400 research outputs found
Far-infrared/millimetre emission in 3C sources - Dust in radio galaxies and quasars
We present far-infrared and millimetric observations of a sample of 3C objects. Millimetre data were taken at 1.25 mm with the IRAM 30 m antenna feeding the MPIfR bolometer array. Mid-infrared (MIR) and far-infrared (FIR) photometry were carried out with the ISOCAM and ISOPHOT cameras on the ISO Satellite. Additional FIR IRAS observations are also included. We present the entire Spectral Energy Distributions (SEDs) from the UV to radio and discuss the emitting mechanisms. Two composite spectra, one for the radio galaxies and one for the radio quasars, are built in the object rest frame. While the SEDs of the two classes differ, they are indistinguishable in the MIR and FIR range where they probably arise as thermal emission from a dusty torus and a larger-scale (cooler) dust distribution in the host galaxy.</p
rPICARD: A CASA-based Calibration Pipeline for VLBI Data
Currently, HOPS and AIPS are the primary choices for the time-consuming
process of (millimeter) Very Long Baseline Interferometry (VLBI) data
calibration. However, for a full end-to-end pipeline, they either lack the
ability to perform easily scriptable incremental calibration or do not provide
full control over the workflow with the ability to manipulate and edit
calibration solutions directly. The Common Astronomy Software Application
(CASA) offers all these abilities, together with a secure development future
and an intuitive Python interface, which is very attractive for young radio
astronomers. Inspired by the recent addition of a global fringe-fitter, the
capability to convert FITS-IDI files to measurement sets, and amplitude
calibration routines based on ANTAB metadata, we have developed the the
CASA-based Radboud PIpeline for the Calibration of high Angular Resolution Data
(rPICARD). The pipeline will be able to handle data from multiple arrays: EHT,
GMVA, VLBA and the EVN in the first release. Polarization and phase-referencing
calibration are supported and a spectral line mode will be added in the future.
The large bandwidths of future radio observatories ask for a scalable reduction
software. Within CASA, a message passing interface (MPI) implementation is used
for parallelization, reducing the total time needed for processing. The most
significant gain is obtained for the time-consuming fringe-fitting task where
each scan be processed in parallel.Comment: 6 pages, 1 figure, EVN 2018 symposium proceeding
ISOPHOT observations of 3CR quasars and radio galaxies
In order to check for consistency with the radio-loud AGN unification scheme, ISOPHOT data obtained for two small sets of intermediate redshift steep-spectrum 3CR radio galaxies and quasars are being examined. Supplementary submillimeter and centimeter radio data for the quasars are also taken into account, in order to assess the magnitude of any beamed nonthermal radiation. The fact that we find broad-lined objects to be somewhat more luminous in their far-infrared output than narrow-lined objects, hints at a contradiction to the unification scheme. However, as the sample objects are not particularly well matched, the sample size is small, and the FIR radiation may still be partly anisotropic, this evidence is, at the moment, weak
Broad-line radio galaxies: old and feeble?
Far-infrared photometry of broad-line radio galaxies shows this class of AGN
to consist of many hot and some cool infrared emitters, with peaks in their
spectral energy distributions around 25 micron or longward of 60 micron,
respectively. Quantitative analysis indicates that this distribution relates to
a substantial dispersion in the strength of the cool dust component: broad-line
radio galaxies are relatively poor in large-scale dust. Possibly they have
undergone a different merger evolution, or are relatively old AGN.Comment: Accepted for publication in A&A Letter
Infrared emission in radio galaxy NGC 4261
We have analyzed the total and nuclear SED for NGC 4261 and find that the
dominant process for the mid- and far-infrared emission in this object is
non-thermal emission from the active nucleus. Modeling the emission from the
optically detected 300 pc dust disk yields no significant disk contribution at
any wavelength. To explain the observations, either the disk has an inflated
inner region which partly absorbs the core, or the intrinsic core spectrum is
curved. The inner 10 pc of the disk can potentially be conceived as an
obscuring torus, albeit with optical depth around unity.Comment: 4 pages, 4 figures. To appear in the proceedings of: "The Spectral
Energy Distribution of Gas-Rich Galaxies: Confronting Models with Data",
Heidelberg, 4-8 Oct. 2004, eds. C.C. Popescu and R.J. Tuffs, AIP Conf. Ser.,
in pres
Spitzer Observations of 3C Quasars and Radio Galaxies: Mid-Infrared Properties of Powerful Radio Sources
We have measured mid-infrared radiation from an orientation-unbiased sample
of 3CRR galaxies and quasars at redshifts 0.4 < z < 1.2 with the IRS and MIPS
instruments on the Spitzer Space Telescope. Powerful emission (L_24micron >
10^22.4 W/Hz/sr) was detected from all but one of the sources. We fit the
Spitzer data as well as other measurements from the literature with synchrotron
and dust components. The IRS data provide powerful constraints on the fits. At
15 microns, quasars are typically four times brighter than radio galaxies with
the same isotropic radio power. Based on our fits, half of this difference can
be attributed to the presence of non-thermal emission in the quasars but not
the radio galaxies. The other half is consistent with dust absorption in the
radio galaxies but not the quasars. Fitted optical depths are anti-correlated
with core dominance, from which we infer an equatorial distribution of dust
around the central engine. The median optical depth at 9.7 microns for objects
with core-dominance factor R > 10^-2 is approximately 0.4; for objects with R <
10^-2, it is 1.1. We have thus addressed a long-standing question in the
unification of FR II quasars and galaxies: quasars are more luminous in the
mid-infrared than galaxies because of a combination of Doppler-boosted
synchrotron emission in quasars and extinction in galaxies, both
orientation-dependent effects.Comment: 42 pages, 14 figures plus two landscape tables. Accepted for
publication in Ap
The ISOPHOT-MAMBO survey of 3CR radio sources: Further evidence for the unified schemes
We present the complete set of ISOPHOT observations of 3CR radio galaxies and
quasars, which are contained in the ISO Data Archive, providing 75 mid- and
far-infrared spectral energy distributions (SEDs) between 5 and 200 micron. For
28 sources they are supplemented with MAMBO 1.2 mm observations and for 15
sources with new submillimetre data from the SCUBA archive.
