracy in the kurtosis case, results of the bootstrap error procedure are also accomplished. Further, an evaluation on the computational time needed for error estimation, is also provided. The comparison is made according to a real set of data derived from UWB measurement campaign accomplished within a modern laboratory/office building in which the two above mentioned indicators have been evaluated.

First results of the joint multisensor mine-signatures measurement campaign (MsMs Project)

2001 ◽  
Author(s):  
Patrick S. A. Verlinde ◽  
Marc P. J. Acheroy ◽  
Giuseppe Nesti ◽  
Alois J. Sieber
Keyword(s):  
Measurement Campaign ◽  
First Results

Seven-colour photometry at the Geneva Observatory

1966 ◽  
Vol 24 ◽  
pp. 262-266 ◽  
Author(s):  
M. Golay
Keyword(s):  
Wide Band ◽  
Electric System ◽  
Band Type

During the last 5 years, we have developed a seven-colour photometry at the Geneva Observatory. Our multicolour photo-electric system is of a wide-band type; the bandwidth being about 500Å for four filters. The three others are similar to theUBVsystem. In Table 1 we give the filter combinations used in our photometry (1).

Discussion of the Oblique Rotator Model Cases Of 108 Aqr and x Serp.

1976 ◽  
Vol 32 ◽  
pp. 577-588
Author(s):  
C. Mégessier ◽  
V. Khokhlova ◽  
T. Ryabchikova
Keyword(s):  
Mathematical Formulation ◽  
The Other ◽  
Rotator Model ◽  
Oblique Rotator ◽  
First Results

My talk will be on the oblique rotator model which was first proposed by Stibbs (1950), and since received success and further developments. I shall present two different attempts at describing a star according to this model and the first results obtained in the framework of a Russian-French collaboration in order to test the precision of the two methods. The aim is to give the best possible representation of the element distributions on the Ap stellar surfaces. The first method is the mathematical formulation proposed by Deutsch (1958-1970) and applied by Deutsch (1958) to HD 125248, by Pyper (1969) to α2CVn and by Mégessier (1975) to 108 Aqr. The other one was proposed by Khokhlova (1974) and used by her group.

Meridional Circulation, Turbulence, and Diffusion Processes in Stars

1976 ◽  
Vol 32 ◽  
pp. 109-116 ◽  
Author(s):  
S. Vauclair
Keyword(s):  
Convection Zone ◽  
Diffusion Processes ◽  
Meridional Circulation ◽  
Diffusion Time ◽  
Work In Progress ◽  
First Results ◽  
Stellar Envelopes ◽  
And Diffusion ◽  
Turbulence And Diffusion ◽  
Hr Diagram

This paper gives the first results of a work in progress, in collaboration with G. Michaud and G. Vauclair. It is a first attempt to compute the effects of meridional circulation and turbulence on diffusion processes in stellar envelopes. Computations have been made for a 2 Mʘstar, which lies in the Am - δ Scuti region of the HR diagram.Let us recall that in Am stars diffusion cannot occur between the two outer convection zones, contrary to what was assumed by Watson (1970, 1971) and Smith (1971), since they are linked by overshooting (Latour, 1972; Toomre et al., 1975). But diffusion may occur at the bottom of the second convection zone. According to Vauclair et al. (1974), the second convection zone, due to He II ionization, disappears after a time equal to the helium diffusion time, and then diffusion may happen at the bottom of the first convection zone, so that the arguments by Watson and Smith are preserved.

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