polarized emission
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A.A. Харченко ◽  
А.М. Надточий ◽  
А.А. Серин ◽  
С.А. Минтаиров ◽  
Н.А. Калюжный ◽  

The electroluminescence spectra of waveguiding structures based on quantum well-dots were investigated with polarization resolution in the temperature range of 60−300 K. It is found that the ground state emission consists of two peaks with different degrees of TE-polarization and these peaks are getting closer with temperature decrease. We attribute the bimodality to the existence of two different types of nanoobjects in the active region: the quantum well-dots, which have partially TE-polarized emission, and quantum dots emitting almost fully TE-polarized light.

2022 ◽  
Ji-Rui Zhang ◽  
Hao-Yi Zhang ◽  
Jia-hui Guo ◽  
Zi-Han Liu ◽  
Cheng-Yu Ma ◽  

The development of luminescent metal-organic frameworks (MOFs) has attracted extensive attention due to their applications in photoelectric device, organic light-emitting diodes (OLEDs), anti-counterfeiting, biological imaging and so on. In this...

2021 ◽  
Vol 923 (2) ◽  
pp. 204
Paulo C. Cortés ◽  
Patricio Sanhueza ◽  
Martin Houde ◽  
Sergio Martín ◽  
Charles L. H. Hull ◽  

Abstract Here, we report ALMA detections of polarized emission from dust, CS(J = 5 → 4), and C33S(J = 5 → 4) toward the high-mass star-forming region NGC 6334I(N). A clear “hourglass” magnetic field morphology was inferred from the polarized dust emission, which is also directly seen from the polarized CS emission across velocity, where the polarization appears to be parallel to the field. By considering previous findings, the field retains a pinched shape that can be traced to clump length scales from the envelope scales traced by ALMA, suggesting that the field is dynamically important across multiple length scales in this region. The CS total intensity emission is found to be optically thick (τ CS = 32 ± 12) while the C33S emission appears to be optically thin ( τ C 33 S = 0.1 ± 0.01 ). This suggests that sources of anisotropy other than large velocity gradients, i.e., anisotropies in the radiation field, are required to explain the polarized emission from CS seen by ALMA. By using four variants of the Davis–Chandrasekhar–Fermi technique and the angle dispersion function methods (ADF), we obtain an average of the estimates for the magnetic field strength on the plane of the sky of B pos = 16 mG from the dust and B pos ∼ 2 mG from the CS emission, where each emission traces different molecular hydrogen number densities. This effectively enables a tomographic view of the magnetic field within a single ALMA observation.

Galaxies ◽  
2021 ◽  
Vol 9 (4) ◽  
pp. 92
Lawrence Rudnick ◽  
Debora Katz ◽  
Lerato Sebokolodi

We present a simple but powerful technique for the analysis of polarized emission from radio galaxies and other objects. It is based on the fact that images of Stokes parameters often contain considerably more information than is available in polarized intensity and angle maps. In general, however, the orientation of the Stokes parameters will not be matched to the position angles of structures in the source. Polarization tomography, the technique presented in this paper, consists of making a series of single linear Stokes parameter images, S(ρ), where each image is rotated by an angle ρ from the initial orientation of Q and U. Examination of these images, in a series of still frames or a movie, reveals often hidden patterns of polarization angles, as well as structures that were obscured by the presence of overlapping polarized emission. We provide both cartoon examples and a quick look at the complex polarized structure in Cygnus A.

2021 ◽  
pp. 2104863
Wei‐Hsiang Lin ◽  
Pin Chieh Wu ◽  
Hamidreza Akbari ◽  
George R. Rossman ◽  
Nai‐Chang Yeh ◽  

2021 ◽  
pp. 2101674
Chang‐Jae Yu ◽  
Dong‐Myung Lee ◽  
Jin‐Kyung Han ◽  
You‐Jin Lee ◽  
Sa‐Wook Kim ◽  

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