56 research outputs found
3D Simulations of the Thermal X-ray Emission from Young Supernova Remnants Including Efficient Particle Acceleration
Supernova remnants (SNRs) are believed to be the major contributors to
Galactic cosmic rays. The detection of non-thermal emission from SNRs
demonstrates the presence of energetic particles, but direct signatures of
protons and other ions remain elusive. If these particles receive a sizeable
fraction of the explosion energy, the morphological and spectral evolution of
the SNR must be modified. To assess this, we run 3D hydrodynamic simulations of
a remnant coupled with a non-linear acceleration model. We obtain the
time-dependent evolution of the shocked structure, impacted by the
Rayleigh-Taylor hydrodynamic instabilities at the contact discontinuity and by
the back-reaction of particles at the forward shock. We then compute the
progressive temperature equilibration and non-equilibrium ionization state of
the plasma, and its thermal emission in each cell. This allows us to produce
the first realistic synthetic maps of the projected X-ray emission from the
SNR. Plasma conditions (temperature, ionization age) can vary widely over the
projected surface of the SNR, especially between the ejecta and the ambient
medium owing to their different composition. This demonstrates the need for
spatially-resolved spectroscopy. We find that the integrated emission is
reduced with particle back-reaction, with the effect being more significant for
the highest photon energies. Therefore different energy bands, corresponding to
different emitting elements, probe different levels of the impact of particle
acceleration. Our work provides a framework for the interpretation of SNR
observations with current X-ray missions (Chandra, XMM-Newton, Suzaku) and with
upcoming X-ray missions (such as Astro-H).Comment: Accepted for publication in ApJ. Figures quality has been reduced for
the arXi
XMM-Newton Large Program on SN1006 - II: Thermal Emission
Based on the XMM-Newton large program on SN1006 and our newly developed
spatially resolved spectroscopy tools (Paper~I), we study the thermal emission
from ISM and ejecta of SN1006 by analyzing the spectra extracted from 583
tessellated regions dominated by thermal emission. With some key improvements
in spectral analysis as compared to Paper~I, we obtain much better spectral
fitting results with less residuals. The spatial distributions of the thermal
and ionization states of the ISM and ejecta show different features, which are
consistent with a scenario that the ISM (ejecta) is heated and ionized by the
forward (reverse) shock propagating outward (inward). Different elements have
different spatial distributions and origins, with Ne mostly from the ISM, Si
and S from the ejecta, and O and Mg from both ISM and ejecta. Fe L-shell lines
are only detected in a small shell-like region SE to the center of SN1006,
indicating that most of the Fe-rich ejecta has not yet or just recently been
reached by the reverse shock. The overall ejecta abundance patterns for most of
the heavy elements, except for Fe and sometimes S, are consistent with typical
Type~Ia SN products. The NW half of the SNR interior probably represents a
region with turbulently mixed ISM and ejecta, so has enhanced emission from O,
Mg, Si, S, lower ejecta temperature, and a large diversity of ionization age.
In addition to the asymmetric ISM distribution, an asymmetric explosion of the
progenitor star is also needed to explain the asymmetric ejecta distribution.Comment: 9 pages, 7 figures, 1 table, MNRAS in pres
XMM-Newton Large Program on SN1006 - I: Methods and Initial Results of Spatially-Resolved Spectroscopy
Based on our newly developed methods and the XMM-Newton large program of
SN1006, we extract and analyze the spectra from 3596 tessellated regions of
this SNR each with 0.3-8 keV counts . For the first time, we map out
multiple physical parameters, such as the temperature (), electron density
(), ionization parameter (), ionization age (), metal
abundances, as well as the radio-to-X-ray slope () and cutoff frequency
() of the synchrotron emission. We construct probability
distribution functions of and , and model them with several
Gaussians, in order to characterize the average thermal and ionization states
of such an extended source. We construct equivalent width (EW) maps based on
continuum interpolation with the spectral model of each regions. We then
compare the EW maps of OVII, OVIII, OVII K, Ne, Mg, SiXIII,
SiXIV, and S lines constructed with this method to those constructed with
linear interpolation. We further extract spectra from larger regions to confirm
the features revealed by parameter and EW maps, which are often not directly
detectable on X-ray intensity images. For example, O abundance is consistent
with solar across the SNR, except for a low-abundance hole in the center. This
"O Hole" has enhanced OVII K and Fe emissions, indicating
recently reverse shocked ejecta, but also has the highest , indicating
forward shocked ISM. Therefore, a multi-temperature model is needed to
decompose these components. The asymmetric metal distributions suggest there is
either an asymmetric explosion of the SN or an asymmetric distribution of the
ISM.Comment: 25 pages, 18 figures, 4 tables, MNRAS, in pres
A fresh perspective on the 3-D dynamics of Tycho's supernova remnant: ejecta asymmetries in X-rays
450 years after the explosion of the Type Ia SN1572, the dynamics of the
Tycho supernova remnant can give us keys to understand the explosion mechanism
and the interaction of the remnant with the interstellar medium. To probe the
asymmetries and the evolution of the SNR, we track the ejecta dynamics using
new methods applied to the deep X-ray observations available in the Chandra
space telescope archive. For the line of sight velocity measurement Vz, we use
the Doppler effect focused on the bright Si line in the 1.6-2.1 keV band. Using
the component separation tool General Morphological Component Analysis (GMCA),
we successfully disentangle the red and blueshifted Si ejecta emission. This
allows us to reconstruct a map of the peak energy of the Si line with a total
coverage of the SNR at a 2'' resolution and a proxy of the velocity in the line
of sight. For the proper motions in the plane of the sky Vxy, we develop a new
