404 research outputs found
APEX observations of supernova remnants - I. Non-stationary MHD-shocks in W44
Aims. The interaction of supernova remnants (SNRs) with molecular clouds
gives rise to strong molecular emission in the far-IR and sub-mm wavelength
regimes. The application of MHD shock models in the interpretation of this line
emission can yield valuable information on the energetic and chemical impact of
supernova remnants. Methods. New mapping observations with the APEX telescope
in CO (3-2), (4-3), (6-5), (7-6) and 13CO (3-2) towards two regions in the
supernova remnant W44 are presented. Integrated intensities are extracted on
five different positions, corresponding to local maxima of CO emission. The
integrated intensities are compared to the outputs of a grid of models, which
combine an MHD shock code with a radiative transfer module based on the large
velocity gradient approximation. Results. All extracted spectra show ambient
and line-of-sight components as well as blue- and red-shifted wings indicating
the presence of shocked gas. Basing the shock model fits only on the
highest-lying transitions that unambiguously trace the shock-heated gas, we
find that the observed CO line emission is compatible with non-stationary
shocks and a pre-shock density of 10^4 cm-3. The ages of the modelled shocks
scatter between values of \sim1000 and \sim3000 years. The shock velocities in
W44F are found to lie between 20 and 25 km/s, while in W44E fast shocks (30-35
km/s) as well as slower shocks (\sim20 km/s) are compatible with the observed
spectral line energy diagrams. The pre-shock magnetic field strength components
perpendicular to the line of sight in both regions have values between 100 and
200 \muG. Our best-fitting models allow us to predict the full ladder of CO
transitions, the shocked gas mass in one beam as well as the momentum- and
energy injection.Comment: 20 pages, 13 figures, 13 tables, accepted for publication in
Astronomy and Astrophysic
Shocks in dense clouds. IV. Effects of grain-grain processing on molecular line emission
Grain-grain processing has been shown to be an indispensable ingredient of
shock modelling in high density environments. For densities higher than
\sim10^5 cm-3, shattering becomes a self-enhanced process that imposes severe
chemical and dynamical consequences on the shock characteristics. Shattering is
accompanied by the vaporization of grains, which can directly release SiO to
the gas phase. Given that SiO rotational line radiation is used as a major
tracer of shocks in dense clouds, it is crucial to understand the influence of
vaporization on SiO line emission. We have developed a recipe for implementing
the effects of shattering and vaporization into a 2-fluid shock model,
resulting in a reduction of computation time by a factor \sim100 compared to a
multi-fluid modelling approach. This implementation was combined with an
LVG-based modelling of molecular line radiation transport. Using this model we
calculated grids of shock models to explore the consequences of different
dust-processing scenarios. Grain-grain processing is shown to have a strong
influence on C-type shocks for a broad range of magnetic fields: they become
hotter and thinner. The reduction in column density of shocked gas lowers the
intensity of molecular lines, at the same time as higher peak temperatures
increase the intensity of highly excited transitions compared to shocks without
grain-grain processing. For OH the net effect is an increase in line
intensities, while for CO and H2O it is the contrary. The intensity of H2
emission is decreased in low transitions and increased for highly excited
lines. For all molecules, the highly excited lines become sensitive to the
value of the magnetic field. Although vaporization increases the intensity of
SiO rotational lines, this effect is weakened by the reduced shock width. The
release of SiO early in the hot shock changes the excitation characteristics of
SiO radiation.Comment: Published in Astronomy and Astrophysics (2013). 26 pages, 16 figures,
14 table
SiO excitation from dense shocks in the earliest stages of massive star formation
Molecular outflows are a direct consequence of accretion, and therefore they
represent one of the best tracers of accretion processes in the still poorly
understood early phases of high-mass star formation. Previous studies suggested
that the SiO abundance decreases with the evolution of a massive young stellar
object probably because of a decay of jet activity, as witnessed in low-mass
star-forming regions. We investigate the SiO excitation conditions and its
abundance in outflows from a sample of massive young stellar objects through
observations of the SiO(8-7) and CO(4-3) lines with the APEX telescope. Through
a non-LTE analysis, we find that the excitation conditions of SiO increase with
the velocity of the emitting gas. We also compute the SiO abundance through the
SiO and CO integrated intensities at high velocities. For the sources in our
