187 research outputs found
A Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 4151
We disentangle X-ray disk reflection from complex line-of-sight absorption in
the nearby Seyfert NGC 4151, using a suite of Suzaku, NuSTAR, and XMM-Newton
observations. Extending upon earlier published work, we pursue a physically
motivated model using the latest angle-resolved version of the lamp-post
geometry reflection model relxillCp_lp together with a Comptonization
continuum. We use the long-look simultaneous Suzaku/NuSTAR observation to
develop a baseline model wherein we model reflected emission as a combination
of lamp-post components at the heights of 1.2 and 15.0 gravitational radii. We
argue for a vertically extended corona as opposed to two compact and distinct
primary sources. We find two neutral absorbers (one full-covering and one
partial-covering), an ionized absorber (), and a highly-ionized
ultra-fast outflow, which have all been reported previously. All analyzed
spectra are well described by this baseline model. The bulk of the spectral
variability between 1 keV and 6 keV can be accounted for by changes in the
column density of both neutral absorbers, which appear to be degenerate and
inversely correlated with the variable hard continuum component flux. We track
variability in absorption on both short (2 d) and long (1 yr) timescales;
the observed evolution is either consistent with changes in the absorber
structure (clumpy absorber at distances ranging from the broad line region
(BLR) to the inner torus or a dusty radiatively driven wind) or a geometrically
stable neutral absorber that becomes increasingly ionized at a rising flux
level. The soft X-rays below 1 keV are dominated by photoionized emission from
extended gas that may act as a warm mirror for the nuclear radiation.Comment: 21 pages, 19 figures, 8 tables, accepted for publication by A&
A redshifted Fe K line from the unusual gamma-ray source PMN J1603-4904
Multiwavelength observations have revealed the highly unusual properties of
the gamma-ray source PMN J1603-4904, which are difficult to reconcile with any
other well established gamma-ray source class. The object is either a very
atypical blazar or compact jet source seen at a larger angle to the line of
sight. In order to determine the physical origin of the high-energy emission
processes in PMN J1603-4904, we study the X-ray spectrum in detail. We
performed quasi-simultaneous X-ray observations with XMM-Newton and Suzaku in
2013 September, resulting in the first high signal-to-noise X-ray spectrum of
this source. The 2-10 keV X-ray spectrum can be well described by an absorbed
power law with an emission line at 5.440.05 keV (observed frame).
Interpreting this feature as a K{\alpha} line from neutral iron, we determine
the redshift of PMN J1603-4904 to be z=0.180.01, corresponding to a
luminosity distance of 87254 Mpc. The detection of a redshifted X-ray
emission line further challenges the original BL Lac classification of PMN
J1603-4904. This result suggests that the source is observed at a larger angle
to the line of sight than expected for blazars, and thus the source would add
to the elusive class of gamma-ray loud misaligned-jet objects, possibly a
{\gamma}-ray bright young radio galaxy.Comment: 5 pages, 1 figure, A&A accepte
The properties of the clumpy torus and BLR in the polar-scattered Seyfert 1 galaxy ESO 323-G77 through X-ray absorption variability
We report results from multi-epoch X-ray observations of the polar-scattered
Seyfert 1 galaxy ESO 323-G77. The source exhibits remarkable spectral
variability from months to years timescales. The observed spectral variability
is entirely due to variations of the column density of a neutral absorber
towards the intrinsic nuclear continuum. The column density is generally
Compton-thin ranging from a few times 10 cm to a few times
10 cm. However, one observation reveals a Compton-thick state
with column density of the order of 1.5 10 cm. The
observed variability offers a rare opportunity to study the properties of the
X-ray absorber(s) in an active galaxy. We identify variable X-ray absorption
from two different components, namely (i) a clumpy torus whose individual
clumps have a density of 1.7 10 cm and an average
column density of 4 10 cm, and (ii) the broad
line region (BLR), comprising individual clouds with density of 0.1-8
10 cm and column density of 10-10 cm. The
derived properties of the clumpy torus can also be used to estimate the torus
half-opening angle, which is of the order of 47 . We also confirm the
previously reported detection of two highly ionized warm absorbers with outflow
velocities of 1000-4000 km s. The observed outflow velocities are
consistent with the Keplerian/escape velocity at the BLR. Hence, the warm
absorbers may be tentatively identified with the warm/hot inter-cloud medium
which ensures that the BLR clouds are in pressure equilibrium with their
surroundings. The BLR line-emitting clouds may well be the cold, dense clumps
of this outflow, whose warm/hot phase is likely more homogeneous, as suggested
by the lack of strong variability of the warm absorber(s) properties during our
monitoring.Comment: 15 pages, 4 tables, and 9 figures. Accepted for publication in MNRA
Sub-milliarcsecond imaging of a bright flare and ejection event in the extragalactic jet 3C 111
Flares in radio-loud AGN are thought to be associated with the injection of
fresh plasma into the compact jet base. Such flares are usually strongest and
appear earlier at shorter radio wavelengths. Hence, VLBI at mm-wavelengths is
best suited to study the earliest structural changes of compact jets associated
