9,475 research outputs found
Discovery of hard X-ray features around hotspots of Cygnus A
We present results of analysis of a Chandra observation of Cygnus A in which
the X-ray hotspots at the ends of the jets are mapped in detail. A hardness map
reveals previously unknown structure in the form of outer and inner hard arcs
around the hotspots, with hardness significantly enhanced compared with the
hotspot central regions. The outer hard arcs may constitute the first detection
of the bow shock; the inner hard arcs may reveal where the jets impact on the
hotspots. We argue that these features cannot result from electrons radiating
by the synchrotron self-Compton process. Instead we consider two possible
sources of the hard emission: the outer arcs may be due to thermal radiation of
hot intracluster gas compressed at the bow shock. Alternatively, both outer and
inner arcs may be due to synchrotron radiation of electrons accelerated in
turbulent regions highly perturbed by shocks and shear flows. Comparison of
measured hardness ratios with simulations of the hardness ratios resulting from
these processes show that it is more diffcult to explain the observations with
a thermal model. Although we cannot rule out a thermal model, we argue in
favour of the non-thermal explanation. The hard regions in the secondary
hotspots suggest that jet activity is still powering these hotspots.Comment: MNRAS in press; 5 pages, 3 figures (2 figures in colour in jpeg
format should be printed separately
Nanoantennas for visible and infrared radiation
Nanoantennas for visible and infrared radiation can strongly enhance the
interaction of light with nanoscale matter by their ability to efficiently link
propagating and spatially localized optical fields. This ability unlocks an
enormous potential for applications ranging from nanoscale optical microscopy
and spectroscopy over solar energy conversion, integrated optical
nanocircuitry, opto-electronics and density-ofstates engineering to
ultra-sensing as well as enhancement of optical nonlinearities. Here we review
the current understanding of optical antennas based on the background of both
well-developed radiowave antenna engineering and the emerging field of
plasmonics. In particular, we address the plasmonic behavior that emerges due
to the very high optical frequencies involved and the limitations in the choice
of antenna materials and geometrical parameters imposed by nanofabrication.
Finally, we give a brief account of the current status of the field and the
major established and emerging lines of investigation in this vivid area of
research.Comment: Review article with 76 pages, 21 figure
Hot gas in Mach cones around Virgo Cluster spiral galaxies
The detailed comparison between observations and simulations of ram pressure
stripped spiral galaxies in the Virgo cluster has led to a three dimensional
view of the galaxy orbits within the hot intracluster medium. The 3D velocities
and Mach numbers derived from simulations can be used to derive simple Mach
cone geometries for Virgo spiral galaxies. We search for indications of hot gas
within Mach cones in X-ray observations of selected Virgo Cluster spiral
galaxies (NGC 4569, NGC 4388, and NGC 4501). We find extraplanar diffuse X-ray
emission in all galaxies. Based on the 3D velocity vectors from dynamical
modelling a simple Mach cone is fitted to the triangular shape of NGC 4569's
diffuse X-ray emission. Assuming that all extraplanar diffuse X-ray emission
has to be located inside the Mach cone, we also fit Mach cones to NGC 4388's
and NGC 4501's extraplanar X-ray emission. For NGC 4569 it is hard to reconcile
the derived Mach cone opening angle with a Mach number based on the sound speed
alone. Instead, a Mach number involving the Alfv\'enic speed seems to be more
appropriate, yielding a magnetic field strength of -6 G for a
intracluster medium density of cm. Whereas the
temperature of the hot component of NGC 4569's X-ray halo (0.5 keV) is at the
high end but typical for a galactic outflow, the temperature of the hot gas
tails of NGC 4388 and NGC 4501 are significantly hotter (0.7-0.9 keV). In NGC
4569 we find direct evidence for a Mach cone which is filled with hot gas from
a galactic superwind. We suggest that the high gas temperatures in the X-ray
tails of NGC 4388 and NGC 4501 are due to the mixing of the stripped ISM into
the hot intracluster medium of the Virgo cluster.Comment: 11 pages, 10 figures, 5 tables. Accepted for publication in Astronomy
and Astrophysic
Multi-wavelength observations of the binary system PSR B1259-63/LS 2883 around the 2010-2011 periastron passage
We report on broad multi-wavelength observations of the 2010-2011 periastron
passage of the gamma-ray loud binary system PSR B1259-63. High resolution
interferometric radio observations establish extended radio emission trailing
the position of the pulsar. Observations with the Fermi Gamma-ray Space
Telescope reveal GeV gamma-ray flaring activity of the system, reaching the
spin-down luminosity of the pulsar, around 30 days after periastron. There are
no clear signatures of variability at radio, X-ray and TeV energies at the time
of the GeV flare. Variability around periastron in the H emission line,
can be interpreted as the gravitational interaction between the pulsar and the
circumstellar disk. The equivalent width of the H grows from a few days
before periastron until a few days later, and decreases again between 18 and 46
days after periastron. In near infrared we observe the similar decrease of the
equivalent width of Br line between the 40th and 117th day after the
periastron. For the idealized disk, the variability of the H line
represents the variability of the mass and size of the disk. We discuss
possible physical relations between the state of the disk and GeV emission
under assumption that GeV flare is directly related to the decrease of the disk
size.Comment: accepted to MNRA
Probing the Solar Wind Acceleration Region with the Sun--Grazing Comet C/2002 S2
Comet C/2002 S2, a member of the Kreutz family of Sungrazing comets, was
discovered in white light images of the SOHO/LASCO coronagraph on 2002
September 18 and observed in \hi\, \lya\, emission by the SOHO/UVCS instrument
at four different heights as it approached the Sun. The \hi\, \lya\, line
profiles detected by UVCS are analyzed to determine the spectral parameters:
line intensity, width and Doppler shift with respect to the coronal background.
