ﻻ يوجد ملخص باللغة العربية
The Effelsberg telescope as well as the DRAO synthesis telescope are currently surveying the Galactic polarized emission at 21 cm in detail. These new surveys reveal an unexpected richness of small-scale structures in the polarized sky. However, observations made with synthesis or single-dish telescopes are not on absolute intensity scales and therefore lack information about the large-scale distribution of polarized emission to a different degree. Until now, absolutely calibrated polarization data from the Leiden/Dwingeloo polarization surveys are used to recover the missing spatial information. However, these surveys cannot meet the requirements of the recent survey projects regarding sampling and noise and new polarization observation were initiated to complement the Leiden/Dwingeloo Survey. In this paper we will outline the observation and report on the progress for a new polarization survey of the northern sky with the 26-m telescope of the DRAO.
We present results of deep polarization imaging at 1.4 GHz with the Dominion Radio Astrophysical Observatory as part of the DRAO Planck Deep Fields project. This deep extragalactic field covers 15.16 square degrees centered at RA = 16h 14m and DEC =
Radio polarimetry at decimetre wavelengths is the principal source of information on the Galactic magnetic field. The diffuse polarized emission is strongly influenced by Faraday rotation in the magneto-ionic medium and rotation measure is the prime
Integrated pulse profiles at 8.6~GHz obtained with the Shanghai Tian Ma Radio Telescope (TMRT) are presented for a sample of 26 pulsars. Mean flux densities and pulse width parameters of these pulsars are estimated. For eleven pulsars these are the f
We report circular polarization measurements from the first two years of observation with the 40 GHz polarimeter of the Cosmology Large Angular Scale Surveyor (CLASS). CLASS is conducting a multi-frequency survey covering 75% of the sky from the Atac
The LSPE is a balloon-borne mission aimed at measuring the polarization of the Cosmic Microwave Background (CMB) at large angular scales, and in particular to constrain the curl component of CMB polarization (B-modes) produced by tensor perturbations