26 research outputs found
Multi-frequency VLBI observations of faint gigahertz peaked spectrum sources
We present the data and analysis of VLBI observations at 1.6, 5 and 15 GHz of
a sample of faint Gigahertz Peaked Spectrum (GPS) sources selected from the
Westerbork Northern Sky Survey (WENSS). The 5 GHz observations involved a
global array of 16 stations and yielded data on the total sample of 47 sources.
A subsample of 26 GPS sources with peak frequencies > 5 GHz and/or peak flux
densities > 125 mJy was observed with the VLBA at 15 GHz. A second subsample of
29 sources, with peak frequencies <5 GHz, was observed at 1.6 GHz using a 14
station global VLBI array. In this way, 44 of the 47 sources (94%) in the
sample were observed above and at or below their spectral peak. Spectral
decomposition allowed us to identify 3, 11, 7, and 2 objects as compact
symmetric objects, compact doubles, core-jet and complex sources respectively.
However, many of the sources classified as compact double or core-jet sources
show only two components making their classification rather tentative. This may
explain why the strong morphological dichotomy of GPS quasars and galaxies
found for radio-bright GPS sources, is not as clear in this faint sample.Comment: Latex, 18 pages, 8 figures; MNRAS, accepted. The paper, with higher
quality figures, may also be obtained from http://www.ast.cam.ac.uk/~snellen
. Minor comments of referee incorporate
On the evolution of young radio-loud AGN
This paper describes an investigation of the early evolution of extragalactic
radio sources using samples of faint and bright Gigahertz Peaked Spectrum (GPS)
and Compact Steep Spectrum (CSS) radio galaxies. Correlations found between
their peak frequency, peak flux density and angular size provide strong
evidence that synchrotron self absorption is the cause of the spectral
turnovers, and indicate that young radio sources evolve in a self-similar way.
In addition, the data seem to suggest that the sources are in equipartition
while they evolve. If GPS sources evolve to large size radio sources, their
redshift dependent birth-functions should be the same. Therefore, since the
lifetimes of radio sources are thought to be short compared to the Hubble time,
the observed difference in redshift distribution between GPS and large size
sources must be due to a difference in slope of their luminosity functions. We
argue that this slope is strongly affected by the luminosity evolution of the
individual sources. A scenario for the luminosity evolution is proposed in
which GPS sources increase in luminosity and large scale radio sources decrease
in luminosity with time. This evolution scenario is expected for a ram-pressure
confined radio source in a surrounding medium with a King profile density. In
the inner parts of the King profile, the density of the medium is constant and
the radio source builds up its luminosity, but after it grows large enough the
density of th e surrounding medium declines and the luminosity of the radio
source decreases. A comparison of the local luminosity function (LLF) of GPS
galaxies with that of extended sources is a good test for this evolution
scenario [abridged].Comment: LaTeX, 11 pages, 8 figures; Accepted by MNRAS. Related papers may be
found at http://www.ast.cam.ac.uk/~snellen . Valuable comments of referee
incorporated. More discussion on simulation
The X-ray properties of young radio-loud AGN
We present XMM-Newton observations of a complete sample of five archetypal
young radio-loud AGN, also known Gigahertz Peaked Spectrum (GPS) sources. They
are among the brightest and best studied GPS/CSO sources in the sky, with radio
powers in the range L_{5GHz}=10^{43-44} erg/s and with 4 sources having
measured kinematic ages of 570 to 3000 yrs. All sources are detected, and have
2-10 keV luminosities from 0.5 to 4.8x10^{44} erg/s. In comparison with the
general population of radio galaxies, we find that: 1) GPS galaxies show a a
range in absorption column densities similar to other radio galaxies. We
therefore find no evidence that GPS galaxies reside in significantly more dense
circumnuclear environment, such that they could be hampered in their expansion.
