The MOJAVE Survey

Minimum credit line: Image courtesy of NRAO/AUI and Matthew Lister (Purdue University) and the MOJAVE Team(for details, see Image Use Policy).

About this Image

MOJAVE (Monitoring of Jets in AGN with VLBA Experiments) is a program to regularly image the changing structures of the brightest 133 active galactic nuclei (AGN) in the northern sky with the VLBA. The smallest details in this montage have angular scales of just under 1 milliarcsecond (several hundred times finer resolution than the Hubble space telescope). The false-color scheme corresponds to radio brightness at a wavelength of 2 cm, with yellow being the strongest, and blue being the weakest. Each image shows the synchrotron emission from a relativistic, jetted outflow that is launched in the vicinity of a supermassive black hole. The jets in the MOJAVE sample are located at distances ranging from 50 million to 5 billion light years, and are among the most powerful known phenomena in the Universe. The name of each object is given at the top left corner of each panel, and the date of the observation is given in the lower right-hand corner.

Investigator(s):  Matthew Lister

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Technical Data

    Telescope VLBA 
    Type of Observation Continuum Observations 
    Band U 
    Wavelength 2.0 cm 
    Frequency 15 GHz 
    Center of Image RA: 01:01:1.00, Dec: 01:01:1.00 (J2000)  
    Technical Caption The MOJAVE sample consists of all AGN with J2000 declination > -20 deg., galactic latitude |b| > 2.5 deg. and 2 cm correlated VLBA flux > 1.5 Jy (or 2 Jy, for sources with dec < 0 deg.) at any epoch between 1994-2003. The 2 cm total intensity images shown here were obtained using all 10 antennas of the VLBA in continuum, full polarization mode with 32 MHz total bandwidth. The ticks on each panel are drawn at intervals of 1 milliarcsecond. The total integration time on each source was approximately 60 minutes, spread out in several scans over a wide range of hour angle. Each panel is labelled with the B1950 name of the radio source and the observation epoch. For further details on the observations see Lister M. L., and Homan, D.C., 2005, AJ, (in press).  

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