150 research outputs found
HST imaging of redshift z>0.5 7C and 3C Quasars
We present preliminary results from HST imaging of radio-loud quasar hosts,
covering a ~x100 range in radio luminosity but in a narrow redshift range (0.5
to 0.65). The sample was selected from our new, spectroscopically complete 7C
survey and the 3CRR catalogue. Despite the very large radio luminosity range,
the host luminosities are only weakly correlated (if at all) with radio power,
perhaps reflecting a predominance of purely central engine processes in the
formation of radio jets, and hence perhaps also in the radio-loud/-quiet
dichotomy at these redshifts. The results also contradict naive expectations
from several quasar formation theories, but the host magnitudes support
radio-loud Unified Schemes.Comment: To appear in the Proceedings of the ESO/IAC Conference on 'Quasar
Hosts' - Tenerife 24-27 September 199
IRAS F10214+4724: the inner 100pc
We use new near-infrared spectroscopy and our published optical spectroscopy
of the gravitationally-lensed Seyfert-2 galaxy F10214+4724 to study both the
links between the starburst and AGN in this object and the properties of the
inner narrow-line clouds. The UV spectrum is consistent with a compact,
moderately- reddened starburst providing about half the UV light. Spectroscopy
of the Halpha /[NII] line blend has enabled us to distinguish emission from the
narrow-line region of the Seyfert-2 and a moderately-reddened emission line
region which we argue is associated with the starburst. Estimates of the star
formation rate from the UV continuum flux and the Halpha flux are broadly
consistent. We can explain the unusual emission line properties of F10214+4724
in terms of conventional models for nearby Seyfert-2 galaxies if lensing is
preferentially magnifying the side of the inner narrow-line region between the
AGN and the observer, and the other side is both less magnified and partially
obscured by the torus. The hydrogen densities of clouds in this region are high
enough to make the Balmer lines optically thick and to suppress forbidden
emission lines with low critical densities. We have deduced the column density
of both ionised and neutral gas in the narrow-line clouds, and the density of
the ionised gas. Using these we have been able to estimate the mass of the
inner narrow-line clouds to be ~ 1 solar mass, and show that the gas:dust ratio
NH/E(B-V) in these clouds must be ~1.3x10^{27}m^{-2}mag^{-1}, significantly
higher than in the Milky Way. The cloud properties are consistent with the
those of the warm absorbers seen in the X-ray spectra of Seyfert-1 galaxies.
Our results favour models in which narrow-line clouds start close to the
nucleus and flow out.Comment: 13 pages, 5 figures. Accepted by MNRA
Thermal-infrared imaging of 3C radio galaxies at z~1
We present the results of a programme of thermal-IR imaging of nineteen z~1
radio galaxies from the 3CR and 3CRR samples. We detect emission at L' (3.8um)
from four objects; in each case the emission is unresolved at 1" resolution.
Fifteen radio galaxies remain undetected to sensitive limits of L'~15.5. Using
these data in tandem with archived HST data and near-IR spectroscopy we show
that 3 of the detected `radio galaxies' (3C22, 3C41, and 3C65) harbour quasars
reddened by Av<5. Correcting for this reddening 3C22 and 3C41 are very similar
to coeval 3C quasars, whilst 3C65 seems unusually underluminous. The fourth
radio galaxy detection (3C265) is a more highly obscured (Av~15) but otherwise
typical quasar which previously has been evident only in scattered light. We
determine the fraction of dust-reddened quasars at z~1 to be 28(+25)(-13)% at
90% confidence. On the assumption that the undetected radio galaxies harbour
quasars similar to those in 3C22, 3C41 and 3C265 (as seems reasonable given
their similar narrow emission line luminosities) we deduce extinctions of Av>15
towards their nuclei. The contributions of reddened quasar nuclei to the total
K-band light ranges from ~0 per cent for the non-detections, through ~10 per
cent for 3C265 to ~80 per cent for 3C22 and 3C41. Correcting for these effects
does not remove the previously reported differences between the K magnitudes of
3C and 6C radio galaxies, so contamination by reddened quasar nuclei is not a
serious problem for drawing cosmological conclusions from the K-z relation for
radio galaxies. We discuss these results in the context of the `receding torus'
model which predicts a small fraction of lightly-reddened quasars in samples of
high radio luminosity sources. We also examine the likely future importance of
thermal-IR imaging in the study of distant powerful radio sources.Comment: 17 pages incl 14 figures, accepted by MNRA
Searches for galaxies at z > 4 through Lyman-limit imaging
We present preliminary results of a search for galaxies at z>4 through
Lyman-limit imaging of the fields of known high-redshift radio-galaxies.