Two dimensional comet images of these parameters are reconstructed at the
different heights. A novel aspect of the observations of this sungrazing comet
data is that, whereas the emission from the most of the tail is blue--shifted,
that along one edge of the tail is red--shifted. We attribute these shifts to a
combination of solar wind speed and interaction with the magnetic field. In
order to use the comet to probe the density, temperature and speed of the
corona and solar wind through which it passes, as well as to determine the
outgassing rate of the comet, we develop a Monte Carlo simulation of the \hi\,
\lya\, emission of a comet moving through a coronal plasma. From the outgassing
rate, we estimate a nucleus diameter of about 9 meters. This rate steadily
increases as the comet approaches the Sun while the optical brightness
decreases by more than a factor of ten and suddenly recovers. This indicates
that the optical brightness is determined by the lifetimes of the grains,
sodium atoms and molecules produced by the comet.Comment: 17 pages, 17 figures. Accepted by Ap
Antenna-coupled silicon-organic hybrid integrated photonic crystal modulator for broadband electromagnetic wave detection
In this work, we design, fabricate and characterize a compact, broadband and
highly sensitive integrated photonic electromagnetic field sensor based on a
silicon-organic hybrid modulator driven by a bowtie antenna. The large
electro-optic (EO) coefficient of organic polymer, the slow-light effects in
the silicon slot photonic crystal waveguide (PCW), and the broadband field
enhancement provided by the bowtie antenna, are all combined to enhance the
interaction of microwaves and optical waves, enabling a high EO modulation
efficiency and thus a high sensitivity. The modulator is experimentally
demonstrated with a record-high effective in-device EO modulation efficiency of
r33=1230pm/V. Modulation response up to 40GHz is measured, with a 3-dB
bandwidth of 11GHz. The slot PCW has an interaction length of 300um, and the
bowtie antenna has an area smaller than 1cm2. The bowtie antenna in the device
is experimentally demonstrated to have a broadband characteristics with a
central resonance frequency of 10GHz, as well as a large beam width which
enables the detection of electromagnetic waves from a large range of incident
angles. The sensor is experimentally demonstrated with a minimum detectable
electromagnetic power density of 8.4mW/m2 at 8.4GHz, corresponding to a minimum
detectable electric field of 2.5V/m and an ultra-high sensitivity of
0.000027V/m Hz^-1/2 ever demonstrated. To the best of our knowledge, this is
the first silicon-organic hybrid device and also the first PCW device used for
the photonic detection of electromagnetic waves. Finally, we propose some
future work, including a Teraherz wave sensor based on antenna-coupled
electro-optic polymer filled plasmonic slot waveguide, as well as a fully
packaged and tailgated device.Comment: 20 pages, 16 figure
Constraining Relativistic Bow Shock Properties in Rotation-Powered Millisecond Pulsar Binaries
Multiwavelength followup of unidentified Fermi sources has vastly expanded
the number of known galactic-field "black widow" and "redback" millisecond
pulsar binaries. Focusing on their rotation-powered state, we interpret the
radio to X-ray phenomenology in a consistent framework. We advocate the
existence of two distinct modes differing in their intrabinary shock
orientation, distinguished by the phase-centering of the double-peaked X-ray
orbital modulation originating from mildly-relativistic Doppler boosting. By
constructing a geometric model for radio eclipses, we constrain the shock
geometry as functions of binary inclination and shock stand-off . We
develop synthetic X-ray synchrotron orbital light curves and explore the model
parameter space allowed by radio eclipse constraints applied on archetypal
systems B1957+20 and J1023+0038. For B1957+20, from radio eclipses the
stand-off is -- fraction of binary separation from the
companion center, depending on the orbit inclination. Constructed X-ray light
curves for B1957+20 using these values are qualitatively consistent with those
observed, and we find occultation of the shock by the companion as a minor
influence, demanding significant Doppler factors to yield double peaks. For
J1023+0038, radio eclipses imply while X-ray light curves
suggest (from the pulsar). Degeneracies in the
model parameter space encourage further development to include transport
considerations. Generically, the spatial variation along the shock of the
underlying electron power-law index should yield energy-dependence in the shape
of light curves motivating future X-ray phase-resolved spectroscopic studies to
probe the unknown physics of pulsar winds and relativistic shock acceleration
therein.Comment: Accepted to ApJ, 36 pages, 15 figures; comments welcom
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