sample we find no significant variation of the SiO abundance with evolution for
a bolometric luminosity-to-mass ratio of between 4 and 50 . We
also find a weak increase of the SiO(8-7) luminosity with the bolometric
luminosity-to-mass ratio. We speculate that this might be explained with an
increase of density in the gas traced by SiO. We find that the densities
constrained by the SiO observations require the use of shock models that
include grain-grain processing. For the first time, such models are compared
and found to be compatible with SiO observations. A pre-shock density of
cm is globally inferred from these comparisons. Shocks with a
velocity higher than 25 km s are invoked for the objects in our sample
where the SiO is observed with a corresponding velocity dispersion. Our
comparison of shock models with observations suggests that sputtering of
silicon-bearing material (corresponding to less than 10% of the total silicon
abundance) from the grain mantles is occurring.Comment: Accepted for publication by A&
Glycolaldehyde in Perseus young solar analogs
Aims: In this paper we focus on the occurrence of glycolaldehyde (HCOCH2OH)
in young solar analogs by performing the first homogeneous and unbiased study
of this molecule in the Class 0 protostars of the nearby Perseus star forming
region. Methods: We obtained sub-arcsec angular resolution maps at 1.3mm and
1.4mm of glycolaldehyde emission lines using the IRAM Plateau de Bure (PdB)
interferometer in the framework of the CALYPSO IRAM large program. Results:
Glycolaldehyde has been detected towards 3 Class 0 and 1 Class I protostars out
of the 13 continuum sources targeted in Perseus: NGC1333-IRAS2A1,
NGC1333-IRAS4A2, NGC1333-IRAS4B1, and SVS13-A. The NGC1333 star forming region
looks particularly glycolaldehyde rich, with a rate of occurrence up to 60%.
The glycolaldehyde spatial distribution overlaps with the continuum one,
tracing the inner 100 au around the protostar. A large number of lines (up to
18), with upper-level energies Eu from 37 K up to 375 K has been detected. We
derived column densities > 10^15 cm^-2 and rotational temperatures Trot between
115 K and 236 K, imaging for the first time hot-corinos around NGC1333-IRAS4B1
and SVS13-A. Conclusions: In multiple systems glycolaldehyde emission is
detected only in one component. The case of the SVS13-A+B and IRAS4-A1+A2
systems support that the detection of glycolaldehyde (at least in the present
Perseus sample) indicates older protostars (i.e. SVS13-A and IRAS4-A2), evolved
enough to develop the hot-corino region (i.e. 100 K in the inner 100 au).
However, only two systems do not allow us to firmly conclude whether the
primary factor leading to the detection of glycolaldehyde emission is the
environments hosting the protostars, evolution (e.g. low value of Lsubmm/Lint),
or accretion luminosity (high Lint).Comment: A&A, in pres
CSF SerpinA1 in Creutzfeldt\u2013Jakob disease and frontotemporal lobar degeneration
Objective: SerpinA1 (alpha-1 antitrypsin) is an acute inflammatory protein, which seems to play a role in neurodegeneration and neuroinflammation. In Alzheimer\u2019s disease and synucleinopathies, SerpinA1 is overexpressed in the brain and the cerebrospinal fluid (CSF) showing abnormal patterns of its charge isoforms. To date, no comprehensive studies explored SerpinA1 CSF isoforms in Creutzfeldt\u2013Jakob disease (CJD) and frontotemporal lobar degeneration (FTLD). Methods: Using a capillary isoelectric focusing immunoassay, we analyzed CSF SerpinA1 isoforms in control cases (n = 31) and patients with a definite or probable diagnosis of CJD (n=77) or FTLD (n = 30), belonging to several disease subtypes. Results: The overall SerpinA1 signal was significantly higher than in controls in CJD subtypes linked to abnormal prion protein (PrPSc) type 1, such as sporadic CJD (sCJD) MM(V)1, and in FTLD-TDP. Moreover, CJD linked to PrPSc type 1 and FTLD-TAU groups showed a significant relative increase of acidic and basic isoforms in comparison with controls, thereby forming two distinct SerpinA1 isoform profiles. Interpretation: CJD linked to PrPSc type 1 and FTLD show a differential upregulation and post-translational modifications of CSF SerpinA1. Further studies are needed to clarify whether these findings may reflect a common, albeit disease-specific, pathogenetic mechanism related to neurodegeneration
Probing MHD Shocks with high-J CO observations: W28F
Context. Observing supernova remnants (SNRs) and modelling the shocks they
are associated with is the best way to quantify the energy SNRs re-distribute
back into the Interstellar Medium (ISM). Aims. We present comparisons of shock
models with CO observations in the F knot of the W28 supernova remnant. These
comparisons constitute a valuable tool to constrain both the shock
characteristics and pre-shock conditions. Methods. New CO observations from the
shocked regions with the APEX and SOFIA telescopes are presented and combined.
