1,995 research outputs found
Long-term OVRO monitoring of LSI+61303: confirmation of the two close periodicities
Context: The gamma-ray binary LSI+61303 shows multiple periodicities. The
timing analysis of 6.7 yr of GBI radio data and of 6 yr of Fermi-LAT GeV
gamma-ray data both have found two close periodicities P1(GBI) = 26.49 \pm 0.07
d, P2(GBI)=26.92 \pm 0.07 d and P1(gamma)=26.48 \pm 0.08 d, P2(gamma) = 26.99
\pm 0.08 d. Aims: The system LSI+61303 is the object of several continuous
monitoring programs at low and high energies. The frequency difference between
f1 and f2 of only 0.0006 d(-1) requires long-term monitoring because the
frequency resolution in timing analysis is related to the inverse of the
overall time interval. The Owens Valley Radio Observatory (OVRO) 40 m telescope
has been monitoring the source at 15 GHz for five years and overlaps with
Fermi-LAT monitoring. The aim of this work is to establish whether the two
frequencies are also resolved in the OVRO monitoring. Methods: We analysed OVRO
data with the Lomb-Scargle method. We also updated the timing analysis of
Fermi-LAT observations. Results: The periodograms of OVRO data confirm the two
periodicities P1(OVRO) = 26.5 \pm 0.1 d and P2(OVRO) = 26.9 \pm 0.1 d.
Conclusions: The three indipendent measurements of P1 and P2 with GBI, OVRO,
and Fermi-LAT observations confirm that the periodicities are permanent
features of the system LSI+61303. The similar behaviours of the emission at
high (GeV) and low (radio) energy when the compact object in LSI+61303 is
toward apastron suggest that the emission is caused by the same periodically
(P1) ejected population of electrons in a precessing (P2) jet.Comment: 4 pages, 7 figures, A&A Letters in pres
Disk-Jet Connection in Agns and Microquasars: The Possibility of Thermal Flares in the Center
We discuss the possibility of thermal flares in centers of AGNs and
microquasars. We present preliminary results of an ongoing study trying to
assess the feasibility of a hypothesis suggesting that certain flares observed
in these sources originate in the very centers of the systems and not in the
relativistic jets. Using a simple toy model we reproduce optical flares with
lightcurves very similar to those observed in the sources. The model suits
especially well those cases where only the latter peak of a double-peaked
optical flare has a radio counterpart.Comment: 6 pages, 1 figure, to appear in the proceedings of the HEPRO II
conference, Buenos Aires, October 26-30 200
Doppler factors, Lorentz factors and viewing angles for quasars, BL Lacertae objects and radio galaxies
We have calculated variability Doppler boosting factors, Lorentz factors, and
viewing angles for a large sample of sources by using total flux density
observations at 22 and 37 GHz and VLBI data. We decomposed the flux curves into
exponential flares and determined the variability brightness temperatures of
the fastest flares. By assuming the same intrinsic brightness temperature for
each source, we calculated the Doppler boosting factors for 87 sources. In
addition we used new apparent jet speed data to calculate the Lorentz factors
and viewing angles for 67 sources. We find that all quasars in our sample are
Doppler-boosted and that the Doppler boosting factors of BL Lacertae objects
are lower than of quasars. The new Lorentz factors are about twice as high as
in earlier studies, which is mainly due to higher apparent speeds in our
analyses. The jets of BL Lacertae objects are slower than of quasars. There are
some extreme sources with very high derived Lorentz factors of the order of a
hundred. These high Lorentz factors could be real. It is also possible that the
sources exhibit such rapid flares that the fast variations have remained
undetected in monitoring programmes, or else the sources have a complicated jet
structure that is not amenable to our simple analysis. Almost all the sources
are seen in a small viewing angle of less than 20 degrees. Our results follow
the predictions of basic unification schemes for AGN.Comment: 12 pages, 14 figures, Accepted for publication in A&
A connection between -ray and parsec-scale radio flares in the blazar 3C 273
We present a comprehensive 5-43 GHz VLBA study of the blazar 3C 273 initiated
after an onset of a strong -ray flare in this source. We have analyzed
the kinematics of new-born components, light curves, and position of the
apparent core to pinpoint the location of the -ray emission. Estimated
location of the -ray emission zone is close to the jet apex, 2 pc to 7
pc upstream from the observed 7 mm core. This is supported by ejection of a new
component. The apparent core position was found to be inversely proportional to
frequency. The brightness temperature in the 7 mm core reached values up to at
least K during the flare. This supports the dominance of particle
energy density over that of magnetic field in the 7 mm core. Particle density
increased during the radio flare at the apparent jet base, affecting
synchrotron opacity. This manifested itself as an apparent core shuttle along
the jet during the 7 mm flare. It is also shown that a region where optical
depth decreases from to spans over several parsecs along
the jet. The jet bulk flow speed estimated at the level of 12c on the basis of
time lags between 7 mm light curves of stationary jet features is 1.5 times
higher than that derived from VLBI apparent kinematics analysis.Comment: Accepted for publication in MNRAS. 17 pages, 15 figures, 10 tables,
with supplementary materials attache
Multi-wavelength observations of the gamma-ray flaring quasar S4 1030+61 in 2009-2014
We present a study of the parsec-scale multi-frequency properties of the
quasar S4 1030+61 during a prolonged radio and gamma-ray activity. Observations
were performed within Fermi gamma-ray telescope, OVRO 40-m telescope and MOJAVE
VLBA monitoring programs, covering five years from 2009. The data are
supplemented by four-epoch VLBA observations at 5, 8, 15, 24, and 43 GHz, which
were triggered by the bright gamma-ray flare, registered in the quasar in 2010.