We check the orientation-dependent unified scheme, in which the powerful FR2
narrow line galaxies are quasars viewed at high inclination, so that their
nuclei are hidden behind a dust torus intercepting the optical-ultraviolet AGN
radiation and reemitting it in the infrared. We find that (1) both the quasars
and the galaxies show a high mid- to far-infrared luminosity ratio typical for
powerful AGNs and (2) -- when matched in 178 MHz luminosity -- both show the
same ratio of isotropic far-infrared to isotropic 178 MHz lobe power.
Therefore, from our large sample investigated here we find strong evidence for
the orientation-dependent unification of the powerful FR2 galaxies with the
quasars.Comment: 16 pages, 7 figures, 3 tables, accepted by Astronomy & Astrophysic
Clumpy tori around active galactic nuclei
We discuss the question whether the matter in dusty tori around active
galactic nuclei has a smooth or a clumpy structure. Nenkova, Ivezic & Elitzur
(2002) have argued that the lack of emission feature in the SEDs of type 1 AGN
galaxies combined with a clear absorption feature in type 2 AGN can be
explained if the circumnuclear dust is distributed in discrete clumps. Our aim
is to verify this. We use multi-dimensional radiative transfer models of smooth
and clumpy tori, and compare the SEDs of equivalent smooth and clumpy models.
We find that the 10 micron emission feature of the clumpy models, when seen
almost face-on, is not appreciably reduced compared to the equivalent smooth
models. Some of the clumpy models have a weak or even absent 10 micron feature,
but so do some of the smooth models. On the whole the SEDs of clumpy and smooth
tori are similar, but some details are different. The absorption feature seen
at edge-on inclinations appears to be less deep in the clumpy models than in
the smooth models, and the average flux in the near-infrared regime is stronger
in the clumpy models. Moreover, at these inclinations the clumpy models have a
slightly wider SED. Whether these differences are unique enough to be used as a
diagnostic for clumpiness of AGN tori is not yet clear.Comment: Accepted for publication in Astronomy & Astrophysic
The Lockman Hole with LOFAR: Searching for GPS and CSS sources at low frequencies
The Lockman Hole Project is a wide international collaboration aimed at exploiting the multi-band extensive and deep information available for the Lockman Hole region, with the aim of better characterizing the physical and evolutionary properties of the various source populations detected in deep radio fields. Recent observations with the LOw-Frequency ARray (LOFAR) extends the multi-frequency radio information currently available for the Lockman Hole (from 350 MHz up to 15 GHz) down to 150 MHz, allowing us to explore a new radio spectral window for the faint radio source population. These LOFAR observations allow us to study the population of sources with spectral peaks at lower radio frequencies, providing insight into the evolution of GPS and CSS sources. In this general framework, I present preliminary results from 150 MHz LOFAR observations of the Lockman Hole field. <P /
Ionospheric Calibration of Low Frequency Radio Interferometric Observations using the Peeling Scheme: I. Method Description and First Results
Calibration of radio interferometric observations becomes increasingly
difficult towards lower frequencies. Below ~300 MHz, spatially variant
refractions and propagation delays of radio waves traveling through the
ionosphere cause phase rotations that can vary significantly with time, viewing
direction and antenna location. In this article we present a description and
first results of SPAM (Source Peeling and Atmospheric Modeling), a new
calibration method that attempts to iteratively solve and correct for
ionospheric phase errors. To model the ionosphere, we construct a time-variant,
2-dimensional phase screen at fixed height above the Earth's surface. Spatial
variations are described by a truncated set of discrete Karhunen-Loeve base
functions, optimized for an assumed power-law spectral density of free
electrons density fluctuations, and a given configuration of calibrator sources
and antenna locations. The model is constrained using antenna-based gain phases
from individual self-calibrations on the available bright sources in the
field-of-view. Application of SPAM on three test cases, a simulated visibility
data set and two selected 74 MHz VLA data sets, yields significant improvements
in image background noise (5-75 percent reduction) and source peak fluxes (up
to 25 percent increase) as compared to the existing self-calibration and
field-based calibration methods, which indicates a significant improvement in
ionospheric phase calibration accuracy.Comment: 23 pages, 14 figures, 2 tables. Accepted for publication in A&A.
Changes in v2: Corrected minor error in Equations A.3 and A.12. Extended
acknowledgment
- …