297 research outputs found
Reflection nebulae in the Galactic Center: the case for soft X-ray imaging polarimetry
The origin of irradiation and fluorescence of the 6.4 keV bright giant
molecular clouds surrounding Sgr A*, the central supermassive black hole of our
Galaxy, remains enigmatic. Testing the theory of a past active period of Sgr A*
requires X-ray polarimetry. In this paper, we show how modern imaging
polarimeters could revolutionize our understanding of the Galactic Center.
Through Monte Carlo modeling, we produce a 4-8 keV polarization map of the
Galactic Center, focusing on the polarimetric signature produced by Sgr B1, Sgr
B2, G0.11-0.11, Bridge E, Bridge D, Bridge B2, MC2, MC1, Sgr C3, Sgr C2, and
Sgr C1. We estimate the resulting polarization, include polarized flux dilution
by the diffuse plasma emission detected toward the GC, and simulate the
polarization map that modern polarimetric detectors would obtain assuming the
performances of a mission prototype. The eleven reflection nebulae investigated
in this paper present a variety of polarization signatures, ranging from nearly
unpolarized to highly polarized (about 77%) fluxes. A major improvement in our
simulation is the addition of a diffuse, unpolarized plasma emission that
strongly impacts soft X-ray polarized fluxes. The dilution factor is in the
range 50% - 70%, making the observation of the Bridge structure unlikely even
in the context of modern polarimetry. The best targets are the Sgr B and Sgr C
complexes, and the G0.11-0.11 cloud. An exploratory observation of a few
hundred kilo-seconds of the Sgr B complex would allow a significant detection
of the polarization and be sufficient to derive hints on the primary source of
radiation. A more ambitious program (few Ms) of mapping the giant molecular
clouds could then be carried out to probe with great precision the turbulent
history of Sgr A*, and place important constraints on the composition and
three-dimensional position of the surrounding gas.Comment: 7 pages, 3 figures, 2 tables, accepted for publication in A&
Light bending scenario for accreting black holes in X-ray polarimetry
We discuss a model of an X-ray illuminating source above an accretion disk of
a rotating black hole. Within the so called lamp-post scheme we compute the
expected (observed) polarization properties of the radiation reaching an
observer. We explore the dependencies on model parameters, employing Monte
Carlo radiation transfer computations of the X-ray reflection on the accretion
disk and taking general relativity effects into account. In particular, we
discuss the role of the black hole spin, of the observer viewing angle, and of
the primary X-ray source distance from the black hole. We give several examples
of the resulting polarization degree for two types of exemplary objects -
active galactic nuclei and Galactic black holes. In order to assess potential
observability of the polarization features, we assume the sensitivity of the
proposed New Hard X-ray Mission (NHXM).
We examine the energy range from several keV to ~50 keV, so the iron-line
complex and the Compton hump are included in our model spectra. We find the
resultant polarization degree to increase at the higher end of the studied
energy band, i.e. at >~20 keV. Thus, the best results for polarimetry of
reflection spectra should be achieved at the Compton hump energy region. We
also obtain higher polarization degree for large spin values of the black hole,
small heights of the primary source, and low inclination angles of the
observer.Comment: 17 pages, 14 figures, accepted in Ap
X-ray Polarimetry: a new window on the high energy sky
Polarimetry is widely considered a powerful observational technique in X-ray
astronomy, useful to enhance our understanding of the emission mechanisms,
geometry and magnetic field arrangement of many compact objects. However, the
lack of suitable sensitive instrumentation in the X-ray energy band has been
the limiting factor for its development in the last three decades. Up to now,
polarization measurements have been made exclusively with Bragg diffraction at
45 degrees or Compton scattering at 90 degrees and the only unambiguous
detection of X-ray polarization has been obtained for one of the brightest
object in the X-ray sky, the Crab Nebula. Only recently, with the development
of a new class of high sensitivity imaging detectors, the possibility to
exploit the photoemission process to measure the photon polarization has become
a reality. We will report on the performance of an imaging X-ray polarimeter
based on photoelectric effect. The device derives the polarization information
from the track of the photoelectrons imaged by a finely subdivided Gas Pixel
Detector. It has a great sensitivity even with telescopes of modest area and
can perform simultaneously good imaging, moderate spectroscopy and high rate
timing. Being truly 2D it is non-dispersive and does not require any rotation.
This device is included in the scientific payload of many proposals of
satellite mission which have the potential to unveil polarimetry also in X-rays
in a few years.Comment: Accepted for publication by NIMA. Proceeding of the 1st International
Conference on "Frontiers in Diagnostic Technologies", November 25-27 2009,
Frascati (Italy). 11 pages, 4 figures, 1 table
Spectral and polarimetric characterization of the Gas Pixel Detector filled with dimethyl ether
The Gas Pixel Detector belongs to the very limited class of gas detectors
optimized for the measurement of X-ray polarization in the emission of
astrophysical sources. The choice of the mixture in which X-ray photons are
absorbed and photoelectrons propagate, deeply affects both the energy range of
the instrument and its performance in terms of gain, track dimension and
ultimately, polarimetric sensitivity. Here we present the characterization of
the Gas Pixel Detector with a 1 cm thick cell filled with dimethyl ether (DME)
at 0.79 atm, selected among other mixtures for the very low diffusion
coefficient. Almost completely polarized and monochromatic photons were
produced at the calibration facility built at INAF/IASF-Rome exploiting Bragg
diffraction at nearly 45 degrees. For the first time ever, we measured the
modulation factor and the spectral capabilities of the instrument at energies
as low as 2.0 keV, but also at 2.6 keV, 3.7 keV, 4.0 keV, 5.2 keV and 7.8 keV.