with emission flares. We study the morphological changes of the parsec-scale
jet in the nearby (z=0.049) gamma-ray bright radio galaxy 3C111 following a
flare that developed into a major radio outburst in 2007. We analyse three
successive observations of 3C111 at 86 GHz with the Global mm-VLBI Array (GMVA)
between 2007 and 2008 which yield a very high angular resolution of ~45muas. In
addition, we make use of single-dish radio flux density measurements from the
F-GAMMA and POLAMI programmes, archival single-dish and VLBI data. We resolve
the flare into multiple plasma components with a distinct morphology resembling
a bend in an otherwise remarkably straight jet. The flare-associated features
move with apparent velocities of ~4.0c to ~4.5c and can be traced also at lower
frequencies in later epochs. Near the base of the jet, we find two bright
features with high brightness temperatures up to ~10^11K, which we associate
with the core and a stationary feature in the jet. The flare led to multiple
new jet components indicative of a dynamic modulation during the ejection. We
interpret the bend-like feature as a direct result of the outburst which makes
it possible to trace the transverse structure of the jet. In this scenario, the
components follow different paths in the jet stream consistent with
expectations for a spine-sheath structure, which is not seen during
intermediate levels of activity. The possibility of coordinated multiwavelength
observations during a future bright radio flare in 3C111 makes this source an
excellent target for probing the radio-gamma-ray connection.Comment: 11 pages, 7 figures, accepted for publication by Astronomy &
Astrophysic
The Soft-Excess in Mrk 509: Warm Corona or Relativistic Reflection?
We present the analysis of the first NuSTAR observations ( ks),
simultaneous with the last SUZAKU observations ( ks), of the active
galactic nucleus of the bright Seyfert 1 galaxy Mrk 509. The time-averaged
spectrum in the keV X-ray band is dominated by a power-law continuum
(), a strong soft excess around 1 keV, and signatures of
X-ray reflection in the form of Fe K emission ( keV), an Fe K
absorption edge ( keV), and a Compton hump due to electron scattering
( keV). We show that these data can be described by two very
different prescriptions for the soft excess: a warm ( keV) and
optically thick () Comptonizing corona, or a relativistically
blurred ionized reflection spectrum from the inner regions of the accretion
disk. While these two scenarios cannot be distinguished based on their fit
statistics, we argue that the parameters required by the warm corona model are
physically incompatible with the conditions of standard coronae. Detailed
photoionization calculations show that even in the most favorable conditions,
the warm corona should produce strong absorption in the observed spectrum. On
the other hand, while the relativistic reflection model provides a satisfactory
description of the data, it also requires extreme parameters, such as maximum
black hole spin, a very low and compact hot corona, and a very high density for
the inner accretion disk. Deeper observations of this source are thus necessary
to confirm the presence of relativistic reflection, and to further understand
the nature of its soft excess.Comment: Accepted for publication in ApJ, 18 pages, 7 figure
Sub-milliarcsecond imaging of a bright flare and ejection event in the extragalactic jet 3C 111
ContextFlares in radio-loud active galactic nuclei are thought to be associated with the injection of fresh plasma into the compact jet base. Such flares are usually strongest and appear earlier at shorter radio wavelengths. Hence, very long baseline interferometry (VLBI) at millimeter(mm)-wavelengths is the best-suited technique for studying the earliest structural changes of compact jets associated with emission flares. AimsWe study the morphological changes of the parsec-scale jet in the nearby (z = 0.049) γ-ray bright radio galaxy 3C 111 following a flare that developed into a major radio outburst in 2007. Methods\ua0We analyse three successive observations of 3C 111 at 86 GHz with the Global mm-VLBI Array (GMVA) between 2007 and 2008 which yield a very high angular resolution of ∼45 μas. In addition, we make use of single-dish radio flux density measurements from the F-GAMMA and POLAMI programmes, archival single-dish and VLBI data. ResultsWe resolve the flare into multiple plasma components with a distinct morphology resembling a bend in an otherwise remarkably straight jet. The flare-associated features move with apparent velocities of ∼4.0c to ∼4.5c and can be traced also at lower frequencies in later epochs. Near the base of the jet, we find two bright features with high brightness temperatures up to ∼1011 K, which we associate with the core and a stationary feature in the jet. ConclusionsThe flare led to multiple new jet components indicative of a dynamic modulation during the ejection. We interpret the bend-like feature as a direct result of the outburst which makes it possible to trace the transverse structure of the jet. In this scenario, the components follow different paths in the jet stream consistent with expectations for a spine-sheath structure, which is not seen during intermediate levels of activity. The possibility of coordinated multiwavelength observations during a future bright radio flare in 3C 111 makes this source an excellent target for probing the radio-γ-ray connection
A new lepto-hadronic model applied to the first simultaneous multiwavelength data set for Cygnus X-1
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