Mon. Not. R. Astron. Soc., 398, 176-188 (2009/September-1)
High-redshift obscured quasars: radio emission at sub-kiloparsec scales.
KLOCKNER H.-R., MARTINEZ-SANSIGRE A., RAWLINGS S. and GARRETT M.A.
Abstract (from CDS):
The radio properties of 11 obscured `radio-intermediate' quasars at redshifts z ≳ 2 have been investigated using the European Very-Long-Baseline-Interferometry Network (EVN) at 1.66 GHz. A sensitivity of ∼25µJy per 17x14mas2beam was achieved, and in seven out of 11 sources unresolved radio emission was securely detected. The detected radio emission of each source accounts for ∼30-100 per cent of the total source flux density. The physical extent of this emission is ≲ 150pc, and the derived properties indicate that this emission originates from an active galactic nucleus (AGN). The missing flux density is difficult to account for by star formation alone, so radio components associated with jets of physical size ≳150pcand ≲40 kpc are likely to be present in most of the sources. Amongst the observed sample steep, flat, gigahertz-peaked and compact-steep spectrum sources are all present. Hence, as well as extended and compact jets, examples of beamed jets are also inferred, suggesting that in these sources, the obscuration must be due to dust in the host galaxy, rather than the torus invoked by the unified schemes. Comparing the total to core (≲150pc) radio luminosities of this sample with different types of AGN suggests that this sample of z ≳ 2 radio-intermediate obscured quasars shows radio properties that are more similar to those of the high-radio-luminosity end of the low-redshift radio-quiet quasar population than those of Fanaroff-Riley type I (FRI) radio galaxies. This conclusion may reflect intrinsic differences, but could be strongly influenced by the increasing effect of inverse-Compton cooling of extended radio jets at high redshift.
© 2009 The Authors. Journal compilation © 2009 RAS
techniques: interferometric - galaxies: active - galaxies: nuclei - quasars: general - radio continuum: galaxies
J2005+7702 and J2205+7752 not identified (may be erroneous identification for J2005+7752 = JVAS J2005+7752)
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