131 research outputs found
S5 1803+78 Revisited
We report on our optical monitoring of the BL Lac object S5 1803+78 from 1996 to 2011. The source showed no clear periodicity, but a time scale of about 1 300 days between major flares is possibly present. No systematic trend of the color index with flux variations is evident, at variance with other BL Lacs. In one flare, however, the source was bluer in the rising phase and redder in the falling one. Two ?-ray flares were detected by Fermi-GST during our monitoring: on the occasion of only one of them we found simultaneous optical brightening. A one-zone Synchrotron Self Compton (SSC) model appears too simple to explain the source behavior
A New Fast Silicon Photomultiplier Photometer
The realization of low-cost instruments with high technical performance is a
goal which deserves some efforts in an epoch of fast technological
developments: indeed such instruments can be easily reproduced and therefore
allow to open new research programs in several Observatories. We realized a
fast optical photometer based on the SiPM technology, using commercially
available modules. Using low-cost components we have developed a custom
electronic chain to extract the signal produced by a commercial MPPC module
produced by Hamamatsu, in order to obtain sub millisecond sampling of the light
curve of astronomical sources, typically pulsars. In the early February 2011 we
observed the Crab Pulsar at the Cassini telescope with our prototype
photometer, deriving its period, power spectrum and shape of its light curve in
very good agreement with the results obtained in the past with other
instruments.Comment: Accepted for Publications of the Astronomical Society of Pacific
(PASP), 8 pages, 8 figure
The Intra-Night Optical Variability of the bright BL Lac object S5 0716+714
We address the topic of the Intra-Night Optical Variability of the BL Lac
object S5 0716+714. To this purpose a long term observational campaign was
performed, from 1996 to 2003, which allowed the collection of a very large data
set, containing 10,675 photometric measurements obtained in 102 nights. The
source brightness varied in a range of about 2 mag, although the majority of
observations were performed when it was in the range 13.0 < R < 13.75.
Variability time scales were estimated from the rates of magnitude variation,
which were found to have a distribution function well fitted by an exponential
law with a mean value of 0.027 mag/h, corresponding to an e-folding time scale
of the flux tau_F = 37.6 h. The highest rates of magnitude variation were
around 0.10--0.12 mag/h and lasted less than 2 h. These rates were observed
only when the source had an R magnitude < 13.4, but this finding cannot be
considered significant because of the low statistical occurrence. The
distribution of tau_F has a well defined modal value at 19 h. Assuming the
recent estimate of the beaming factor delta about 20, we derived a typical size
of the emitting region of about 5 times 10^{16}/(1 + z) cm. The possibility to
search for a possible correlation between the mean magnitude variation rate and
the long term changes of the velocity of superluminal components in the jet is
discussed.Comment: 12 pages, 10 figures, accepted for Astronomy and Astrophysic
The Long Term Optical Variability of the BL Lac object S5 0716+714: Evidence for a Precessing Jet
We present the historic light curve of the BL Lac object S5 0716+714,
spanning the time interval from 1953 to 2003, built using Asiago archive plates
and our recent CCD observations, together with literature data. The source
shows an evident long term variability, over which well known short term
variations are superposed. In particular, in the period from 1961 to 1983 the
mean brightness of S5 0716+714 remained significantly fainter than that
observed after 1994. Assuming a constant variation rate of the mean magnitude
we can estimate a value of about 0.11 magnitude/year. The simultaneous
occurrence of decreasing ejection velocities of superluminal moving components
in the jet reported by Bach et al. (2005) suggests that both phenomena are
related to the change of the direction of the jet to the line of sight from
about 5 to 0.7 degrees for an approximately constant bulk Lorentz factor of
about 12. A simple explanation is that of a precessing relativistic jet, which
should presently be close to the smallest orientation angle. One can therefore
expect in the next ten years a decrease of the mean brightness of about 1
magnitude.Comment: to appear on The Astronomical Journal, 17 pages, 7 figures. Fig.2 is
given as a separated jpg fil
A New Fast Silicon Photomultiplier Photometer
The Crab pulsar is one of the most intensively studied X-ray/optical objects, but up to now only a small number of research groups have based their photometers on SiPM technology. In early February 2011, the Crab pulsar signal was observed with our photometer prototype. With low-cost instrumentation, the results of the analysis are very significant: the processed data acquired on the Crab pulsar gave both a good light curve and a good power spectrum, in comparison with the data analysis results of other more expensive photometer instrumentation
Optical and Radio monitoring of S5 1803+74
The optical (BVRI) and radio (8.4 GHz) light curves of S5 1803+784 on a time
span of nearly 6 years are presented and discussed. The optical light curve
showed an overall variation greater than 3 mag, and the largest changes occured
in three strong flares. No periodicity was found in the light curve on time
scales up to a year. The variability in the radio band is very different, and
shows moderate oscillations around an average constant flux density rather than
relevant flares, with a maximum amplitude of 30%, without a simultaneous
correspondence between optical and radio luminosity. The optical spectral
energy distribution was always well fitted by a power law. The spectral index
shows small variations and there is indication of a positive correlation with
the source luminosity. Possible explanations of the source behaviour are
discussed in the framework of current models.Comment: 25 pages, 12 figure
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