method, named Poisson Optical Flow, to measure the displacement of 2D features
between the observations of 2003 and 2009. The result is a field of 1700
velocity vectors covering the entire SNR. These exhaustive 3D velocity
measurements reveal the complex and patchy dynamics of the SNR. At the
large-scale, an asymmetry with the North being dominantly blueshifted and the
South redshifted is observed. The proper motion vector field Vxy highlights
different dynamics between the East and the West parts of the SNR. The eastern
velocity field is more disturbed by external inhomogeneities and the South-East
ejecta knot. In particular, a slow-down is observed in the North-East which
could be due to the interaction with higher densities as seen in other
wavelengths. The vector field is also used to backtrace the center of the
explosion which is then compared with potential stellar progenitors distances
from the latest Gaia DR3, leaving only stars B and E as possible candidates.Comment: Accepted for publication in A&A. 18 pages, 12 figure
The discovery of a new non-thermal X-ray filament near the Galactic Centre
We report the discovery by XMM-Newton and Chandra of a hard extended X-ray
source (XMM J174540-2904.5) associated with a compact non-thermal radio
filament (the Sgr A-E `wisp'=1LC 359.888-0.086= G359.88-0.07), which is located
within ~4 arcmin of the Galactic Centre. The source position is also coincident
with the peak of the molecular cloud, M -0.13-0.08 (the `20 km/s' cloud). The
X-ray spectrum is non-thermal with an energy index of 1.0 (+1.1 -0.9) and
column density of 38 (+7 -11) x 10^22 H/cm2. The observed 2--10 keV flux of 4 x
10^-13 erg/s/cm2 converts to an unabsorbed X-ray luminosity of 1 x 10^34 erg/s
assuming a distance of 8.0 kpc. The high column density strongly suggests that
this source is located in or behind the Galactic Centre Region. Taking account
of the broad-band spectrum, as well as the source morphology and the positional
coincidence with a molecular cloud, we concluded that both the radio and X-ray
emission are the result of synchrotron radiation. This is the first time a
filamentary structure in the Galactic Centre Region. has been shown,
unequivocally, to have a non-thermal X-ray spectrum.Comment: 5 pages, 4 figures, Accepted for publication in MNRAS, also found in
http://www.star.le.ac.uk/~mas/research/paper/#Sakano2002mnra
Unusual X-ray transients in the Galactic Centre
We report the discovery in the Galactic Centre region of two hard X-ray
sources, designated as XMM J174457-2850.3 and XMM J174544-2913.0, which
exhibited flux variations in the 2--10 keV band in excess of a factor of 100 in
observations spanning roughly a year. In both cases the observed hydrogen
column density is consistent with a location near to the Galactic Centre,
implying peak X-ray luminosities of ~5 x 10^34 erg/s. These objects may
represent a new population of transient source with very different properties
to the much more luminous Galactic Centre transients associated with neutron
star and black-hole binary systems. Spectral analysis shows that XMM
J174457-2850.3 has relatively weak iron-line emission set against a very hard
continuum. XMM J174544-2913.0, on the other hand, has an extremely strong
K-line from helium-like iron with an equivalent width of ~2.4keV. The nature of
the latter source is of particular interest. Does it represent an entirely new
class of object or does it correspond to a known class of source in a very
extreme configuration?Comment: 9 pages, 5 figures, to appear in MNRAS, figures with full resolution
are available at
http://www.star.le.ac.uk/~mas/research/paper/#Sakano2004mnra
Thermal and Nonthermal Emission from the Forward Shock in Tycho's Supernova Remnant
We present Chandra X-ray images of Tycho's supernova remnant that delineate
its outer shock as a thin, smooth rim along the straight northeastern edge and
most of the circular western half. The images also show that the Si and S
ejecta are highly clumpy, and have reached near the forward shock at numerous
locations. Most of the X-ray spectra that we examine along the rim show
evidence of line emission from Si and S ejecta, while the continuum is
well-represented by either a thermal or nonthermal model. If the continuum is
assumed to be thermal, the electron temperatures at the rim are all similar at
about 2 keV, while the ionization ages are very low, because of the overall
weakness of the line emission. These electron temperatures are substantially
below those expected for equilibration of the electron and ion temperatures,
assuming shock velocities inferred from radio and X-ray expansion measurements;
the electron to mean temperature ratios are <~0.1-0.2, indicating that
collisionless heating of the electrons at the shock is modest. The nonthermal
contribution to these spectra may be important, but cannot be strongly
constrained by these data. It could account for as much as half of the flux in
the 4-6 keV energy range, based on an extrapolation of the hard X-ray spectrum
above 10 keV.Comment: ApJ, in press; 32 pages LaTeX, 9 postscript figures; replaced version
to better match ApJ versio
The warm interstellar medium around the Cygnus Loop
Observations of the oxygen lines [OII]3729 and [OIII]5007 in the medium
immediately beyond the Cygnus Loop supernova remnant were carried out with the
scanning Fabry-P\'erot spectrophotometer ESOP. Both lines were detected in
three different directions - east, northeast and southwest - and up to a
distance of 15 pc from the shock front. The ionized medium is in the immediate
vicinity of the remnant, as evinced by the smooth brightening of both lines as
the adiabatic shock transition (defined by the X-ray perimeter) is crossed.
These lines are usually brighter around the Cygnus Loop than in the general
background in directions where the galactic latitude is above 5 degrees. There
is also marginal (but significant) evidence that the degree of ionization is
somewhat larger around the Cygnus Loop. We conclude that the energy necessary
to ionize this large bubble of gas could have been supplied by an O8 or O9 type
progenitor or the particles heated by the expanding shock front. The second
possibility, though highly atractive, would have to be assessed by extensive
modelling.Comment: 18 pages, 8 figures, ApJ 512 in pres
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