336 research outputs found
Advanced Microwave Precipitation Radiometer (AMPR) for remote observation of precipitation
The design, development, and tests of the Advanced Microwave Precipitation Radiometer (AMPR) operating in the 10 to 85 GHz range specifically for precipitation retrieval and mesoscale storm system studies from a high altitude aircraft platform (i.e., ER-2) are described. The primary goals of AMPR are the exploitation of the scattering signal of precipitation at frequencies near 10, 19, 37, and 85 GHz together to unambiguously retrieve precipitation and storm structure and intensity information in support of proposed and planned space sensors in geostationary and low earth orbit, as well as storm-related field experiments. The development of AMPR will have an important impact on the interpretation of microwave radiances for rain retrievals over both land and ocean for the following reasons: (1) A scanning instrument, such as AMPR, will allow the unambiguous detection and analysis of features in two dimensional space, allowing an improved interpretation of signals in terms of cloud features, and microphysical and radiative processes; (2) AMPR will offer more accurate comparisons with ground-based radar data by feature matching since the navigation of the ER-2 platform can be expected to drift 3 to 4 km per hour of flight time; and (3) AMPR will allow underflights of the SSM/I satellite instrument with enough spatial coverage at the same frequencies to make meaningful comparisons of the data for precipitation studies
An original interferometric study of NGC 1068 with VISIR BURST mode images
We present 12.8 microns images of the core of NGC 1068 obtained with the
BURST mode of the VLT/VISIR. We trace structures under the diffraction limit of
one UT and we investigate the link between dust in the vicinity of the central
engine of NGC 1068, recently resolved by interferometry with MIDI, and more
extended structures. This step is mandatory for a multi-scale understanding of
the sources of mid-infrared emission in AGNs. A speckle processing of VISIR
BURST mode images was performed to extract very low spatial-frequency
visibilities, first considering the full field of VISIR BURST mode images and
then limiting it to the mask used for the acquisition of MIDI data. Extracted
visibilities are reproduced with a multi-component model. We identify two major
sources of emission: one compact < 85 mas, associated with the dusty torus, and
an elliptical one, (< 140) mas x 1187 mas at P.A.=-4 degrees from N to E. This
is consistent with previous deconvolution processes. The combination with MIDI
data reveals the close environment of the dusty torus to contribute to about 83
percent of the MIR flux seen by MIDI. This strong contribution has to be
considered in modeling long baseline interferometric data. It must be related
to the NS elongated component which is thought to originate from individually
unresolved dusty clouds and is located inside the ionization cone. Low
temperatures of the dusty torus are not challenged, emphasizing the scenarios
of clumpy torus.Comment: 10 pages, 7 figures, accepted for publication in A&
Birth and death processes with absorption
Spectral measures and transition probabilities of birth and death processes with λ0=μ0=0 are obtained as limite when λ0→0+ of the corresponding quantities. In particular the case of finite population is discussed in full detail. Pure birth and death processes are used to derive an inequality for Dirichlet polynomials
A Multi-Wavelength Infrared Study of NGC 891
We present a multi-wavlength infrared study of the nearby, edge-on, spiral
galaxy NGC 891. We have examined 20 independent, spatially resolved IR images
of this galaxy, 14 of which are newly reduced and/or previously unpublished
images. These images span a wavelength regime from 1.2 microns in which the
emission is dominated by cool stars, through the MIR, in which emission is
dominated by PAHs, to 850 microns, in which emission is dominated by cold dust
in thermal equilibrium with the radiation field. The changing morphology of the
galaxy with wavelength illustrates the changing dominant components. We detect
extra-planar dust emission in this galaxy, consistent with previously published
results, but now show that PAH emission is also in the halo, to a vertical
distance of z >= 2.5 kpc. We compare the vertical extents of various components
and find that the PAHs (from 7.7 and 8 micron data) and warm dust (24 microns)
