The University of Michigan radio astronomy data base. I - Structure function analysis and the relation between BL Lacertae objects and quasi-stellar objects

1992 ◽  
Vol 396 ◽  
pp. 469 ◽  
Author(s):  
P. A. Hughes ◽  
H. D. Aller ◽  
M. F. Aller
Keyword(s):  
Structure Function ◽  
Data Base ◽  
Radio Astronomy ◽  
Function Analysis ◽  
University Of Michigan ◽  
Bl Lacertae Objects ◽  
Stellar Objects ◽  
Bl Lacertae ◽  
Quasi Stellar Objects ◽  
The University

Absorption by neutral hydrogen and ionized magnesium in quasi-stellar objects and BL Lacertae objects

1977 ◽  
Vol 218 ◽  
pp. 605 ◽  
Author(s):  
B. M. Peterson ◽  
P. A. Strittmatter ◽  
R. E. Williams ◽  
G. D. Coleman
Keyword(s):  
Neutral Hydrogen ◽  
Bl Lacertae Objects ◽  
Stellar Objects ◽  
Ionized Magnesium ◽  
Bl Lacertae ◽  
Quasi Stellar Objects

scholarly journals The Recent Highly-Polarized Centimeter Burst in BL Lacertae

1998 ◽  
Vol 164 ◽  
pp. 167-168
Author(s):  
H. D. Aller ◽  
P. A. Hughes ◽  
M. F. Aller
Keyword(s):  
Position Angle ◽  
University Of Michigan ◽  
Conical Flow ◽  
Bl Lacertae ◽  
The University

AbstractObservations with the University of Michigan 26-meter paraboloid at 4.8, 8.0, and 14.5 GHz have been used to test generic shock-based models of the emitting region of BL Lacertae. Large changes in the polarization position angle since 1980 are not consistent with a jet with a simple conical flow.

scholarly journals Radio variability properties for sources at multi-frequencies

2007 ◽  
Vol 3 (S245) ◽  
pp. 251-252
Author(s):  
Y. Liu ◽  
J. H. Fan ◽  
H. G. Wang
Keyword(s):  
Time Series ◽  
Radio Astronomy ◽  
Power Spectral Analysis ◽  
Light Curves ◽  
University Of Michigan ◽  
Astronomy Observatory ◽  
Period Analysis ◽  
Radio Astronomy Observatory ◽  
Power Spectral ◽  
The University

AbstractUsing three radio databases of the university of Michigan Radio Astronomy Observatory (UMRAO), the National Radio Astronomy Observatory (NRAO), and the Metsähovi Observatory, we analyzed the radio light curves by the power spectral analysis and CLEANest method in search for possible periodicity. Multiple periods are found in some sources at multi-frequencies. We adopted the wavelets for period analysis of unevenly sampled time series to search for the evolution of the parameters (period, amplitude) of possible periodicities. Some possible variation of these parameters are found.

scholarly journals Brightness temperature for radio sources

2007 ◽  
Vol 3 (S245) ◽  
pp. 245-246
Author(s):  
J. H. Fan ◽  
Y. Huang ◽  
Y. Liu ◽  
Y. Gao ◽  
T. X. Hua ◽  
...  
Keyword(s):  
Brightness Temperature ◽  
Radio Astronomy ◽  
Radio Sources ◽  
University Of Michigan ◽  
Astronomy Observatory ◽  
Radio Astronomy Observatory ◽  
Brightness Temperatures ◽  
The University

AbstractIn this work, using the database of the university of Michigan Radio Astronomy Observatory (UMRAO), we determined the brightness temperatures, TB for a sample of 167 radio sources. The value of TB is in a range of log TB(K) = 10.46 to 20.08, which suggested that the boosting factors are in a range of δ = 0.41 to 41.26.

Novae in the Magellanic Clouds

1979 ◽  
Vol 46 ◽  
pp. 96-101
Author(s):  
J.A. Graham
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
University Of Michigan ◽  
The Past ◽  
Spectroscopic Information ◽  
Objective Prism ◽  
The University ◽  
Small Cloud ◽  
Low Dispersion

During the past several years, a systematic search for novae in the Magellanic Clouds has been carried out at Cerro Tololo Inter-American Observatory. The Curtis Schmidt telescope, on loan to CTIO from the University of Michigan is used to obtain plates every two weeks during the observing season. An objective prism is used on the telescope. This provides additional low-dispersion spectroscopic information when a nova is discovered. The plates cover an area of 5°x5°. One plate is sufficient to cover the Small Magellanic Cloud and four are taken of the Large Magellanic Cloud with an overlap so that the central bar is included on each plate. The methods used in the search have been described by Graham and Araya (1971). In the CTIO survey, 8 novae have been discovered in the Large Cloud but none in the Small Cloud. The survey was not carried out in 1974 or 1976. During 1974, one nova was discovered in the Small Cloud by MacConnell and Sanduleak (1974).

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