126 research outputs found
Measurement of the Integrated Faraday Rotations of BL Lac Objects
We present the results of multi-frequency polarization VLA observations of
radio sources from the complete sample of northern, radio-bright BL Lac objects
compiled by H. Kuhr and G. Schmidt. These were used to determine the integrated
rotation measures of 18 objects, 15 of which had never been measured
previously, which hindered analysis of the intrinsic polarization properties of
objects in the complete sample. These measurements make it possible to correct
the observed orientations of the linear polarizations of these sources for the
effect of Faraday rotation. The most probable origin for Faraday rotation in
these objects is the Galactic interstellar medium. The results presented
complete measurements of the integrated rotation measures for all 34 sources in
the complete sample of BL Lac objects.Comment: 9 pages, 7 figure
Absolute kinematics of radio source components in the complete S5 polar cap sample. III. First wide-field high-precision astrometry at 15.4 GHz
We report on the first wide-field, high-precision astrometric analysis of the
13 extragalactic radio sources of the complete S5 polar cap sample at 15.4 GHz.
We describe new algorithms developed to enable the use of differenced phase
delays in wide-field astrometric observations and discuss the impact of using
differenced phase delays on the precision of the wide-field astrometric
analysis. From this global fit, we obtained estimates of the relative source
positions with precisions ranging from 14 to 200 as at 15.4 GHz, depending
on the angular separation of the sources (from 1.6 to 20.8
degrees). These precisions are 10 times higher than the achievable
precisions using the phase-reference mapping technique.Comment: 9 pages, 7 figure
The BL Lac objects OQ 530 and S5 0716+714. Simultaneous observations in the X-rays, radio, optical and TeV bands
We present the results of the BeppoSAX observations of two BL Lacs, OQ 530
and S5 0716+714, as part of a ToO program for the simultaneous observation at
radio, optical, X-ray and TeV energies. Both sources are detected in the LECS
and MECS, with S5 0716+714 visible also in the PDS band, up to about 60 keV.
The X-ray spectra of both sources are better fitted by a double power-law
model, with a steep soft X-ray component flattening at harder energies, with
breaks at 0.3 and 1.5 keV, respectively. The concave shape of the spectra in
both objects is consistent with soft X-rays being produced by the synchrotron
and harder X-rays by the inverse Compton processes. Also the X-ray variability
properties confirm this scenario, in particular for S5 0716+714 our observation
shows variations by about a factor 3 over one hour below 3 keV and no
variability above. Their simultaneous broad band energy spectral distributions
can be successfully interpreted within the frame of a homogeneous synchrotron
and inverse Compton model, including a possible contribution from an external
source of seed photons with the different spectral states of S5 0716+714 being
reproduced by changing the injected power. The resulting parameters are fully
consistent with the two sources being intermediate objects within the
"sequence" scenario proposed for blazars.Comment: 10 pages, 8 figures, accepted by A&
Spectral energy distributions of a large sample of BL Lacertae objects
We have collected a large amount of multifrequency data for the objects in
the Metsahovi Radio Observatory BL Lacertae sample and computed their spectral
energy distributions (SED). This is the first time the SEDs of BL Lacs have
been studied with a sample of over 300 objects. The synchrotron components of
the SEDs were fitted with a parabolic function to determine the synchrotron
peak frequency. We checked the dependence between luminosities at several
frequency bands and synchrotron peak frequency to test the blazar sequence
scenario, which states that the source luminosity depends on the location of
the synchrotron peak. We also calculated broad band spectral indices and
plotted them against each other and the peak frequency. The range of peak
frequencies in our study was considerably extended compared to previous
studies. There were 22 objects for which log\nu_{peak}>19. The data shows that
at 5 GHz, 37 GHz and 5500 A there is negative correlation between luminosity
and nu_{peak}. There is no significant correlation between source luminosity at
synchrotron peak and peak frequency. Several low radio luminosity-low energy
peaked BL Lacs were found. The negative correlation between broad band spectral
indices and nu_{peak} is also significant, although there is substantial
scatter. Therefore we find that neither alpha_{rx} nor alpha_{ro} can be used
to determine the synchrotron peak of BL Lacs. On the grounds of our results we
conclude that the blazar sequence scenario is not valid. In all our results the
BL Lac population is continuous with no hint of the bimodality of the first BL
Lac samples.Comment: 10 + 27 pages, 13 figures, accepted to A&
On the coherence loss in phase-referenced VLBI observations
Context: Phase referencing is a standard calibration technique in radio
interferometry, particularly suited for the detection of weak sources close to
the sensitivity limits of the interferometers. However, effects from a changing
atmosphere and inaccuracies in the correlator model may affect the
phase-referenced images, leading to wrong estimates of source flux densities
and positions. A systematic observational study of signal decoherence in phase
referencing, and its effects in the image plane, has not been performed yet.