The integrated intensities are compared to the outputs of a grid of models,
which were combined from an MHD shock code that calculates the dynamical and
chemical structure of these regions, and a radiative transfer module based on
the 'large velocity gradient' (LVG) approximation. Results. We base our
modelling method on the higher J CO transitions, which unambiguously trace the
passage of a shock wave. We provide fits for the blue- and red-lobe components
of the observed shocks. We find that only stationary, C-type shock models can
reproduce the observed levels of CO emission. Our best models are found for a
pre-shock density of 104 cm-3, with the magnetic field strength varying between
45 and 100 {\mu}G, and a higher shock velocity for the so-called blue shock
(\sim25 km s-1) than for the red one (\sim20 km s-1). Our models also
satisfactorily account for the pure rotational H2 emission that is observed
with Spitzer.Comment: 8 pages, 6 figures, 1 table, accepted for A&A SOFIA/GREAT Special
Issu
Star Forming Dense Cloud Cores in the TeV {\gamma}-ray SNR RX J1713.7-3946
RX J1713.7-3946 is one of the TeV {\gamma}-ray supernova remnants (SNRs)
emitting synchrotron X rays. The SNR is associated with molecular gas located
at ~1 kpc. We made new molecular observations toward the dense cloud cores,
peaks A, C and D, in the SNR in the 12CO(J=2-1) and 13CO(J=2-1) transitions at
angular resolution of 90". The most intense core in 13CO, peak C, was also
mapped in the 12CO(J=4-3) transition at angular resolution of 38". Peak C shows
strong signs of active star formation including bipolar outflow and a
far-infrared protostellar source and has a steep gradient with a
r^{-2.20.4} variation in the average density within radius r. Peak C and
the other dense cloud cores are rim-brightened in synchrotron X rays,
suggesting that the dense cloud cores are embedded within or on the outer
boundary of the SNR shell. This confirms the earlier suggestion that the X rays
are physically associated with the molecular gas (Fukui et al. 2003). We
present a scenario where the densest molecular core, peak C, survived against
the blast wave and is now embedded within the SNR. Numerical simulations of the
shock-cloud interaction indicate that a dense clump can indeed survive shock
erosion, since shock propagation speed is stalled in the dense clump.
Additionally, the shock-cloud interaction induces turbulence and magnetic field
amplification around the dense clump that may facilitate particle acceleration
in the lower-density inter-clump space leading to the enhanced synchrotron X
rays around dense cores.Comment: 22 pages, 7 figures, to accepted in The Astrophysical Journal. A full
color version with higher resolution figures is available at
http://www.a.phys.nagoya-u.ac.jp/~sano/ApJ10/ms_sano.pd
PACS and SPIRE photometer maps of M33: First results of the Herschel M33 extended survey (HERM33ES)
Within the framework of the HERM33ES key project, we are studying the star
forming interstellar medium in the nearby, metal-poor spiral galaxy M33,
exploiting the high resolution and sensitivity of Herschel. We use PACS and
SPIRE maps at 100, 160, 250, 350, and 500 micron wavelength, to study the
variation of the spectral energy distributions (SEDs) with galacto-centric
distance. Detailed SED modeling is performed using azimuthally averaged fluxes
in elliptical rings of 2 kpc width, out to 8 kpc galacto-centric distance.