The S4 1030+61 jet exhibits an apparent superluminal velocity of (6.4+-0.4)c
and does not show ejections of new components in the observed period, while
decomposition of the radio light curve reveals nine prominent flares. The
measured variability parameters of the source show values typical for
Fermi-detected quasars. Combined analysis of radio and gamma-ray emission
implies a spatial separation between emitting regions at these bands of about
12 pc and locates the gamma-ray emission within a parsec from the central
engine. We detected changes in the value and direction of the linear
polarization and the Faraday rotation measure. The value of the intrinsic
brightness temperature of the core is above the equipartition state, while its
value as a function of distance from the core is well approximated by the
power-law. Altogether these results show that the radio flaring activity of the
quasar is accompanied by injection of relativistic particles and energy losses
at the jet base, while S4 1030+61 has a stable, straight jet well described by
standard conical jet theories.Comment: accepted by MNRAS, 16 pages, 14 figures, 8 tables, 5 pages of
supplementary materia
Locating the gamma-ray emission site in Fermi/LAT blazars from correlation analysis between 37 GHz radio and gamma-ray light curves
We address the highly debated issue of constraining the gamma-ray emission
region in blazars from cross-correlation analysis using discrete correlation
function between radio and gamma-ray light curves. The significance of the
correlations is evaluated using two different approaches: simulating light
curves and mixed source correlations. The cross-correlation analysis yielded 26
sources with significant correlations. In most of the sources, the gamma-ray
peaks lead the radio with time lags in the range +20 and +690 days, whereas in
sources 1633+382 and 3C 345 we find the radio emission to lead the gamma rays
by -15 and -40 days, respectively. Apart from the individual source study, we
stacked the correlations of all sources and also those based on sub-samples.
The time lag from the stacked correlation is +80 days for the whole sample and
the distance travelled by the emission region corresponds to 7 pc. We also
compared the start times of activity in radio and gamma rays of the correlated
flares using Bayesian block representation. This shows that most of the flares
at both wavebands start at almost the same time, implying a co-spatial origin
of the activity. The correlated sources show more flares and are brighter in
both bands than the uncorrelated ones.Comment: 15 pages, 8 figures and 4 tables. Published in MNRAS. Online-only
Figure 6 is available as ancillary file with this submissio
Constraints on Blazar Jet Conditions During Gamma-Ray Flaring from Radiative Transfer Modeling
As part of a program to investigate jet flow conditions during GeV gamma-ray
flares detected by Fermi, we are using UMRAO multi-frequency, centimeter-band
total flux density and linear polarization monitoring observations to constrain
radiative transfer models incorporating propagating shocks orientated at an
arbitrary angle to the flow direction. We describe the characteristics of the
model, illustrate how the data are used to constrain the models, and present
results for three program sources with diverse characteristics: PKS 0420-01, OJ
287, and 1156+295. The modeling of the observed spectral behavior yields
information on the sense, strength and orientation of the shocks producing the
radio-band flaring; on the energy distribution of the radiating particles; and
on the observer's viewing angle with respect to the jet independent of VLBI
data. We present evidence that, while a random component dominates the jet
magnetic field, a distinguishing feature of those radio events with an
associated gamma-ray flare is the presence of a weak but non-negligible ordered
magnetic field component along the jet axis.Comment: 6 pages, 4 figures. To appear in the proceedings of "The Innermost
Regions of Relativistic Jets and Their Magnetic Fields", Granada, Spai
Challenges for the Therapeutic use of Pluripotent Stem Derived Cells
Human embryonic stem cells (hESC) and induced pluripotent stem cells (hiPSC) are an attractive cell source for regenerative medicine. These cells can be expanded to vast numbers and can be differentiated to many desired pluripotent stem cells (PSC) derived therapeutic cells. Cell replacement bears promises, but also challenges. The introduction of exogenous cells in a recipient must address several different topics; its safety, the exclusion of tumor formation, the immunological response and possible rejection, the cells cleanliness and their biological quality, and quantity representing the functionality of the PSC derived therapeutic cells. Tumor formation requires the removal of any PSC remaining after differentiation. Immunological rejection can be addressed with immunomodulation of the cells and the recipient. Cleanliness can be optimized using good manufacturing practice quality systems. At last, the functionality of the cells must be tested in in vitro and in animal models. After addressing these challenges, precise strategies are developed to monitor the status of the cells at different times and in case of undesired results, corresponding counteracting strategies must exist before any clinical attempt
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