Aims: We systematically studied how the signal coherence in
Very-Long-Baseline-Interferometry (VLBI) observations is affected by a
phase-reference calibration at different frequencies and for different
calibrator-to-target separations. The results obtained should be of interest
for a correct interpretation of many phase-referenced observations with VLBI.
Methods: We observed a set of 13 strong sources (the S5 polar cap sample) at
8.4 and 15 GHz in phase-reference mode, with 32 different calibrator/target
combinations spanning angular separations between 1.5 and 20.5 degrees. We
obtained phase-referenced images and studied how the dynamic range and peak
flux density depend on observing frequency and source separation.
Results: We obtained dynamic ranges and peak flux densities of the
phase-referenced images as a function of frequency and separation from the
calibrator. We compared our results with models and phenomenological equations
previously reported.
Conclusions: The dynamic range of the phase-referenced images is strongly
limited by the atmosphere at all frequencies and for all source separations.
The limiting dynamic range is inversely proportional to the sine of the
calibrator-to-target separation. We also find that the peak flux densities,
relative to those obtained with the self-calibrated images, decrease with
source separation.Comment: 5 pages, 3 figures. Submitted to A&A on 5.02.2010; accepted on
11.03.2010
Water vapour at high redshift: Arecibo monitoring of the megamaser in MG J0414+0534
The study of water masers at cosmological distances would allow us to
investigate the parsec-scale environment around powerful radio sources, to
probe the physical conditions of the molecular gas in the inner parsecs of
quasars, and to estimate their nuclear engine masses in the early universe. To
derive this information, the nature of the maser source, jet or disk-maser,
needs to be assessed through a detailed investigation of the observational
characteristics of the line emission. We monitored the maser line in the lensed
quasar MGJ0414+0534 at z = 2.64 with the 300-m Arecibo telescope for ~15 months
to detect possible additional maser components and to measure a potential
velocity drift of the lines. In addition, we follow the maser and continuum
emissions to reveal significant variations in their flux density and to
determine correlation or time-lag, if any, between them. The main maser line
profile is complex and can be resolved into a number of broad features with
line widths of 30-160 km/s. A new maser component was tentatively detected in
October 2008 that is redshifted by 470 km/s w.r.t the systemic velocity of the
quasar. The line width of the main maser feature increased by a factor of two
between the Effelsberg and EVLA observations reported by Impellizzeri et al.
(2008) and the first epoch of the Arecibo monitoring campaign. After correcting
for the lens magnification, we find that the total H2O isotropic luminosity of
the maser in MGJ0414+0534 is now ~30,000 Lsun, making this source the most
luminous ever discovered.[Abridged]Comment: 8 pages, 6 figures, accepted for publication in A&
A Multi-Epoch VLBI Survey of the Kinematics of CJF Sources; Part I: Model-Fit Parameters and Maps
Context: This is the first of a series of papers presenting VLBI observations
of the 293 Caltech-Jodrell Bank Flat-Spectrum (hereafter CJF) sources and their
analysis. Aims: One of the major goals of the CJF is to make a statistical
study of the apparent velocities of the sources. Methods: We have conducted
global VLBI and VLBA observations at 5 GHz since 1990, accumulating thirteen
separate observing campaigns. Results: We present here an overview of the
observations, give details of the data reduction and present the source
parameters resulting from a model-fitting procedure. For every source at every
observing epoch, an image is shown, built up by restoring the model-fitted
components, convolved with the clean beam, into the residual image, which was
made by Fourier transforming the visibility data after first subtracting the
model-fitted components in the uv-plane. Overplotted we show symbols to
represent the model components. Conclusions: We have produced VLBI images of
all but 5 of the 293 sources in the complete CJF sample at several epochs and
investigated the kinematics of 266 AGN.Comment: Figure 1 and Table 2 are only available in electronic form at the CDS
and soon at http://www.mpifr-bonn.mpg.de/staff/sbritzen/cjf.htm
A multifrequency analysis of radio variability of blazars
We have carried out a multifrequency analysis of the radio variability of
blazars, exploiting the data obtained during the extensive monitoring programs
carried out at the University of Michigan Radio Astronomy Observatory (UMRAO,
at 4.8, 8, and 14.5 GHz) and at the Metsahovi Radio Observatory (22 and 37
