Other
Scientific paper
Feb 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aj....109..486o&link_type=abstract
Astronomical Journal (ISSN 0004-6256), vol. 109, no. 2, p. 486-499
Other
7
Faint Objects, Galactic Evolution, Luminosity, Radio Galaxies, Astronomical Photography, Astronomical Spectroscopy, Line Spectra, Radial Velocity, Radio Emission, Radio Observation, Red Shift, Star Formation
Scientific paper
We present results from radio imaging and optical imaging and spectroscopic studies of a sample of 12 sources taken from the B3 radio survey, covering sources with lower radio flux than hitherto available. Redshifts are reported for 9 of the 12 objects, 8 of them in the range z = 0.6 - 1.0. For the objects with measured redshifts, we have calculated absolute parameters for the radio emission and the optical line and broadband emission. These parameters are generally consistent with the ranges observed for radio galaxies of similar radio luminosity at lower redshifts. Thus little evidence exists from these data for dramatic changes in properties connected to the radio source or line emission between the present epoch and redshifts of about unity. We do see systematically weaker 4000 A continuum breaks than at lower redshifts, in accord with the level of passive evolution expected for old stellar systems (perhaps with some star formation continuing to z approximately 1). One exception to this overlap with properties of nearby galaxies is 0213+392 which has a large velocity gradient and extended (Ne V) lambda 3426 as well as (O II) lambda 3727 emission. This is best accounted for by either anisotropic ionizing radiation or scattering of a bright central emission region, perhaps from material with significant radial motion. Association with the radio plasma is rendered unlikely by the 70 deg offset between optical and radio elongations in this galaxy (which thus furnishes a dramatic counterexample to the general alignment effect). One galaxy, B3 1156+389, is found in a tight group or cluster or projected dimensions approximately 200 kpc. The other apparent members share similar (R-J) or (R-K) colors, strengthening the case for association at z = 0.955.
Keel William C.
Owen Frazer N.
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