Objects were selected by means of their broad-band colours, and spectroscopy of
candidate objects in one of the fields has been performed through multi-slit
spectroscopy at the 4.2m William Herschel Telescope. These spectra show some of
the first z>4 galaxies to be identified using the Lyman break technique.Comment: 4 pages, LaTeX, requires paspconf.sty (included). To appear in
Proceedings of "The Young Universe", Rome Observatory, Sep 29 - Oct 3 199
Steve Lacy Workshop
Steve Lacy Workshop
Razzo Hall, Traina Center
2001https://commons.clarku.edu/vpae/1040/thumbnail.jp
A sample of 6C radio sources with virtually complete redshifts. II - optical spectroscopy
This is the second of two papers presenting basic observational data on the
6CE sample of extragalactic radio sources. It presents the results of optical
spectroscopy which has yielded virtually complete redshift information for the
6CE sample: 56 of the 59 sample members have spectroscopic redshifts which,
with the exception of seven cases, are secure. The redshift distribution N(z)
is fairly flat over the redshift range 0 < z < 2, with a median redshift of 1.1
and a high-redshift tail reaching to z = 3.4. The highest-redshift (z > 1.75)
members of the 6CE sample have similar optical spectra and a tight (less than
one dex) spread in narrow-Lyalpha emission line luminosity.Comment: 18 pages, 4 figures, accepted for publication in MNRA
No evidence for a `redshift cut-off' for the most powerful classical double radio sources
We use three samples (3CRR, 6CE and 6C*) to investigate the radio luminosity
function (RLF) for the `most powerful' low-frequency selected radio sources. We
find that the data are well fitted by a model with a constant co-moving space
density at high redshift as well as by one with a declining co-moving space
density above some particular redshift. This behaviour is very similar to that
inferred for steep-spectrum radio quasars by Willott et al (1998) in line with
the expectations of Unified Schemes. We conclude that there is as yet no
evidence for a `redshift cut-off' in the co-moving space densities of powerful
classical double radio sources, and rule out a cut-off at z < 2.5.Comment: To appear in `The Hy-redshift universe: Galaxy formation and
evolution at high redshift' eds. A.J. Bunker and W.J.M. van Breuge
The emission line - radio correlation for radio sources using the 7C Redshift Survey
We have used narrow emission line data from the new 7C Redshift Survey to
investigate correlations between the narrow-line luminosities and the radio
properties of radio galaxies and steep-spectrum quasars. The 7C Redshift Survey
is a low-frequency (151 MHz) selected sample with a flux-density limit about
25-times fainter than the 3CRR sample. By combining these samples, we can for
the first time distinguish whether the correlations present are controlled by
151 MHz radio luminosity L_151 or redshift z. We find unequivocal evidence that
the dominant effect is a strong positive correlation between narrow line
luminosity L_NLR and L_151, of the form L_NLR proportional to L_151 ^ 0.79 +/-
0.04. Correlations of L_NLR with redshift or radio properties, such as linear
size or 151 MHz (rest-frame) spectral index, are either much weaker or absent.
We use simple assumptions to estimate the total bulk kinetic power Q of the
jets in FRII radio sources, and confirm the underlying proportionality between
jet power and narrow line luminosity first discussed by Rawlings & Saunders
(1991). We make the assumption that the main energy input to the narrow line
region is photoionisation by the quasar accretion disc, and relate Q to the
disc luminosity, Q_phot. We find that 0.05 < Q / Q_phot < 1 so that the jet
power is within about an order of magnitude of the accretion disc luminosity.
The most powerful radio sources are accreting at rates close to the Eddington
limit of supermassive black holes (~ 10^9 - 10^10 solar masses), whilst lower
power sources are accreting at sub-Eddington rates.Comment: 20 pages, 7 figures, to be published in MNRA
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