extend to smaller z heights than the cool dust (450 microns). For six locations
in the galaxy for which the S/N was sufficient, we present SEDs of the IR
emission, including two in the halo - the first time a halo SED in an external
galaxy has been presented. We have modeled these SEDs and find that the PAH
fraction is similar to Galactic values (within a factor of two), with the
lowest value at the galaxy's center, consistent with independent results of
other galaxies. In the halo environment, the fraction of dust exposed to a
colder radiation field, is of order unity, consistent with an environment in
which there is no star formation. The source of excitation is likely from
photons escaping from the disk.Comment: 24 pages, 17 figures, 7 tables, accepted for publication in MNRA
The effects of star formation on the low-metallicity ISM: NGC4214 mapped with Herschel/PACS spectroscopy
We present Herschel/PACS spectroscopic maps of the dwarf galaxy NC4214
observed in 6 far infrared fine-structure lines: [C II] 158mu, [O III] 88mu, [O
I] 63mu, [O I] 146mu, [N II] 122mu, and [N II] 205mu. The maps are sampled to
the full telescope spatial resolution and reveal unprecedented detail on ~ 150
pc size scales. We detect [C II] emission over the whole mapped area, [O III]
being the most luminous FIR line. The ratio of [O III]/[C II] peaks at about 2
toward the sites of massive star formation, higher than ratios seen in dusty
starburst galaxies. The [C II]/CO ratios are 20 000 to 70 000 toward the 2
massive clusters, which are at least an order of magnitude larger than spiral
or dusty starbursts, and cannot be reconciled with single-slab PDR models.
Toward the 2 massive star-forming regions, we find that L[CII] is 0.5 to 0.8%
of the LTIR . All of the lines together contribute up to 2% of LTIR . These
extreme findings are a consequence of the lower metallicity and young,
massive-star formation commonly found in dwarf galaxies. These conditions
promote large-scale photodissociation into the molecular reservoir, which is
evident in the FIR line ratios. This illustrates the necessity to move to
multiphase models applicable to star-forming clusters or galaxies as a whole.Comment: Accepted for publication in the A&A Herschel Special Issu
Sustainable approaches for drug repurposing in rare diseases: recommendations from the IRDiRC Task Force
Drug repurposing represents a real opportunity to address unmet needs and improve the lives of rare disease patients. It is often presented as a faster, safer and cheaper path for bringing drugs into new indications. However, several economic, regulatory and scientific barriers can impede the successful repurposing of drugs for rare diseases. The International Rare Diseases Research Consortium (IRDiRC) set up the Task Force on Sustainable Models in Drug Repurposing with the objective of identifying key factors for achieving sustainable repurposing approaches in rare diseases. In order to help inform expert opinion, the Task Force investigated six cases of medicinal products repurposed into new rare indications and four cases of ongoing development programs. A questionnaire addressing the major steps of the repurposing approach was developed by the Task Force and sent to contact points of the organizations. In addition, interviews were conducted with the relevant organization representatives to conduct a deeper dive into the sustainability of the repurposing approach for each of the selected cases. Based on the collective experience of the members of the Task Force and the output from the questionnaires/interviews, we have identified ten key factors that should be considered by those embarking on repurposing projects. These factors include the identification of unmet patient needs and partnership with patients, collection of evidence concerning disease prevalence, patient numbers, drug pharmacology and disease etiology, drug industrial property status, off-label or compounding use, data from past clinical studies and needs for extended non-clinical and clinical studies. The development of a collaborative funding framework and early discussion with regulators and payers are additional factors to implement early in the development of sustainable drug repurposing projects
ALMA Resolves 30 Doradus: Sub-parsec Molecular Cloud Structure Near the Closest Super-Star Cluster
We present ALMA observations of 30 Doradus -- the highest resolution view of
molecular gas in an extragalactic star formation region to date (~0.4pc x
