NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-04-19 T14:00:12 PDT
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For refcode 1995AJ....109.2318C:
Retrieve 403 NED objects in this reference.
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1995AJ....109.2318C RADIO IDENTIFICATIONS OF EXTRAGALACTIC IRAS SOURCES J. J. CONDON AND E. ANDERSON National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, Virginia 22903; Electronic mail: jcondon@nrao.edu, eanderso@nrao.edu J. J. BRODERICK Department of Physics, Virginia Polytechnic Institute and State University, Blacksburg, Virginia 24061 Electronic mail: jjb@vtpcn.phys.vt.edu Received 1995 January 4; revised 1995 February 14 ABSTRACT Extragalactic sources detected at {lambda}= 60 microns were selected from the IRAS Faint Source Catalog, Version 2 by the criterion S_60 microns_ >= S_12_ microns. They were identified by position coincidence with radio sources stronger than 25 mJy at 4.85 GHz in the 6.0 sr declination band 0^deg^ < {delta} < +75^deg^ (excluding the 0.05 sr region 12^h^40^m^< {alpha} < 14^h^40^m^, 0^deg^< +5^deg^) and with radio sources stronger than 80 mJy in the 3.4 sr area o^h^ <{alpha} < 2o^h^, -40^deg^ < {delta} < 0^deg^ (plus the region 12^h^40^m^ < {alpha} < 14^h^40^m^, 0^deg^<{delta} <+5^deg^). Fields containing new candidate identifications were mapped by the VLA at 4.86 GHz with about 15" FWHM resolution. Difficult cases were confirmed or rejected with the aid of accurate ({sigma} ~ 1") radio and optical positions. The final sample of 354 identifications in {OMEGA} = 9.4 sr is reliable and large enough to contain statistically useful numbers of radio-loud FIR galaxies and quasars. The logarithmic FIR radio flux ratio parameter q can be used to distinguish radio sources powered by "starbursts" from those powered by "monsters." Starbursts and normal spiral galaxies in a {lambda} = 60 micron flux-limited sample have a narrow ({sigma}_q_ = 0.14 +/- 0.01) q distribution with mean <q> = 2.74 +/- 0.01, and none have "warm" FIR spectra [{alpha}(25 microns, 60 microns) < 1.5]. The absence of radio- quiet (but not completely silent) blazars indicates that nearly all blazars become optically thin at frequencies v<~100 GHz. Nonthermal sources with steep FIR/optical spectra and dusty-embedded sources visible only at FIR and radio wavelengths must be very rare.
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