The influence of high-density environment on the radio-far-infrared correlation of spiral galaxies

1991 ◽  
Vol 372 ◽  
pp. 419 ◽  
Author(s):  
T. K. Menon
Keyword(s):  
Spiral Galaxies ◽  
Far Infrared ◽  
High Density

Development of short-wavelength far-infrared laser for high density plasma diagnostics

2001 ◽  
Vol 72 (1) ◽  
pp. 1094-1097 ◽  
Author(s):  
S. Okajima ◽  
K. Nakayama ◽  
H. Tazawa ◽  
K. Kawahata ◽  
K. Tanaka ◽  
...  
Keyword(s):  
Plasma Diagnostics ◽  
Short Wavelength ◽  
Far Infrared ◽  
Infrared Laser ◽  
High Density ◽  
Far Infrared Laser ◽  
Density Plasma

scholarly journals Magnetic Field Strengths of Spiral Galaxies and the Far-Infrared/Radio Correlation

1990 ◽  
Vol 140 ◽  
pp. 241-241
Author(s):  
A. J. Fitt ◽  
P. Alexander
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Field Distribution ◽  
Detection Rate ◽  
Spiral Galaxies ◽  
Far Infrared ◽  
Magnetic Field Distribution ◽  
Selection Effects ◽  
The Magnetic Field ◽  
Field Strengths

We have calculated equipartition magnetic fields for a complete, optically-selected sample of 165 spiral galaxies. The magnetic field distribution (fig. 1) is type independent, and shows remarkably little spread in values, around 1 decade in B. This is not due to selection effects because of the nature of the sample and the 95 percent detection rate.

scholarly journals Spatial Distribution of Far Infrared and Radio Continuum Emission in Spiral Galaxies

1996 ◽  
Vol 171 ◽  
pp. 415-415
Author(s):  
Y.D. Mayya ◽  
T.N. Rengarajan
Keyword(s):  
Spiral Galaxies ◽  
Far Infrared ◽  
Radio Continuum ◽  
Continuum Emission ◽  
Emission Profile ◽  
Exponential Component ◽  
Dust Temperature ◽  
Order Of Magnitude ◽  
Disk Component ◽  
Exponential Disk

A study of 8 nearby spiral galaxies (NGC 2903, 3079, 3198, 3628, 4303, 4321, 4656 and 6946) is carried out using the radio continuum (RC) and far infrared (FIR) images at 1′ resolution. These images are used to study the radial gradients in the ratios of FIR to RC (Q60 and Q100), warm dust temperature (Td(60/100)) etc. The main results are illustrated with NGC 2903 as an example in Fig. 1, where azimuthally averaged quantities are plotted. Td(60/100) decreases away from the center (45–25 K), increasing again by ∼ 5 K in outer galaxies. Typically Q60 decreases by a factor of three away from the center in a given galaxy, but has an order of magnitude spread in the pixel values over all the galaxies. In contrast, Q100 shows flatter gradient, which is expected from the observed temperature gradient. 20 cm RC emission profile is also shown in Fig. 1. The RC and FIR profiles can be fitted by a combination of central gaussian and exponential disk components. In general RC and FIR have about the same fraction of exponential component with the exception of NGC 3628, in which the FIR is dominated by the gaussian while the RC is mostly disk component (see Fig. 2). In 5 of the remaining 7 galaxies, the exponential component contributes > 50% of the total. In general RC scale lengths are larger than the FIR.

Far-Infrared Transmission of Commercially Available Crystals and High-Density Polyethylene

1966 ◽  
Vol 20 (3) ◽  
pp. 190-191 ◽  
Author(s):  
W. G. Fateley ◽  
R. E. Witkowski ◽  
G. L. Carlson
Keyword(s):  
High Density Polyethylene ◽  
Far Infrared ◽  
High Density ◽  
Infrared Transmission
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