301 research outputs found
Simultaneous Planck, Swift, and Fermi observations of X-ray and gamma-ray selected blazars
We present simultaneous Planck, Swift, Fermi, and ground-based data for 105 blazars belonging to three samples with flux limits in the soft X-ray, hard X-ray, and gamma-ray bands, with additional 5GHz flux-density limits to ensure a good probability of a Planck detection. We compare our results to those of a companion paper presenting simultaneous Planck and multi-frequency observations of 104 radio-loud northern active galactic nuclei selected at radio frequencies. While we confirm several previous results, our unique data set allows us to demonstrate that the selection method strongly influences the results, producing biases that cannot be ignored. Almost all the BL Lac objects have been detected by the Fermi Large Area Telescope (LAT), whereas 30% to 40% of the flat-spectrum radio quasars (FSRQs) in the radio, soft X-ray, and hard X-ray selected samples are still below the gamma-ray detection limit even after integrating 27 months of Fermi-LAT data. The radio to sub-millimetre spectral slope of blazars is quite flat, with similar to 0 up to about 70GHz, above which it steepens to similar to -0.65. The BL Lacs have significantly flatter spectra than FSRQs at higher frequencies. The distribution of the rest-frame synchrotron peak frequency (nu(S)(peak)) in the spectral energy distribution (SED) of FSRQs is the same in all the blazar samples with = 10(13.1+.1) Hz, while the mean inverse Compton peak frequency, , ranges from 10(21) to 10(22) Hz. The distributions of nu(S)(peak) and nu(S)(peak) of BL Lacs are much broader and are shifted to higher energies than those of FSRQs; their shapes strongly depend on the selection method. The Compton dominance of blazars, defined as the ratio of the inverse Compton to synchrotron peak luminosities, ranges from less than 0.2 to nearly 100, with only FSRQs reaching values larger than about 3. Its distribution is broad and depends strongly on the selection method, with gamma-ray selected blazars peaking at similar to 7 or more, and radio-selected blazars at values close to 1, thus implying that the common assumption that the blazar power budget is largely dominated by high-energy emission is a selection effect. A comparison of our multi-frequency data with theoretical predictions shows that simple homogeneous SSC models cannot explain the simultaneous SEDs of most of the gamma-ray detected blazars in all samples. The SED of the blazars that were not detected by Fermi-LAT may instead be consistent with SSC emission. Our data challenge the correlation between bolometric luminosity and nu(S)(peak) predicted by the blazar sequence. --author-supplied descriptio
Results from the Blazar Monitoring Campaign at the Whipple 10m Gamma-ray Telescope
In September 2005, the observing program of the Whipple 10 m gamma-ray
telescope was redefined to be dedicated almost exclusively to AGN monitoring.
Since then the five Northern Hemisphere blazars that had already been detected
at Whipple are monitored routinely each night that they are visible. Thanks to
the efforts of a large number of multiwavelength collaborators, the first year
of this program has been very successful. We report here on the analysis of
Markarian 421 observations taken from November, 2005 to May, 2006 in the
gamma-ray, X-ray, optical and radio bands.Comment: 4 pages; contribution to the 30th International Cosmic Ray
Conference, Merida, Mexico, July 200
Frequency dependent core shifts and parameter estimation for the blazar 3C 454.3
We study the core shift effect in the parsec scale jet of the blazar 3C 454.3
using the 4.8 GHz - 36.8 GHz radio light curves obtained from three decades of
continuous monitoring. From a piecewise Gaussian fit to each flare, time lags
between the observation frequencies and spectral indices
based on peak amplitudes are determined. From the fit , indicating equipartition between
the magnetic field energy density and the particle energy density. From the fit
, is in the range to . A mean
magnetic field strength at 1 pc, G, and at the core,
mG, are inferred, consistent with previous
estimates. The measure of core position offset is
pc GHz when averaged over all frequency pairs. Based on the
statistical trend shown by the measured core radius as a
function of , we infer that the synchrotron opacity model may not be valid
for all cases. A Fourier periodogram analysis yields power law slopes in the
range to describing the power spectral density shape and gives
bend timescales in the range yr. This result, and both positive
and negative , indicate that the flares originate from multiple shocks
in a small region. Important objectives met in our study include: the
demonstration of the computational efficiency and statistical basis of the
piecewise Gaussian fit; consistency with previously reported results; evidence
for the core shift dependence on observation frequency and its utility in jet
diagnostics in the region close to the resolving limit of very long baseline
interferometry observations.Comment: 12 pages, 11 figures (23 sub-figures), 5 tables. Accepted for
publication in MNRA
The core shift effect in the blazar 3C 454.3
Opacity-driven shifts of the apparent VLBI core position with frequency (the
"core shift" effect) probe physical conditions in the innermost parts of jets
in active galactic nuclei. We present the first detailed investigation of this
effect in the brightest gamma-ray blazar 3C454.3 using direct measurements from
simultaneous 4.6-43 GHz VLBA observations, and a time lag analysis of 4.8-37
GHz lightcurves from the UMRAO, CrAO, and Metsahovi observations in 2007-2009.
