scholarly journals Limits from the FUNK experiment on the mixing strength of hidden-photon dark matter in the visible and near-ultraviolet wavelength range

2020 ◽  
Vol 102 (4) ◽  
Author(s):  
Arnaud Andrianavalomahefa ◽  
Christoph M. Schäfer ◽  
Darko Veberič ◽  
Ralph Engel ◽  
Thomas Schwetz ◽  
...  
Keyword(s):  
Dark Matter ◽  
Wavelength Range ◽  
Near Ultraviolet ◽  
Ultraviolet Wavelength

Spectrophotometry of basic disinfectants in the ultraviolet wavelength range

2021 ◽  
Vol 64 (4) ◽  
pp. 294-299
Author(s):  
A.V. Arefiev ◽  
R.B. Guliev ◽  
E.E. Maiorov ◽  
V.B. Kotskovich ◽  
V.P. Pushkina ◽  
...  
Keyword(s):  
Wavelength Range ◽  
Ultraviolet Wavelength

Photon channeling in the vacuum‐ultraviolet wavelength range

1995 ◽  
Vol 66 (2) ◽  
pp. 2203-2205
Author(s):  
J. E. Rowe ◽  
R. A. Malic ◽  
E. E. Chaban ◽  
R. J. Chichester ◽  
C.‐M. Chiang ◽  
...  
Keyword(s):  
Wavelength Range ◽  
Vacuum Ultraviolet ◽  
Ultraviolet Wavelength

scholarly journals Bloch surface waves biosensing in the ultraviolet wavelength range – Bragg structure design for investigating protein adsorption by in situ Kretschmann-Raether ellipsometry

2021 ◽  
Vol 536 ◽  
pp. 147869 ◽  
Author(s):  
Benjamin Kalas ◽  
Karpat Ferencz ◽  
Andras Saftics ◽  
Zsolt Czigany ◽  
Miklos Fried ◽  
...  
Keyword(s):  
Surface Waves ◽  
Protein Adsorption ◽  
Wavelength Range ◽  
Structure Design ◽  
Bragg Structure ◽  
Ultraviolet Wavelength

Visualization of Radioactive Sources Without Gamma-Radiation With UV Imaging Systems

2009 ◽  
Author(s):  
Oleg Ivanov ◽  
Alexey Danilovich ◽  
Vyacheslav Stepanov ◽  
Sergey Smirnov ◽  
Anatoly Volkovich
Keyword(s):  
Gamma Radiation ◽  
Spectral Region ◽  
Imaging Systems ◽  
Measurement Time ◽  
Moving Targets ◽  
Atmospheric Air ◽  
Output Image ◽  
Uv Imaging ◽  
Near Ultraviolet ◽  
Ultraviolet Wavelength

New UV cameras are suitable for imaging of α-contamination by fluorescence of atmospheric air the near ultraviolet (wavelength — 280 – 390 nm) region. Their parameters are: FOV for detecting in UV spectral region is 8° × 6°. The optical FOV is about 48° × 36°. DayCor SUPERB UV camera has sensitivity 3×10−18 W/cm2 enables detection and displaying corona emission as weak as 1.5 pC at distance 8 m, and capture moving targets without smearing the output image. Instruments sensitivity for alpha contamination registration in terms of minimum measurable activities (MMA) have been estimated as, 40–100 Bq/cm2 (measurement time is 3600–600 sec correspondently).

Reflectivity measurements in the vacuum ultraviolet wavelength range on technical surfaces for the Wolter I telescope on board the X-ray astronomy satellite ROSAT

1986 ◽  
Vol 125 (1) ◽  
pp. 169-174 ◽  
Author(s):  
K. H. Stephan ◽  
H. Braeuninger ◽  
H. Kaase ◽  
J. Metzdorf
Keyword(s):  
Wavelength Range ◽  
Vacuum Ultraviolet ◽  
X Ray ◽  
Ultraviolet Wavelength

scholarly journals IUE Observations of Novae

1980 ◽  
Vol 5 ◽  
pp. 285-291
Author(s):  
Warren M. Sparks ◽  
Chi-Chao Wu ◽  
Albert V. Holm ◽  
Francis H. Schiffer
Keyword(s):  
Emission Line ◽  
Absorption Line ◽  
Wavelength Range ◽  
Emission Lines ◽  
First Year ◽  
Time Behavior ◽  
International Ultraviolet Explorer ◽  
Ultraviolet Wavelength ◽  
Visual Magnitude ◽  
The Continuum

In addition to offering observing time on a regular schedule, the International Ultraviolet Explorer (IUE) satellite is also being used to observe “targets of opportunity.” Novae represent one of the most exciting targets of opportunity and also one of the most difficult because of their rapid time behavior. During the first year of operation of IUE we were extremely fortunate to have three bright novae outbursts occur: Nova Cygni 1978, WZ Sagittae, and U Scorpii.Nova Cyg 1978, a fast nova, reached a maximum apparent visual magnitude of 6.2 on September 12, 1978 (Slovak and Vogt 1979). Figure 1 shows the relative flux of Nova Cyg 1978 in the long ultraviolet wavelength range (1900-3200Å) at several different times. One day after maximum (Sept. 13), the nova is still in its absorption line phase. At this point it looks like a supergiant F star with mostly Fell absorption lines (also see Cassatella et al. 1979). Later spectra show the emergence of emission lines, which is the characteristic behavior of novae in the visual. Magnesium II at 2800Å is the strongest emission line in this part of the spectrum for at least a month after outburst. The last spectrum (Nov. 1) shows mainly semi-forbidden lines of carbon, nitrogen, and oxygen. It should also be noted that the slope of the continuum flattens as the nova evolves.

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