0.6pc). The 30Dor-10 cloud north of R136 was mapped in 12CO 2-1, 13CO 2-1, C18O
2-1, 1.3mm continuum, the H30alpha recombination line, and two H2CO 3-2
transitions. Most 12CO emission is associated with small filaments and clumps
(<1pc, ~1000 Msun at the current resolution). Some clumps are associated with
protostars, including "pillars of creation" photoablated by intense radiation
from R136. Emission from molecular clouds is often analyzed by decomposition
into approximately beam-sized clumps. Such clumps in 30 Doradus follow similar
trends in size, linewidth, and surface density to Milky Way clumps. The 30
Doradus clumps have somewhat larger linewidths for a given size than predicted
by Larson's scaling relation, consistent with pressure confinement. They extend
to higher surface density at a given size and linewidth compared to clouds
studied at 10pc resolution. These trends are also true of clumps in Galactic
infrared-dark clouds; higher resolution observations of both environments are
required. Consistency of clump masses calculated from dust continuum, CO, and
the virial theorem reveals that the CO abundance in 30 Doradus clumps is not
significantly different from the LMC mean, but the dust abundance may be
reduced by ~2. There are no strong trends in clump properties with distance
from R136; dense clumps are not strongly affected by the external radiation
field, but there is a modest trend towards lower dense clump filling fraction
deeper in the cloud.Comment: accepted to Ap
Spectral characteristics of water megamaser galaxies II: ESO 103-G035, TXS 2226-184, and IC 1481
Long-slit optical emission-line spectra of the H2O megamaser galaxies ESO
103-G03, TXS 2226-184, and IC 1481 are evaluated in order to look for
characteristics typical for water-megamaser galaxies. We present rotation
curves, line ratios, electron densities, temperatures, and Hbeta luminosities.
The successful line-profile decompositions rest on d-Lorentzians with an
additional parameter d to adjust the wings, rather than Gaussians or
Lorentzians as basic functions. No significant velocity gradient is found along
the major axis in the innermost 2 kpc of TXS 2226-184. IC 1481 reveals a
spectrum suggestive of a vigorous starburst in the central kiloparsec 10^8
years ago. None of the three galaxies shows any hints for outflows nor special
features which could give clues to the presence of H2O megamaser emission. The
galaxies are of normal Seyfert-2 (ESO 103-G035) or LINER (TXS 2226-184, IC
1481) type.Comment: 12 pages, 14 figures, accepted for publication in A&A, corrected
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The small dispersion of the mid IR -- hard X-ray correlation in AGN
Context: We investigate mid-infrared and X-ray properties of the dusty torus
in unification scenarios for active galactic nuclei.
Aims: We use the relation between mid IR and hard X-ray luminosities to
constrain AGN unification scenarios.
Methods: With VISIR at the VLT, we have obtained the currently highest
angular resolution (0".35 FWHM) narrow-band mid infrared images of the nuclei
of 8 nearby Seyfert galaxies. Combining these observations with X-ray data from
the literature we study the correlation between their mid IR and hard X-ray
luminosities.
Results: We find that the rest frame 12.3 mircon (L_MIR) and 2-10 keV (L_X)
luminosities are correlated at a highly significant level. The best fit
power-law to our data is log L_MIR \propto (1.60 \pm 0.22) log L_X, showing a
much smaller dispersion than earlier studies.
Conclusions: The similarity in the og L_MIR / log L_X ratio between Sy1s and
Sy2s even using high angular resolution MIR data implies that the similarity is
intrinsic to AGN and not caused by contamination from extra-nuclear emission.
This supports clumpy torus models. The exponent of the correlation constrains
the inner geometry of the torus.Comment: 5 pages, 3 figures, accepted for publication in Astronomy &
Astrophysic
Bianchi type II,III and V diagonal Einstein metrics re-visited
We present, for both minkowskian and euclidean signatures, short derivations
of the diagonal Einstein metrics for Bianchi type II, III and V. For the first
two cases we show the integrability of the geodesic flow while for the third
case a somewhat unusual bifurcation phenomenon takes place: for minkowskian
signature elliptic functions are essential in the metric while for euclidean
signature only elementary functions appear
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