GHz). Two different techniques detect, in the Metsahovi light curves, evidences
of periodicity at both frequencies for 5 sources (0224+671, 0945+408, 1226+023,
2200+420, and 2251+158). For the last three sources consistent periods are
found also at the three UMRAO frequencies and the Scargle (1982) method yields
an extremely low false-alarm probability. On the other hand, the 22 and 37 GHz
periodicities of 0224+671 and 0945+408 (which were less extensively monitored
at Metsahovi and for which we get a significant false-alarm probability) are
not confirmed by the UMRAO database, where some indications of ill-defined
periods about a factor of two longer are retrieved. We have also investigated
the variability index, the structure function, and the distribution of
intensity variations of the most extensively monitored sources. We find a
statistically significant difference in the distribution of the variability
index for BL Lac objects compared to flat-spectrum radio quasars (FSRQs), in
the sense that the former objects are more variable. For both populations the
variability index steadily increases with increasing frequency. The
distribution of intensity variations also broadens with increasing frequency,
and approaches a log-normal shape at the highest frequencies. We find that
variability enhances by 20-30% the high frequency counts of extragalactic
radio-sources at bright flux densities, such as those of the WMAP and Planck
surveys.Comment: A&A accepted. 12 pages, 16 figure
Optical and radio behaviour of the BL Lacertae object 0716+714
Eight optical and four radio observatories have been intensively monitoring
the BL Lac object 0716+714 in the last years: 4854 data points have been
collected in the UBVRI bands since 1994, while radio light curves extend back
to 1978. Many of these data are presented here for the first time. The
long-term trend shown by the optical light curves seems to vary with a
characteristic time scale of about 3.3 years, while a longer period of 5.5-6
years seems to characterize the radio long-term variations. In general, optical
colour indices are only weakly correlated with brightness. The radio flux
behaviour at different frequencies is similar, but the flux variation amplitude
decreases with increasing wavelength. The radio spectral index varies with
brightness (harder when brighter), but the radio fluxes seem to be the sum of
two different-spectrum contributions: a steady base level and a harder-spectrum
variable component. Once the base level is removed, the radio variations appear
as essentially achromatic, similarly to the optical behaviour. Flux variations
at the higher radio frequencies lead the lower-frequency ones with week-month
time scales. The behaviour of the optical and radio light curves is quite
different, the broad radio outbursts not corresponding in time to the faster
optical ones and the cross-correlation analysis indicating only weak
correlation with long time lags. However, minor radio flux enhancements
simultaneous with the major optical flares can be recognized, which may imply
that the mechanism producing the strong flux increases in the optical band also
marginally affects the radio one.Comment: 18 pages, 15 Postscript figures, 5 JPEG figures, accepted for
publication in A&
Absolute kinematics of radio source components in the complete S5 polar cap sample
We observed the thirteen extragalactic radio sources of the complete S5 polar
cap sample at 15.4 GHz with the Very Long Baseline Array, on 27 July 1999
(1999.57) and 15 June 2000 (2000.46). We present the maps from those two
epochs, along with maps obtained from observations of the 2 cm VLBA survey for
some of the sources of the sample, making a total of 40 maps. We discuss the
apparent morphological changes displayed by the radio sources between the
observing epochs. Our VLBA observations correspond to the first two epochs at
15.4 GHz of a program to study the absolute kinematics of the radio source
components of the members of the sample, by means of phase delay astrometry at
8.4 GHz, 15.4 GHz, and 43 GHz.
Our 15.4 GHz VLBA imaging allowed us to disentangle the inner milliarcsecond
structure of some of the sources, thus resolving components that appeared
blended at 8.4 GHz. For most of the sources, we identified the brightest
feature in each radio source with the core. These identifications are supported
by the spectral index estimates for those brightest features, which are in
general flat, or even inverted. Most of the sources display core-dominance in
the overall emission. We find that three of the sources have their most
inverted spectrum component shifted with respect to the origin in the map,
which approximately coincides with the peak-of-brightness at both 15.4 GHz and
8.4 GHz.Comment: Accepted by A&A (in press). 23 pages, 14 figure
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