2) The ratio of radio to X-ray luminosity is significantly higher than for
classical radio sources. This is consistent with an evolution scenario in which
young radio sources are more efficient radio emitters than large extended
objects at a constant accretion power. 3) Taking the X-ray luminosity of radio
sources as a measure of ionisation power, we find that GPS galaxies are
significantly underluminous in their [OIII]_{5007 Angstrom}, including a weak
trend with age. This is consistent with the fact that the Stroemgren sphere
should still be expanding in these young objects. This would mean that here we
are witnessing the birth of the narrow line region of radio-loud AGN.Comment: 11 pages, 6 figures. Accepted for publication by the MNRA
On the lives of extra-galactic radio sources: the first 100,000 years
In this paper we discuss the early phase of radio source evolution as
represented by Gigahertz Peaked Spectrum (GPS) and Compact Steep Spectrum (CSS)
radio sources. Correlations between their spectral peak and angular size
strongly suggest that the spectral turnovers are caused by synchrotron self
absorption, and indicate that young radio sources evolve in a self similar way.
We argue that the evolution of a radio source during its first 10^5 years is
qualitatively very different from that during the rest of its life-time. This
may be caused by the difference in the density gradient of the intra-galactic
medium inside and outside the core-radius of the host galaxy.Comment: LaTeX, 7 pages & 2 figs. Invited talk at `Lifecycles of Radio
Galaxies' workshop, ed J. Biretta et al., New Astronomy Reviews. More papers
of the authors at http://www.ast.cam.ac.uk/~snelle
Parsec-scale radio structures in the nuclei of four Seyfert galaxies
We present 18-cm radio maps of four Seyfert nuclei, Mrk 1, Mrk 3, Mrk 231 and
Mrk 463E, made with the European VLBI Network (EVN). Linear radio structures
are present in three out of four sources on scales of ~100 pc to ~1 kpc, and
the 20-mas beam of the EVN enables us to resolve details within the radio
structures on scales of <10 pc. Mrk 3 was also imaged using MERLIN and the data
combined with the EVN data to improve the sensitivity to extended emission. We
find an unresolved flat-spectrum core in Mrk 3, which we identify with the
hidden Seyfert 1 nucleus in this object, and we also see marked differences
between the two highly-collimated radio jets emanating from the core. The
western jet terminates in a bright hotspot and resembles an FRII radio
structure, whilst the eastern jet has more in common with an FRI source. In Mrk
463E, we use the radio and optical structure of the source to argue that the
true nucleus lies approximately 1 arcsec south of the position of the radio and
optical brightness peaks, which probably represent a hotspot at the working
surface of a radio jet. The EVN data also provide new evidence for a 100-pc
radio jet powering the radio source in the Type 1 nucleus of Mrk 231. However,
the Seyfert 2 galaxy Mrk 1 shows no evidence for radio jets down to the limits
of resolution (~10 pc). We discuss the range of radio source size and
morphology which can occur in the nuclei of Seyfert galaxies and the
implications for Seyfert unification schemes and for radio surveys of large
samples of objects.Comment: 23 pages, 7 postscript figures (supplied as separate files), uses AAS
aaspp4 LaTeX style file, to appear in the 10 June 1999 issue of The
Astrophysical Journa
A very brief description of LOFAR - the Low Frequency Array
LOFAR (Low Frequency Array) is an innovative radio telescope optimized for
the frequency range 30-240 MHz. The telescope is realized as a phased aperture
array without any moving parts. Digital beam forming allows the telescope to
point to any part of the sky within a second. Transient buffering makes
retrospective imaging of explosive short-term events possible. The scientific
focus of LOFAR will initially be on four key science projects (KSPs): 1)
detection of the formation of the very first stars and galaxies in the universe
during the so-called epoch of reionization by measuring the power spectrum of
the neutral hydrogen 21-cm line (Shaver et al. 1999) on the ~5' scale; 2)
low-frequency surveys of the sky with of order expected new sources; 3)
all-sky monitoring and detection of transient radio sources such as gamma-ray
bursts, x-ray binaries, and exo-planets (Farrell et al. 2004); and 4) radio
detection of ultra-high energy cosmic rays and neutrinos (Falcke & Gorham 2003)
allowing for the first time access to particles beyond 10^21 eV (Scholten et
al. 2006). Apart from the KSPs open access for smaller projects is also
planned. Here we give a brief description of the telescope.Comment: 2 pages, IAU GA 2006, Highlights of Astronomy, Volume 14, K.A. van
der Hucht, e