Simple isothermal and two-component grey body models, with fixed dust
emissivity index, are fitted to the SEDs between 24 and 500 micron using also
MIPS/Spitzer data, to derive first estimates of the dust physical conditions.
The far-infrared and submillimeter maps reveal the branched, knotted spiral
structure of M33. An underlying diffuse disk is seen in all SPIRE maps (250-500
micron). Two component fits to the SEDs agree better than isothermal models
with the observed, total and radially averaged flux densities. The two
component model, with beta fixed at 1.5, best fits the global and the radial
SEDs. The cold dust component clearly dominates; the relative mass of the warm
component is less than 0.3% for all the fits. The temperature of the warm
component is not well constrained and is found to be about 60K plus/minus 10K.
The temperature of the cold component drops significantly from about 24K in the
inner 2 kpc radius to 13K beyond 6 kpc radial distance, for the best fitting
model. The gas-to-dust ratio for beta=1.5, averaged over the galaxy, is higher
than the solar value by a factor of 1.5 and is roughly in agreement with the
subsolar metallicity of M33.Comment: 5 pages, 3 figures, accepted for publication in the A&A Herschel
Special Issu
Cool and warm dust emission from M33 (HerM33es)
We study the far-infrared emission from the nearby spiral galaxy M33 in order
to investigate the dust physical properties such as the temperature and the
luminosity density across the galaxy. Taking advantage of the unique wavelength
coverage (100, 160, 250, 350 and 500 micron) of the Herschel Space Observatory
and complementing our dataset with Spitzer-IRAC 5.8 and 8 micron and
Spitzer-MIPS 24 and 70 micron data, we construct temperature and luminosity
density maps by fitting two modified blackbodies of a fixed emissivity index of
1.5. We find that the 'cool' dust grains are heated at temperatures between 11
and 28 K with the lowest temperatures found in the outskirts of the galaxy and
the highest ones in the center and in the bright HII regions. The
infrared/submillimeter total luminosity (5 - 1000 micron) is estimated to be
1.9x10^9 Lsun. 59% of the total luminosity of the galaxy is produced by the
'cool' dust grains (~15 K) while the rest 41% is produced by 'warm' dust grains
(~55 K). The ratio of the cool-to-warm dust luminosity is close to unity
(within the computed uncertainties), throughout the galaxy, with the luminosity
of the cool dust being slightly enhanced in the center of the galaxy.
Decomposing the emission of the dust into two components (one emitted by the
diffuse disk of the galaxy and one emitted by the spiral arms) we find that the
fraction of the emission in the disk in the mid-infrared (24 micron) is 21%,
while it gradually rises up to 57% in the submillimeter (500 micron). We find
that the bulk of the luminosity comes from the spiral arm network that produces
70% of the total luminosity of the galaxy with the rest coming from the diffuse
dust disk. The 'cool' dust inside the disk is heated at a narrow range of
temperatures between 18 and 15 K (going from the center to the outer parts of
the galaxy).Comment: 12 pages, 14 figures, accepted for publication in A&
VizieR Online Data Catalog: Glycolaldehyde in Perseus young solar analogs (De Simone+, 2017)
Glycolaldehyde spatial distributions towards NGC1333-IRAS2A1, NGC1333-IRAS4A, NGC1333-IRAS4B1, and NGC1333 SVS13-A. The glycolaldehyde distribution refers to (1) the sum of the 76,2-65,1 and 76,1-65,2 emission with (220.2GHz, Eu=37K), and (2) the 222,21-211,20 emission (232.3GHz, Eu=135K). (2 data files). <P /
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