1,274 research outputs found
Study of underlying particle spectrum during huge X-ray flare of Mkn 421 in April 2013
Context: In April 2013, the nearby (z=0.031) TeV blazar, Mkn 421, showed one
of the largest flares in X-rays since the past decade. Aim: To study all
multiwavelength data available during MJD 56392 to 56403, with special emphasis
on X-ray data, and understand the underlying particle energy distribution.
Methods: We study the correlations between the UV and gamma bands with the
X-ray band using the z-transformed discrete correlation function. We model the
underlying particle spectrum with a single population of electrons emitting
synchrotron radiation, and do a statistical fitting of the simultaneous,
time-resolved data from the Swift-XRT and the NuSTAR. Results: There was rapid
flux variability in the X-ray band, with a minimum doubling timescale of hrs. There were no corresponding flares in UV and gamma bands. The
variability in UV and gamma rays are relatively modest with and
respectively, and no significant correlation was found with the
X-ray light curve. The observed X-ray spectrum shows clear curvature which can
be fit by a log parabolic spectral form. This is best explained to originate
from a log parabolic electron spectrum. However, a broken power law or a power
law with an exponentially falling electron distribution cannot be ruled out
either. Moreover, the excellent broadband spectrum from keV allows us
to make predictions of the UV flux. We find that this prediction is compatible
with the observed flux during the low state in X-rays. However, during the
X-ray flares, the predicted flux is a factor of smaller than the
observed one. This suggests that the X-ray flares are plausibly caused by a
separate population which does not contribute significantly to the radiation at
lower energies. Alternatively, the underlying particle spectrum can be much
more complex than the ones explored in this work.Comment: 11 pages, 7 figures, Accepted in A&
A fit to the simultaneous broadband spectrum of Cygnus X-1 using the transition disk model
We have used the transition disk model to fit the simultaneous broad band
( keV) spectrum of Cygnus X-1 from OSSE and Ginga observations. In this
model, the spectrum is produced by saturated Comptonization within the inner
region of the accretion disk, where the temperature varies rapidly with radius.
In an earlier attempt, we demonstrated the viability of this model by fitting
the data from EXOSAT, XMPC balloon and OSSE observations, though these were not
made simultaneously. Since the source is known to be variable, however, the
results of this fit were not conclusive. In addition, since only once set of
observations was used, the good agreement with the data could have been a
chance occurrence. Here, we improve considerably upon our earlier analysis by
considering four sets of simultaneous observations of Cygnus X-1, using an
empirical model to obtain the disk temperature profile. The vertical structure
is then obtained using this profile and we show that the analysis is self-
consistent. We demonstrate conclusively that the transition disk spectrum is a
better fit to the observations than that predicted by the soft photon
Comptonization model. Since the temperature profile is obtained by fitting the
data, the unknown viscosity mechanism need not be specified. The disk structure
can then be used to infer the viscosity parameter , which appears to
vary with radius and luminosity. This behavior can be understood if
depends intrinsically on the local parameters such as density, height and
temperature. However, due to uncertainties in the radiative transfer,
quantitative statements regarding the variation of cannot yet be made.Comment: 8 figures. uses aasms4.sty, accepted by ApJ (Mar 98
Tagging single muons and other long-flying relativistic charged particles by ultra-fast timing in air Cherenkov telescopes
Atmospheric air Cherenkov telescopes are successfully used for ground-based,
very high-energy (VHE) gamma ray astronomy. Triggers from the so-called single
muon and other long-flying relativistic charged particle events are an unwanted
background for the Cherenkov telescope. Because of low rate at TeV energies the
muon background is unimportant. It is much more intense for telescopes with
high photon sensitivity and low energy threshold. Below a few hundred GeV
energy, the so-called muon background becomes so intense, that it can
deteriorate the sensitivity of telescopes (the so-called muon-wall problem).
From general considerations it can be anticipated that the signature of these
particles should be a light pulse with a narrow time structure. In fact,
simulations show that the pulses from muons have a very narrow time profile
that is well below the time resolutions of nearly all currently operating
telescopes. In this report we elaborate on the time profile of Cherenkov light
from the so-called single muons and show that a telescope with ultra-fast time
response can open a new dimension allowing one to tag and to reject those
events.Comment: Accepted by Astroparticle Physic
Broadband study of blazar 1ES 1959+650 during flaring state in 2016
Aim : The nearby TeV blazar 1ES 1959+650 (z=0.047) was reported to be in
flaring state during June - July 2016 by Fermi-LAT, FACT, MAGIC and VERITAS
collaborations. We studied the spectral energy distributions (SEDs) in
different states of the flare during MJD 57530 - 57589 using simultaneous
multiwaveband data to understand the possible broadband emission scenario
during the flare. Methods : The UV/optical and X-ray data from UVOT and XRT
respectively on board Swift and high energy -ray data from Fermi-LAT
are used to generate multiwaveband lightcurves as well as to obtain high flux
states and quiescent state SEDs. The correlation and lag between different
energy bands is quantified using discrete correlation function. The synchrotron
self Compton (SSC) model was used to reproduce the observed SEDs during flaring
and quiescent states of the source. Results : A decent correlation is seen
between X-ray and high energy -ray fluxes. The spectral hardening with
increase in the flux is seen in X-ray band. The powerlaw index vs flux plot in
-ray band indicates the different emission regions for 0.1 - 3 GeV and
3-300 GeV energy photons. Two zone SSC model satisfactorily fits the observed
broadband SEDs. The inner zone is mainly responsible for producing synchrotron
peak and high energy -ray part of the SED in all states. The second
zone is mainly required to produce less variable optical/UV and low energy
-ray emission. Conclusions : Conventional single zone SSC model does
not satisfactorily explain broadband emission during observation period
considered. There is an indication of two emission zones in the jet which are
responsible for producing broadband emission from optical to high energy
-rays.Comment: 11 pages, 12 figures, Accepted in A&
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