These measurements cover almost completely the energy range of the instrument
and allows to compare the sensitivity achieved with that of the standard
mixture, composed of helium and DME.Comment: 20 pages, 11 figures, 5 tables. Accepted for publication by NIM
Thermal disc emission from a rotating black hole: X-ray polarization signatures
Thermal emission from the accretion disc around a black hole can be
polarized, due to Thomson scattering in a disc atmosphere. In Newtonian space,
the polarization angle must be either parallel or perpendicular to the
projection of the disc axis on the sky. As first pointed out by Stark and
Connors in 1977, General Relativity effects strongly modify the polarization
properties of the thermal radiation as observed at infinity. Among these
effects, the rotation of the polarization angle with energy is particularly
useful as a diagnostic tool.
In this paper, we extend the Stark and Connors calculations by including the
spectral hardening factor, several values of the optical depth of the
scattering atmosphere and rendering the results to the expected performances of
planned X-ray polarimeters. In particular, to assess the perspectives for the
next generation of X-ray polarimeters, we consider the expected sensitivity of
the detectors onboard the planned POLARIX and IXO missions. We assume the two
cases of a Schwarzschild and an extreme Kerr black hole with a standard thin
disc and a scattering atmosphere. We compute the expected polarization degree
and the angle as functions of the energy as they could be measured for
different inclinations of the observer, optical thickness of the atmosphere and
different values of the black hole spin. We assume the thermal emission
dominates the X-ray band. Using the flux level of the microquasar GRS 1915+105
in the thermal state, we calculate the observed polarization.Comment: 8 pages, 7 figures, accepted by MNRA
A strong X-ray polarization signal from the magnetar 1RXS J170849.0-400910
Magnetars are the most strongly magnetized neutron stars, and one of the most promising targets for X-ray polarimetric measurements. We present here the first Imaging X-ray Polarimetry Explorer observation of the magnetar 1RXS J170849.0-400910, jointly analyzed with a new Swift observation and archival NICER data. The total (energy- and phase-integrated) emission in the 2–8 keV energy range is linerarly polarized, at a ∼35% level. The phase-averaged polarization signal shows a marked increase with energy, ranging from ∼20% at 2–3 keV up to ∼80% at 6–8 keV, while the polarization angle remains constant. This indicates that radiation is mostly polarized in a single direction. The spectrum is well reproduced by a combination of either two thermal (blackbody) components or a blackbody and a power law. Both the polarization degree and angle also show a variation with the spin phase, and the former is almost anticorrelated with the source counts in the 2–8 and 2–4 keV bands. We discuss the possible implications and interpretations, based on a joint analysis of the spectral, polarization, and pulsation properties of the source. A scenario in which the surface temperature is not homogeneous, with a hotter cap covered by a gaseous atmosphere and a warmer region in a condensed state, provides a satisfactory description of both the phase- and energy-dependent spectro-polarimetric data. The (comparatively) small size of the two emitting regions, required to explain the observed pulsations, does not allow to reach a robust conclusion about the presence of vacuum birefringence effects
Radiation tests of the Silicon Drift Detectors for LOFT
During the three years long assessment phase of the LOFT mission, candidate
to the M3 launch opportunity of the ESA Cosmic Vision programme, we estimated
and measured the radiation damage of the silicon drift detectors (SDDs) of the
satellite instrumentation. In particular, we irradiated the detectors with
protons (of 0.8 and 11 MeV energy) to study the increment of leakage current
and the variation of the charge collection efficiency produced by the
displacement damage, and we "bombarded" the detectors with hypervelocity dust
grains to measure the effect of the debris impacts. In this paper we describe
the measurements and discuss the results in the context of the LOFT mission.Comment: Proc. SPIE 9144, Space Telescopes and Instrumentation 2014:
Ultraviolet to Gamma Ray, 91446
Simulations of the X-ray imaging capabilities of the Silicon Drift Detectors (SDD) for the LOFT Wide Field Monitor
The Large Observatory For X-ray Timing (LOFT), selected by ESA as one of the
four Cosmic Vision M3 candidate missions to undergo an assessment phase, will
revolutionize the study of compact objects in our galaxy and of the brightest
supermassive black holes in active galactic nuclei. The Large Area Detector
(LAD), carrying an unprecedented effective area of 10 m^2, is complemented by a
coded-mask Wide Field Monitor, in charge of monitoring a large fraction of the
sky potentially accessible to the LAD, to provide the history and context for
the sources observed by LAD and to trigger its observations on their most
interesting and extreme states. In this paper we present detailed simulations
of the imaging capabilities of the Silicon Drift Detectors developed for the
LOFT Wide Field Monitor detection plane. The simulations explore a large
parameter space for both the detector design and the environmental conditions,
allowing us to optimize the detector characteristics and demonstrating the
X-ray imaging performance of the large-area SDDs in the 2-50 keV energy band.Comment: Proceedings of SPIE, Vol. 8443, Paper No. 8443-210, 201
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