The results support the standard Konigl model of jet physics in the VLBI core
region. The distance of the core from the jet origin r_c(nu), the core size
W(nu), and the lightcurve time lag DT(nu) all depend on the observing frequency
nu as r_c(nu)~W(nu)~ DT(nu)~nu^-1/k. The obtained range of k=0.6-0.8 is
consistent with the synchrotron self-absorption being the dominating opacity
mechanism in the jet. The similar frequency dependence of r_c(nu) and W(nu)
suggests that the external pressure gradient does not dictate the jet geometry
in the cm-band core region. Assuming equipartition, the magnetic field strength
scales with distance r as B = 0.4(r/1pc)^-0.8 G. The total kinetic power of
electron/positron jet is about 10^44 ergs/s.Comment: Accepted for publication in MNRAS; 10 pages, 6 figure
A peculiar multi-wavelength flare in the Blazar 3C 454.3
The blazar 3C454.3 exhibited a strong flare seen in gamma-rays, X-rays, and
optical/NIR bands during 3--12 December 2009. Emission in the V and J bands
rose more gradually than did the gamma-rays and soft X-rays, though all peaked
at nearly the same time. Optical polarization measurements showed dramatic
changes during the flare, with a strong anti-correlation between optical flux
and degree of polarization (which rose from ~ 3% to ~ 20%) during the declining
phase of the flare. The flare was accompanied by large rapid swings in
polarization angle of ~ 170 degree. This combination of behaviors appear to be
unique. We have cm-band radio data during the same period but they show no
correlation with variations at higher frequencies. Such peculiar behavior may
be explained using jet models incorporating fully relativistic effects with a
dominant source region moving along a helical path or by a shock-in-jet model
incorporating three-dimensional radiation transfer if there is a dominant
helical magnetic field. We find that spectral energy distributions at different
times during the flare can be fit using modified one-zone models where only the
magnetic field strength and particle break frequencies and normalizations need
change. An optical spectrum taken at nearly the same time provides an estimate
for the central black hole mass of ~ 2.3 * 10^9 M_sun. We also consider two
weaker flares seen during the d span over which multi-band data are
available. In one of them, the V and J bands appear to lead the -ray
and X-ray bands by a few days; in the other, all variations are simultaneous.Comment: 11 pages, 4 figures, 2 tables; MNRAS in pres
Decreased spermatogonial quantity in prepubertal boys with leukaemia treated with alkylating agents
Non peer reviewe
Research and Innovation As a Catalyst For Food System Transformation
Background Food systems are associated with severe and persistent problems worldwide. Governance approaches aiming to foster sustainable transformation of food systems face several challenges due to the complex nature of food systems.
Scope and approach In this commentary we argue that addressing these governance challenges requires the development and adoption of novel research and innovation (R&I) approaches that will provide evidence to inform food system transformation and will serve as catalysts for change. We first elaborate on the complexity of food systems (transformation) and stress the need to move beyond traditional linear R&I approaches to be able to respond to persistent problems that affect food systems. Though integrated transdisciplinary approaches are promising, current R&I systems do not sufficiently support such endeavors. As such, we argue, we need strategies that trigger a double transformation – of food systems and of their R&I systems.
Key Findings and Conclusions Seizing the opportunities to transform R&I systems has implications for how research is done – pointing to the need for competence development among researchers, policy makers and society in general – and requires specific governance interventions that stimulate a systemic approach. Such interventions should foster transdisciplinary and transformative research agendas that stimulate portfolios of projects that will reinforce one another, and stimulate innovative experiments to shape conditions for systemic change. In short, a thorough rethinking of the role of R&I as well as how it is funded is a crucial step towards the development of the integrative policies that are necessary to engender systemic change – in the food system and beyond
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