scholarly journals 5 GHz Polarization Observations of 33 Galactic Radio Sources

1975 ◽  
Vol 28 (2) ◽  
pp. 209 ◽  
Author(s):  
DK Milne ◽  
JR Dickel
Keyword(s):  
Supernova Remnants ◽  
Radio Sources ◽  
5 Ghz ◽  
Galactic Radio

Polarization observations have been made of 33 galactic radio sources, mostly supernova remnants, at a frequency of 5 GHz using the 64 m telescope at Parkes. Maps of the observed polarization vectors superposed upon total intensity isotherms are presented for each source.

scholarly journals Some Observations of Shell-type Galactic Radio Sources

1967 ◽  
Vol 20 (3) ◽  
pp. 297 ◽  
Author(s):  
ER Hill
Keyword(s):  
Radio Emission ◽  
Spherical Symmetry ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Milky Way ◽  
Radio Sources ◽  
Radio Observations ◽  
Shell Type ◽  
Rosette Nebula ◽  
Galactic Radio

Radio evidence for two new supernova remnants in the Southern Milky Way is presented. Some new observations of the known supernova remnant, source 1439-62, and of the Rosette nebula, a shell source but not a supernova remnant, are also presented. The problem of finding model shells to fit the radio observations is considered and it is shown that the radio emission from 1439-62 is unlikely to originate in a shell with spherical symmetry.

scholarly journals Classification of Supernova Remnants and HII Regions from their Recombination Line Emission

1972 ◽  
Vol 25 (5) ◽  
pp. 539 ◽  
Author(s):  
JR Dickel ◽  
DK Milne
Keyword(s):  
Electron Temperature ◽  
Supernova Remnants ◽  
Line Emission ◽  
Hii Regions ◽  
Radio Sources ◽  
Recombination Line ◽  
Line Frequency ◽  
Upper Limits ◽  
Galactic Radio

H109a, recombination line observations are used in an attempt to classify 46 galactic radio sources as either supernova remnants or HII regions. Long integrations at the H109a line frequency on two well-known supernova remnants (IC 443 and 3C 391) provide improved upper limits on the line emission from these objects. From these results the electron temperature in IC 443 is estimated to be in excess of 1�6 � 104 K.

scholarly journals The VSOP Survey: final aggregate results

2006 ◽  
Vol 2 (S238) ◽  
pp. 357-358
Author(s):  
R. Dodson ◽  
S. Horiuchi ◽  
W. Scott ◽  
E. Fomalont ◽  
Z. Paragi ◽  
...  
Keyword(s):  
Brightness Temperature ◽  
Radio Astronomy ◽  
Radio Sources ◽  
Survey Paper ◽  
Brightness Temperatures ◽  
Future Space ◽  
Magnetic Spectrum ◽  
Electro Magnetic ◽  
5 Ghz ◽  
Galactic Radio

AbstractIn February 1997 the Japanese radio astronomy satellite HALCA was launched to provide the space-borne element for the VSOP mission. HALCA provided linear baselines three-times greater than that of ground arrays, thus providing higher resolution and higher AGN brightness temperature measurements and limits. Twenty-five percent of the scientific time of the mission was devoted to the “VSOP survey” of bright, compact, extra-galactic radio sources at 5 GHz. A complete list of 294 survey targets were selected from pre-launch surveys, 91% of which were observed during the satellite's lifetime.The major goals of the VSOP Survey are statistical in nature: to determine the brightness temperature and approximate structure, to provide a source list for use with future space VLBI missions, and to compare radio properties with other data throughout the electro-magnetic spectrum. All the data collected have now been analysed and is being prepared for the final image Survey paper. In this paper we present details of the mission, and some statistics of the images and brightness temperatures.

scholarly journals Radio Emission from Novae and Supernovae

1956 ◽  
Vol 9 (1) ◽  
pp. 84 ◽  
Author(s):  
BY Mills ◽  
AG Little ◽  
KV Sheridan
Keyword(s):  
Radio Emission ◽  
Supernova Remnants ◽  
Milky Way ◽  
Radio Sources ◽  
Constant Ratio ◽  
Radio Observations ◽  
Maximum Emission ◽  
Galactic Radio Emission ◽  
Galactic Radio

Attempts have been made to observe the radio emission at 3?5 m from two supernovae and ten novae. Kepler's star was the only reasonably certain identification. A comparison with radio observations of other supernova remnants suggests a constant ratio between the present radio emission and the maximum emission of light. It is concluded that for common novae, which are not detectable as radio sources, this ratio must be smaller than for supernovae. The galactic radio emission near the plane of the Milky Way could be largely the integrated emission of supernova remnants but common novae could not contribute appreciably.

The prevalence of supernova remnants among unidentified Galactic radio sources

1989 ◽  
Vol 341 ◽  
pp. 151 ◽  
Author(s):  
David J. Helfand ◽  
T. Velusamy ◽  
R. H. Becker ◽  
Felix J. Lockman
Keyword(s):  
Supernova Remnants ◽  
Radio Sources ◽  
Galactic Radio

scholarly journals Combined-Array Imaging of Extra-Galactic Radio Sources

1994 ◽  
Vol 140 ◽  
pp. 123-124
Author(s):  
Chidi E. Akujor ◽  
Lars B. Bååth
Keyword(s):  
Structural Information ◽  
Small Scale ◽  
Radio Sources ◽  
Single Image ◽  
Yield Information ◽  
5 Ghz ◽  
Array Imaging ◽  
The Relationship ◽  
Telescope Arrays ◽  
Galactic Radio

The resolving powers of existing telescope arrays are quite different. For example the extended new MERLIN at 5 GHz readily yields maps of ~ 50 mas resolution compared with the VLA ~ 350 mas, WSRT ~ 4000 mas, EVN ~ 5 mas, global VLBI ~ 1 mas, etc. This means that images obtained with these instruments yield information on different scales that sometimes appear unrelated. However, the need to have structural information on intermediate scales demands that data from different arrays be combined to make a single image. This is particularly important in extra-galactic radio sources where the relationship between core-jet features on different scales (parsec and kiloparsec) and the connection between small-scale and extended features need to be established.By combining uvdata from two or more arrays we can routinely make images that represent a balance between the capabilities of the combined arrays, (e.g. VLA + MERLIN, MERLIN+VLBI, VLA+WSRT etc) at cm wavelengths. In order to do this, one has to overcome a number of calibration and mapping difficulties (see Zhang et al. 1991; Akujor et al. 1992, in prep.).

scholarly journals 5-GHz VLBI Imaging Observations of 7 Equatorial AGNs

2002 ◽  
Vol 184 ◽  
pp. 304-305
Author(s):  
Z.-Q. Shen ◽  
D. R. Jiang ◽  
Y.J. Chen ◽  
T.-S. Wan
Keyword(s):  
Radio Sources ◽  
Preliminary Results ◽  
The Third ◽  
5 Ghz

AbstractSince 1992 we have been conducting a 5-GHz VLBI imaging survey of southern and equatorial radio sources. So far, we have published the results of two observing sessions with 26 southern radio sources imaged in total (Shen et al. 1997; 1998). In this paper, we present the preliminary results of the third session of observations of 7 equatorial sources in the sample.

scholarly journals The follow-up European VLBI Network observations of twelve GPS radio sources at 5 GHz

2010 ◽  
Vol 518 ◽  
pp. A23 ◽  
Author(s):  
L. Cui ◽  
X. Liu ◽  
J. Liu ◽  
H.-G. Song ◽  
Z. Ding
Keyword(s):  
Radio Sources ◽  
5 Ghz
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