Identifications and redshifts of faint 3CR radio sources

Creators: Djorgovski, S.; Spinrad, H.; McCarthy, P.; Dickinson, M.; van Breugel, W.; Strom, R. G.

Abstract

We report new and confirmed optical identifications of 12 3CR radio sources, and redshifts for nine of them. Seven have redshifts in excess of 1, with the highest being 1.841 for 3C 454.1; the remaining three sources are also likely to be at z > 1. One of the newly identified sources, 3C 194, shows a moderately strong Lyα emission, and may be a member of the new class of objects, possible young/forming galaxies, typified by 3C 326.1 and 3C 294. The optical identifications of the 3CR sources are now complete, and only six are lacking redshifts. Practically all of the new identifications are galaxies whose light appears to be dominated by stars, rather than nonthermal active nuclei, although their powerful radio emission argues that they are likely to be highly unusual objects. Their observed properties are similar to those of previously identified high-redshift powerful radio galaxies.

Additional Information

© 1988 American Astronomical Society. Provided by the NASA Astrophysics Data System. Received 2 May 1988. Based in part on the data obtained at Lick Observatory, University of California, and the Multiple Mirror Telescope Observatory, a joint facility of the Smithsonian Institution and University of Arizona. We are very grateful to the staffs of Kitt Peak, Lick, MMT, CFHT, VLA, and Cerro Tololo observatories, without whose expertise and help this work would not have been possible. We thank Arnold Klemola for his generous assistance with the Lick astrometric machine, and Michael Strauss and Susan Tokarz for help in reducing the spectroscopic data. We are also indebted to several of our colleagues, and in particular to James Douglas, Tim Heckman, Robert Laing, Frazer Owen, Larry Rudnick, and Derek and Beverly Wills for communicating unpublished radio positions. The WSRT is operated by the Netherlands Foundation for Radio Astronomy with the financial support of the Netherlands Organisation for Scientific Research (NWO). Part of this work was done while S. D. was at Harvard University, and partial financial support from there is gratefully acknowledged. This work was supported in part by the NSF grants nos. AST85-13416 and AST84-16177, and by the California Institute of Technology.

Attached Files

Published - 1988AJ_____96__836D.pdf

Files

1988AJ_____96__836D.pdf

Files (1.3 MB)

Name	Size	Download all
1988AJ_____96__836D.pdf md5:e7a737bdfad9b4b746f54c3c534f111a	1.3 MB	Preview Download

Additional details

	All versions	This version
Views	0	0
Downloads	0	0
Data volume	0 Bytes	0 Bytes